Datasets:
question string | source string | source_material string | question_id string | subfield string | cutoff_year int64 | cutoff_date timestamp[s] | control_subtype string | txt_n_words int64 | txt_n_entities int64 | txt_n_numbers int64 | txt_has_causal int64 | txt_has_comparison int64 | txt_has_mechanism int64 | txt_has_measurable int64 | txt_has_alternatives int64 | txt_has_falsification int64 | txt_is_yesno int64 | txt_specificity int64 | ev_top1_sim float64 | ev_top5_mean_sim float64 | ev_n_similar int64 | ev_n_instruments int64 | ev_tension_density float64 | ev_age_mean float64 | ev_age_std float64 | ev_recency_share float64 | ev_native_n_papers int64 | ev_native_year_spread int64 | ev_has_native_record int64 | nov_nn_sim float64 | nov_semantic_distance float64 | nov_mean_top10_sim float64 | nov_pair_doc_count int64 | nov_new_pair int64 | nov_review_overlap float64 | fal_outcome_variable int64 | fal_competing_rule int64 | fal_quant_threshold int64 | fal_named_dataset int64 | tra_n_facilities_mentioned int64 | tra_n_facilities_operational int64 | tra_mentions_future_facility int64 | tra_needs_new_instrument int64 | tra_archival_data int64 | tra_longitudinal int64 | tra_needs_theory int64 | tra_sample_scale int64 | env_pub_volume_3y int64 | env_pub_share_3y float64 | env_growth_ratio float64 | env_review_count_3y int64 | env_years_to_next_facility float64 | env_facility_within_3y int64 | fal_observable int64 | fal_competing_llm int64 | fal_quant_test int64 | fal_falsification_path int64 | future_paper_count int64 | future_paper_count_weak int64 | first_follow_up_date timestamp[s] | lead_time_months int64 | review_recognition bool | top_ids list | top_sims list | addressed bool | answer_status string | n_direct int64 | n_adjacent int64 | premise_status string | supporting_ids list | rationale string | confidence float64 | judge_model string |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
What is the cause of the 4-sigma discrepancy in the depth of Ks-band transits compared to J-band transits for the same exoplanet, and how can future observations resolve this discrepancy? | evidence_tension | {"cluster": [{"arxiv_id": "astro-ph/0509407", "published": "2005-09-14", "sentence": "Though this result seems to be inconsistent with the recently reported HST-STIS findings we point out its limited statistical meaning: the results disagree within 1-sigma, but agree within 2-sigma."}, {"arxiv_id": "1104.0011", "publis... | exoplanet_atmospheres-2012-000 | exoplanet_atmospheres | 2,012 | 2012-12-31T00:00:00 | null | 30 | 0 | 1 | 1 | 1 | 0 | 0 | 0 | 0 | 0 | 1 | 0.229336 | 0.183971 | 4 | 2 | 0.4 | 0.9 | 0.830662 | 1 | 2 | 6 | 1 | 0.229336 | 0.770664 | 0.15102 | 0 | 1 | 0.043837 | 0 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 332 | 0.008184 | 1.860335 | 2 | 6 | 0 | 1 | 0 | 0 | 1 | 1 | 8 | 2014-06-12T00:00:00 | 18 | false | [
"1406.3261",
"1305.1643",
"1608.02346",
"1301.3380",
"1410.4286",
"1712.01285",
"1409.2775",
"1702.02150"
] | [
0.20599327787108127,
0.1579894660405408,
0.1443682356957679,
0.14308831390681104,
0.134100247992351,
0.12846106163684345,
0.12456431389194372,
0.12034823699969274
] | false | not_addressed | 0 | 8 | intact | [] | None of the candidate papers directly investigate the specific 4-sigma discrepancy in Ks-band versus J-band transit depths for the same exoplanet, nor do they provide evidence that resolves this discrepancy. | 1 | gpt-4o |
What is the orbital eccentricity of the hypothetical second planet interacting with the hot Jupiter that has an anomalously large radius, and how does this eccentricity affect the stability and survival of short-period hot Jupiters? | evidence_tension | {"cluster": [{"arxiv_id": "astro-ph/0503554", "published": "2005-03-24", "sentence": "This planet has an anomalously large radius (1.35 times that of Jupiter), which may be the result of ongoing tidal dissipation, but this explanation requires a non-zero orbital eccentricity (~0.03), maintained by interaction with a hy... | exoplanet_atmospheres-2012-001 | exoplanet_atmospheres | 2,012 | 2012-12-31T00:00:00 | null | 35 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 0 | 1 | 0.2063 | 0.154098 | 1 | 0 | 0.4 | 3.4 | 2.332381 | 0.5 | 3 | 6 | 1 | 0.2063 | 0.7937 | 0.138749 | 0 | 1 | 0.053042 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 332 | 0.008184 | 1.860335 | 2 | 6 | 0 | 1 | 0 | 1 | 1 | 0 | 6 | null | null | false | [
"1408.1053",
"1605.01325",
"1305.4070",
"1710.11140",
"1305.1717",
"1404.3686",
"1604.00010",
"1612.06068"
] | [
0.13122486922052243,
0.13062748815065275,
0.1303356009801549,
0.12799481583686156,
0.12717908424389132,
0.12115589650199692,
0.11801505987322589,
0.11279296512294404
] | false | not_addressed | 0 | 5 | intact | [] | None of the candidate papers directly investigate the orbital eccentricity of a hypothetical second planet interacting with a hot Jupiter or its effect on the stability and survival of short-period hot Jupiters. | 1 | gpt-4o |
What are the underlying physical mechanisms that cause the observed discrepancies in radius variations and brightness in the mid-infrared secondary eclipse for pM Class planets, specifically for HD 149026b and HD 209458b? | evidence_tension | {"cluster": [{"arxiv_id": "astro-ph/0509292", "published": "2005-09-12", "sentence": "This not unexpected result has direct consequences for the method of transmission spectroscopy for characterizing the atmospheres of transiting giant planets."}, {"arxiv_id": "1010.2451", "published": "2010-10-12", "sentence": "We fin... | exoplanet_atmospheres-2012-002 | exoplanet_atmospheres | 2,012 | 2012-12-31T00:00:00 | null | 32 | 2 | 0 | 1 | 0 | 1 | 1 | 0 | 0 | 0 | 3 | 0.197313 | 0.16486 | 4 | 1 | 0.4 | 3.9 | 2.022375 | 0.2 | 3 | 5 | 1 | 0.197313 | 0.802687 | 0.144084 | 0 | 1 | 0.065976 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 332 | 0.008184 | 1.860335 | 2 | 6 | 0 | 1 | 0 | 0 | 1 | 1 | 4 | 2017-10-20T00:00:00 | 58 | false | [
"1710.07642",
"1405.5923",
"1409.5336",
"1712.07643",
"1409.8187",
"1603.09343",
"1406.6437",
"1511.06064"
] | [
0.1992193716592585,
0.15197288316989666,
0.1430245865612445,
0.1327797920064225,
0.11968756468762516,
0.1193311594477775,
0.1180540529002563,
0.11688132293336452
] | true | partially_addressed | 4 | 2 | intact | [
"1710.07642",
"1405.5923",
"1409.5336",
"1409.8187"
] | The papers [1710.07642], [1405.5923], [1409.5336], and [1409.8187] provide new observations and analyses of HD 149026b and HD 209458b, contributing evidence on their atmospheric properties and thermal inversions, which are relevant to understanding the discrepancies in radius variations and brightness. However, the que... | 0.9 | gpt-4o |
What is the true value of the angle lambda between the sky projections of the stellar spin axis and the orbit normal for the system studied in astro-ph/0609506, and how does it relate to the anomalous Doppler shifts observed in the stellar spectrum during transits? | evidence_tension | {"cluster": [{"arxiv_id": "astro-ph/0609506", "published": "2006-09-18", "sentence": "By modeling the Rossiter-McLaughlin effect (the anomalous Doppler shift due to the partial eclipse of the rotating stellar surface), we find the angle between the sky projections of the stellar spin axis and orbit normal to be lambda ... | exoplanet_atmospheres-2012-003 | exoplanet_atmospheres | 2,012 | 2012-12-31T00:00:00 | null | 45 | 0 | 1 | 0 | 0 | 0 | 1 | 0 | 0 | 0 | 2 | 0.412602 | 0.207768 | 2 | 4 | 0.4 | 2.5 | 2.247221 | 0.6 | 3 | 4 | 1 | 0.412602 | 0.587398 | 0.152707 | 0 | 1 | 0.026568 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 332 | 0.008184 | 1.860335 | 2 | 6 | 0 | 1 | 0 | 1 | 1 | 1 | 5 | 2013-06-04T00:00:00 | 6 | false | [
"1306.0878",
"1407.7710",
"1710.11140",
"1405.0960",
"1307.2249",
"1704.07771",
"1612.02776",
"1711.02684"
] | [
0.19224736542876375,
0.1781339168704444,
0.1483241728744539,
0.14720204831753989,
0.12227300105526678,
0.11391062577407836,
0.11277613011573545,
0.1052794521477452
] | false | not_addressed | 0 | 8 | intact | [] | None of the candidate papers directly investigate the specific system or question regarding the angle lambda and its relation to anomalous Doppler shifts as posed in the original question. | 1 | gpt-4o |
What are the additional sources of internal heat or mechanisms that suppress cooling in hot Jupiters with anomalously inflated radii exceeding Jupiter's size by more than 60%? | evidence_tension | {"cluster": [{"arxiv_id": "astro-ph/0612603", "published": "2006-12-20", "sentence": "Discovery of hot Jupiter exo-planets, those with anomalously inflated size and low density relative to Jupiter, has evoked much discussion as to possible sources of internal heat production."}, {"arxiv_id": "1008.0645", "published": "... | exoplanet_atmospheres-2012-004 | exoplanet_atmospheres | 2,012 | 2012-12-31T00:00:00 | null | 27 | 0 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 0 | 2 | 0.279061 | 0.1865 | 3 | 1 | 0.5 | 1.7 | 1.846619 | 0.7 | 4 | 5 | 1 | 0.279061 | 0.720939 | 0.142357 | 0 | 1 | 0.027066 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 332 | 0.008184 | 1.860335 | 2 | 6 | 0 | 1 | 0 | 0 | 1 | 4 | 6 | 2013-03-01T00:00:00 | 3 | false | [
"1511.00135",
"1303.0293",
"1706.07605",
"1510.00067",
"1711.07294",
"1501.02087",
"1612.01739",
"1712.07643"
] | [
0.21921435852235704,
0.2078641998691058,
0.19994154688080648,
0.18208238683651626,
0.13147277561632642,
0.12295103648175151,
0.1143900013754407,
0.10368422681717046
] | true | partially_addressed | 5 | 3 | intact | [
"1511.00135",
"1303.0293",
"1706.07605",
"1510.00067",
"1501.02087"
] | Several papers, including [1511.00135], [1303.0293], [1706.07605], [1510.00067], and [1501.02087], contribute substantive new evidence on mechanisms such as ohmic heating, deep energy deposition, and atmospheric heat redistribution that could explain the inflated radii of hot Jupiters. However, the question is not full... | 1 | gpt-4o |
How does the atmospheric opacity of exoplanets vary with wavelength in the mid-infrared, specifically comparing the opacity at 3.6 microns to that at 4.5 microns, and what factors contribute to the observed discrepancies with model predictions? | evidence_tension | {"cluster": [{"arxiv_id": "astro-ph/0702700", "published": "2007-02-27", "sentence": "This represents a departure from predictions made by previous simulations in the literature that used the shallow water formalism; we find that the disagreement is explained by the factor of 30 shorter radiative timescale used in our ... | exoplanet_atmospheres-2012-005 | exoplanet_atmospheres | 2,012 | 2012-12-31T00:00:00 | null | 36 | 0 | 2 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 2 | 0.122587 | 0.119418 | 0 | 3 | 0.5 | 3.2 | 1.661325 | 0.3 | 2 | 4 | 1 | 0.122587 | 0.877413 | 0.109544 | 0 | 1 | 0.039212 | 0 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 332 | 0.008184 | 1.860335 | 2 | 6 | 0 | 1 | 0 | 1 | 1 | 0 | 1 | null | null | false | [
"1711.10529",
"1608.00056",
"1409.5108",
"1711.08463",
"1403.2723",
"1307.2083",
"1510.01706",
"1705.05468"
] | [
0.1340807960467252,
0.11744003226833212,
0.11496066940071693,
0.11355756597771256,
0.1062410810013587,
0.10593475328489482,
0.10376880165532679,
0.09987370185789392
] | true | partially_addressed | 2 | 6 | intact | [
"1608.00056",
"1711.08463"
] | Paper 1608.00056 provides phase curve observations of WASP-43b at 3.6 and 4.5 microns, directly addressing the question of atmospheric opacity variation with wavelength. Paper 1711.08463 discusses the implications of wavelength-dependent opacity on thermal phase curves, contributing to understanding discrepancies with ... | 1 | gpt-4o |
What are the underlying mechanisms that lead to the anomalously large radii of hot Jupiters, and how do these mechanisms relate to their migration history and the observed inclination and eccentricity distributions? | evidence_tension | {"cluster": [{"arxiv_id": "astro-ph/0703418", "published": "2007-03-16", "sentence": "Some short-period exoplanets (hot Jupiters) are observed by their transits to have anomalously large radii."}, {"arxiv_id": "0901.0735", "published": "2009-01-07", "sentence": "If deposited sufficiently deep, these heating rates may e... | exoplanet_atmospheres-2012-006 | exoplanet_atmospheres | 2,012 | 2012-12-31T00:00:00 | null | 32 | 0 | 0 | 1 | 0 | 1 | 1 | 0 | 0 | 0 | 1 | 0.159348 | 0.149734 | 2 | 1 | 0.3 | 1.7 | 1.615549 | 0.7 | 4 | 4 | 1 | 0.159348 | 0.840652 | 0.134568 | 0 | 1 | 0.034404 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 332 | 0.008184 | 1.860335 | 2 | 6 | 0 | 1 | 0 | 0 | 1 | 0 | 8 | null | null | false | [
"1408.3668",
"1710.01737",
"1603.09506",
"1309.0011",
"1309.1520",
"1604.03107",
"1308.4968",
"1604.00010"
] | [
0.1772727461884997,
0.16189784167695975,
0.14686519699555778,
0.13768673255310684,
0.13720286849980443,
0.13107713213600625,
0.13084459350150593,
0.12090476698094534
] | true | partially_addressed | 3 | 5 | intact | [
"1603.09506",
"1604.03107",
"1308.4968"
] | Papers 1603.09506, 1604.03107, and 1308.4968 contribute substantive new evidence on the migration mechanisms and their effects on hot Jupiters, including the role of high-eccentricity migration and tidal dissipation. However, the question is not fully settled. | 0.9 | gpt-4o |
What are the reasons for the inconsistency between the spectral data for HD 189733b and the 8 um-photometry obtained with Spitzer's IRAC, and how do these discrepancies affect the detection of spectral features in the K-band? | evidence_tension | {"cluster": [{"arxiv_id": "0705.2457", "published": "2007-05-16", "sentence": "Here we suggest that, in the absence of flux variability, the spectral data for HD 189733b are inconsistent with 8 um-photometry obtained with Spitzer's InfraRed Array Camera (IRAC), perhaps an indication of problems with the challenging red... | exoplanet_atmospheres-2012-007 | exoplanet_atmospheres | 2,012 | 2012-12-31T00:00:00 | null | 36 | 1 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 2 | 0.276864 | 0.182551 | 4 | 2 | 0.1 | 2.8 | 2.271563 | 0.4 | 2 | 4 | 1 | 0.276864 | 0.723136 | 0.157255 | 1 | 0 | 0.074012 | 0 | 0 | 1 | 1 | 1 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 332 | 0.008184 | 1.860335 | 2 | 6 | 0 | 1 | 0 | 0 | 1 | 0 | 10 | null | null | false | [
"1405.1056",
"1401.7601",
"1601.03959",
"1602.05584",
"1601.04761",
"1507.08070",
"1609.06148",
"1409.4000"
] | [
0.14698189745681553,
0.1450828919413198,
0.13942121905689203,
0.13441612761328303,
0.13359235519817694,
0.132870493064,
0.13279830217730965,
0.12780505005522305
] | true | posed_but_open | 1 | 4 | intact | [
"1401.7601"
] | Paper 1401.7601 directly investigates the spectral data discrepancies for HD 189733b, discussing the controversy and performing a uniform spectral retrieval analysis, but it does not provide a definitive resolution to the question. | 0.9 | gpt-4o |
How do the atmospheric dynamics of terrestrial planets differ from those of hot Jupiters, and what specific imaging or modeling techniques can accurately capture these differences? | evidence_tension | {"cluster": [{"arxiv_id": "0706.1047", "published": "2007-06-07", "sentence": "In light of the overwhelming dominance of dynamics-based methods over the past decade, we challenge the notion that spectra of terrestrial planets necessarily require extreme imaging methods."}, {"arxiv_id": "0907.2692", "published": "2009-0... | exoplanet_atmospheres-2012-008 | exoplanet_atmospheres | 2,012 | 2012-12-31T00:00:00 | null | 26 | 0 | 0 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0.172409 | 0.137556 | 1 | 7 | 0.2 | 3 | 1.788854 | 0.4 | 2 | 2 | 1 | 0.172409 | 0.827591 | 0.11523 | 1 | 0 | 0.124019 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 332 | 0.008184 | 1.860335 | 2 | 6 | 0 | 1 | 0 | 0 | 1 | 0 | 0 | null | null | false | [
"1412.1731",
"1709.09678",
"1308.1670",
"1306.0567",
"1610.03893",
"1407.4150",
"1311.0003",
"1406.6566"
] | [
0.11945001039278966,
0.10946535074296085,
0.10575671987519808,
0.10133729002513837,
0.0983817764697739,
0.09768821933512473,
0.09114351420337585,
0.08816525337200211
] | false | not_addressed | 0 | 0 | not_applicable | [] | No future paper reached the minimum relevance threshold. | 0.9 | auto_threshold |
What are the specific atmospheric conditions, including the presence of an inversion layer and potential stratospheric absorbers, that lead to the observed discrepancies in the emission spectra of exoplanets, particularly regarding the 4.5 and 5.8 micron bandpasses and the 8 micron brightness temperature? | evidence_tension | {"cluster": [{"arxiv_id": "0709.3984", "published": "2007-09-25", "sentence": "These eclipse depths reveal that the shape of the inferred emission spectrum for the planet differs significantly from the predictions of standard atmosphere models; instead the most plausible explanation would require the presence of an inv... | exoplanet_atmospheres-2012-009 | exoplanet_atmospheres | 2,012 | 2012-12-31T00:00:00 | null | 43 | 0 | 3 | 1 | 0 | 0 | 1 | 0 | 0 | 0 | 3 | 0.223937 | 0.161332 | 3 | 2 | 0.2 | 3.2 | 1.4 | 0.3 | 4 | 2 | 1 | 0.223937 | 0.776063 | 0.140706 | 0 | 1 | 0.037562 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 332 | 0.008184 | 1.860335 | 2 | 6 | 0 | 1 | 0 | 0 | 1 | 0 | 7 | null | null | false | [
"1510.01706",
"1611.09272",
"1610.03504",
"1604.02310",
"1502.02132",
"1711.08463",
"1504.05942",
"1411.3093"
] | [
0.16313770817845713,
0.13959280432002413,
0.13137609497264802,
0.13096274887714163,
0.13086620872296226,
0.1293048027532721,
0.1209813741593414,
0.11668956303303085
] | true | partially_addressed | 1 | 7 | intact | [
"1504.05942"
] | Paper 1504.05942 directly investigates the emission spectra of HD209458b in the 4.5 and 5.8 micron bandpasses and the 8 micron brightness temperature, contributing evidence relevant to the question of atmospheric conditions affecting these observations. | 0.9 | gpt-4o |
What are the detailed chemical compositions and physical properties of the atmospheres of various exoplanets, particularly those that are not hot Jupiters? | direct_llm | {"n_titles_shown": 60} | exoplanet_atmospheres-2012-010 | exoplanet_atmospheres | 2,012 | 2012-12-31T00:00:00 | null | 22 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0.172169 | 0.132914 | 1 | 3 | 0 | 1.8 | 1.661325 | 0.7 | 0 | 0 | 0 | 0.172169 | 0.827831 | 0.119156 | 0 | 1 | 0.107114 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 332 | 0.008184 | 1.860335 | 2 | 6 | 0 | 1 | 0 | 0 | 0 | 0 | 7 | null | null | false | [
"1402.1169",
"1612.04372",
"1607.04062",
"1604.06092",
"1710.06433",
"1602.06733",
"1403.0121",
"1403.6891"
] | [
0.1752309926464765,
0.152143779750957,
0.15210899688932505,
0.14924752994845011,
0.1349872457165391,
0.1347706791470928,
0.12534975244840463,
0.11925805525862293
] | false | not_addressed | 0 | 8 | intact | [] | None of the candidate papers directly investigate the chemical compositions and physical properties of exoplanet atmospheres beyond hot Jupiters. They focus primarily on hot Jupiters or general atmospheric studies. | 1 | gpt-4o |
How do atmospheric circulation patterns vary among different types of exoplanets, and what are the implications for climate and habitability? | direct_llm | {"n_titles_shown": 60} | exoplanet_atmospheres-2012-011 | exoplanet_atmospheres | 2,012 | 2012-12-31T00:00:00 | null | 20 | 0 | 0 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0.178875 | 0.147797 | 2 | 1 | 0 | 1.3 | 1.552417 | 0.8 | 0 | 0 | 0 | 0.178875 | 0.821125 | 0.12281 | 1 | 0 | 0.09319 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 332 | 0.008184 | 1.860335 | 2 | 6 | 0 | 1 | 0 | 0 | 0 | 1 | 5 | 2017-10-03T00:00:00 | 58 | false | [
"1710.01405",
"1303.7079",
"1708.07009",
"1604.06092",
"1603.00950",
"1409.5108",
"1706.01224",
"1705.05535"
] | [
0.19701791055779172,
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0.15102853323571316,
0.14279295702217615,
0.1289639555470238,
0.11358153039501226,
0.10548414204347849,
0.10541551736254151
] | true | partially_addressed | 2 | 6 | intact | [
"1303.7079",
"1409.5108"
] | Paper 1303.7079 investigates atmospheric circulation patterns on close-in land planets, contributing to understanding variations among exoplanets. Paper 1409.5108 models atmospheric circulation of the eccentric hot Jupiter HAT-P-2b, providing insights into circulation patterns on different exoplanet types. | 0.9 | gpt-4o |
What mechanisms drive atmospheric escape in exoplanets, particularly in relation to their mass, distance from their host stars, and stellar activity? | direct_llm | {"n_titles_shown": 60} | exoplanet_atmospheres-2012-012 | exoplanet_atmospheres | 2,012 | 2012-12-31T00:00:00 | null | 21 | 0 | 0 | 1 | 0 | 1 | 1 | 0 | 0 | 0 | 1 | 0.206965 | 0.170173 | 4 | 2 | 0 | 2.2 | 1.661325 | 0.7 | 0 | 0 | 0 | 0.206965 | 0.793035 | 0.144383 | 0 | 1 | 0.022488 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 332 | 0.008184 | 1.860335 | 2 | 6 | 0 | 1 | 0 | 0 | 1 | 0 | 11 | null | null | false | [
"1412.3380",
"1308.1585",
"1411.0636",
"1404.1073",
"1403.0652",
"1308.0511",
"1306.0973",
"1303.4596"
] | [
0.15419336080126594,
0.15288045592987037,
0.1459456507434802,
0.14349890289035297,
0.14088894328215712,
0.13438510717025284,
0.13277025360609135,
0.12998619933986724
] | true | partially_addressed | 4 | 4 | intact | [
"1412.3380",
"1308.1585",
"1308.0511",
"1306.0973"
] | Papers 1412.3380 and 1306.0973 explore the role of XUV radiation and stellar activity in driving atmospheric escape, while 1308.1585 investigates atmospheric escape in a specific exoplanet, and 1308.0511 discusses the conservation of escape rates under certain conditions. These contribute evidence on mechanisms of atmo... | 1 | gpt-4o |
How do the presence of clouds and hazes affect the observable spectra of exoplanet atmospheres, and what are the best methods to detect and characterize them? | direct_llm | {"n_titles_shown": 60} | exoplanet_atmospheres-2012-013 | exoplanet_atmospheres | 2,012 | 2012-12-31T00:00:00 | null | 26 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0.17506 | 0.159162 | 3 | 0 | 0.1 | 1.5 | 1.204159 | 0.8 | 0 | 0 | 0 | 0.17506 | 0.82494 | 0.137598 | 0 | 1 | 0.059061 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 332 | 0.008184 | 1.860335 | 2 | 6 | 0 | 1 | 0 | 0 | 0 | 1 | 13 | 2013-01-23T00:00:00 | 1 | false | [
"1301.5627",
"1511.01492",
"1601.03492",
"1701.01113",
"1705.08893",
"1504.07655",
"1512.06698",
"1512.04341"
] | [
0.1869785634542086,
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0.14443305170898926,
0.14328927427132931,
0.14147577038798043,
0.13760229392224865,
0.13176519704950573,
0.12817303803102767
] | true | partially_addressed | 7 | 1 | intact | [
"1301.5627",
"1511.01492",
"1601.03492",
"1701.01113",
"1705.08893",
"1512.06698",
"1512.04341"
] | Multiple papers, such as 1301.5627 and 1511.01492, discuss the impact of clouds and hazes on exoplanet spectra and methods for their detection and characterization. Papers like 1601.03492 and 1705.08893 provide models and metrics for predicting and analyzing cloud presence, contributing substantive evidence but not ful... | 1 | gpt-4o |
What are the long-term stability and evolution of exoplanet atmospheres under varying stellar and environmental conditions? | direct_llm | {"n_titles_shown": 60} | exoplanet_atmospheres-2012-014 | exoplanet_atmospheres | 2,012 | 2012-12-31T00:00:00 | null | 16 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0.139829 | 0.106245 | 0 | 1 | 0 | 2.4 | 0.916515 | 0.4 | 0 | 0 | 0 | 0.139829 | 0.860171 | 0.095405 | 0 | 1 | 0.088443 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 332 | 0.008184 | 1.860335 | 2 | 6 | 0 | 1 | 0 | 0 | 0 | 1 | 2 | 2014-08-05T00:00:00 | 20 | false | [
"1408.1053",
"1605.01955",
"1702.01137",
"1703.00001",
"1709.06124",
"1304.6673",
"1706.06349",
"1707.01534"
] | [
0.1872285698041652,
0.1202090711349349,
0.11537034535355467,
0.11364271209024977,
0.11312935666574088,
0.1073010737885151,
0.1054296618087458,
0.10461398132486804
] | true | partially_addressed | 2 | 5 | intact | [
"1709.06124",
"1706.06349"
] | Papers 1709.06124 and 1706.06349 provide substantive new evidence on the atmospheric conditions and stability of exoplanet atmospheres, specifically addressing the transmission spectroscopy of TrES-3 b and the ionospheric conditions of hot Jupiters, respectively. These contribute to understanding the long-term stabilit... | 0.9 | gpt-4o |
What is the range of the dayside luminosity for WASP-12b, and how does it affect the predicted day/night effective temperature contrast? | future_work | {"statement": {"arxiv_id": "1201.1023", "published": "2012-01-04", "sentence": "We also revisit WASP-12b's energy budget on the basis of secondary eclipse observations: the dayside luminosity is a relatively poorly constrained (2.0-4.3) x 10^30 erg/s, but this still allows us to predict a day/night effective temperatur... | exoplanet_atmospheres-2012-015 | exoplanet_atmospheres | 2,012 | 2012-12-31T00:00:00 | null | 21 | 1 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 0 | 2 | 0.280828 | 0.200434 | 7 | 2 | 0.1 | 1.2 | 0.979796 | 0.9 | 0 | 0 | 0 | 0.280828 | 0.719172 | 0.174869 | 1 | 0 | 0.041403 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 332 | 0.008184 | 1.860335 | 2 | 6 | 0 | 1 | 0 | 1 | 1 | 4 | 18 | 2013-01-06T00:00:00 | 1 | false | [
"1512.09342",
"1301.0968",
"1709.03502",
"1707.05790",
"1405.5923",
"1305.1643",
"1309.5261",
"1710.03556"
] | [
0.201506269026,
0.19102872206125548,
0.18600014699091302,
0.18063188520004464,
0.17668993585766404,
0.1629329388229367,
0.15587393971734229,
0.14243476541255515
] | true | posed_but_open | 1 | 7 | intact | [
"1301.0968"
] | Paper 1301.0968 revisits the emission spectrum of WASP-12b and finds it consistent with a featureless blackbody, indicating a nearly isothermal photosphere on the day side. However, it concludes that the current data is insufficient to constrain the atmospheric composition, leaving the question open. | 1 | gpt-4o |
What is the age of the system, considering the conflicting results from stellar evolution models, gyrochronology, and lithium abundance? | future_work | {"statement": {"arxiv_id": "1107.2032", "published": "2011-07-11", "sentence": "The age of the system remains uncertain, with stellar evolution models pointing either to a few tens Ma or several Ga, while gyrochronology and lithium abundance point towards ages of a few hundred Ma."}} | exoplanet_atmospheres-2012-016 | exoplanet_atmospheres | 2,012 | 2012-12-31T00:00:00 | null | 19 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 0 | 1 | 0.223371 | 0.162746 | 3 | 5 | 0 | 1.8 | 0.979796 | 0.7 | 0 | 0 | 0 | 0.223371 | 0.776629 | 0.120665 | 1 | 0 | 0.026609 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 332 | 0.008184 | 1.860335 | 2 | 6 | 0 | 1 | 3 | 0 | 1 | 0 | 2 | null | null | false | [
"1603.03038",
"1601.07680",
"1506.05685",
"1712.01035",
"1403.6891",
"1608.03833",
"1712.07891",
"1505.03516"
] | [
0.13502123792004994,
0.12272170598753705,
0.10076829222698598,
0.09655488086376149,
0.08657942473878565,
0.08492027679053253,
0.08423188053993529,
0.08205226185949765
] | false | not_addressed | 0 | 4 | intact | [] | None of the candidate papers directly investigate the age of the system in question or provide evidence that would resolve the conflicting results from stellar evolution models, gyrochronology, and lithium abundance. | 1 | gpt-4o |
What is the H2 density in the water-emitting region, and how does it relate to the H2O abundance relative to H2? | future_work | {"statement": {"arxiv_id": "0805.0573", "published": "2008-05-05", "sentence": "The H2 density in the water-emitting region is not well constrained by our observations, but is likely between 3 10^4 and 10^6 cm^3, yielding an H2O abundance relative to H2 of between 2 10^-5 and 6 10^-4."}} | exoplanet_atmospheres-2012-017 | exoplanet_atmospheres | 2,012 | 2012-12-31T00:00:00 | null | 21 | 0 | 0 | 0 | 1 | 0 | 1 | 0 | 0 | 0 | 1 | 0.377618 | 0.248307 | 13 | 2 | 0 | 2.8 | 1.469694 | 0.5 | 0 | 0 | 0 | 0.377618 | 0.622382 | 0.213873 | 1 | 0 | 0.015515 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 332 | 0.008184 | 1.860335 | 2 | 6 | 0 | 1 | 0 | 1 | 1 | 3 | 13 | 2013-03-25T00:00:00 | 3 | false | [
"1403.4821",
"1702.08618",
"1303.6177",
"1703.08973",
"1601.00821",
"1306.6325",
"1412.4818",
"1307.2627"
] | [
0.27600447326641464,
0.20982938580625893,
0.1898367249212686,
0.17279540080062342,
0.1667347118433483,
0.16419898530860436,
0.15750614744517444,
0.15114991238387157
] | true | partially_addressed | 3 | 2 | intact | [
"1403.4821",
"1303.6177",
"1412.4818"
] | Papers 1403.4821, 1303.6177, and 1412.4818 provide evidence on water abundance and its relation to H2 density in star-forming regions, contributing substantive new evidence to the question but not fully settling it. | 0.9 | gpt-4o |
What are the uncertainties in the details of the radiative forcing and frictional drag in hot-Jupiter circulation models? | future_work | {"statement": {"arxiv_id": "1208.0126", "published": "2012-08-01", "sentence": "Although the outcome of hot-Jupiter circulation models depend on details of the radiative forcing and frictional drag, aspects of which remain uncertain, we conclude that the specification of initial conditions is not a source of uncertaint... | exoplanet_atmospheres-2012-018 | exoplanet_atmospheres | 2,012 | 2012-12-31T00:00:00 | null | 18 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0.30275 | 0.233899 | 7 | 0 | 0 | 1.3 | 1.417745 | 0.9 | 0 | 0 | 0 | 0.30275 | 0.69725 | 0.189921 | 1 | 0 | 0.139046 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 332 | 0.008184 | 1.860335 | 2 | 6 | 0 | 1 | 0 | 0 | 0 | 1 | 4 | 2016-01-01T00:00:00 | 37 | false | [
"1601.00069",
"1410.2382",
"1401.7571",
"1610.03893",
"1405.6109",
"1706.00466",
"1712.07643",
"1704.06813"
] | [
0.31150657193393533,
0.16596451279094304,
0.1580625902210863,
0.1526816962692652,
0.11615685253712639,
0.11477476281372254,
0.1083922257847463,
0.10345765738060518
] | true | partially_addressed | 1 | 7 | intact | [
"1401.7571"
] | Paper 1401.7571 provides a comprehensive analysis of atmospheric dynamics in exoplanetary atmospheres, including the effects of frictional drag and radiative forcing, contributing substantive evidence to the question of uncertainties in hot-Jupiter circulation models. | 0.9 | gpt-4o |
What future observations are needed to constrain the orbital inclination of HAT-P-13c and its mutual inclination to HAT-P-13b? | future_work | {"statement": {"arxiv_id": "0907.3525", "published": "2009-07-21", "sentence": "While we have not detected significant transit timing variations of HAT-P-13b, due to gravitational and light-travel time effects, future observations will constrain the orbital inclination of HAT-P-13c, along with its mutual inclination to... | exoplanet_atmospheres-2012-019 | exoplanet_atmospheres | 2,012 | 2012-12-31T00:00:00 | null | 18 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1 | 0.350825 | 0.183401 | 2 | 3 | 0 | 1.7 | 1.187434 | 0.6 | 0 | 0 | 0 | 0.350825 | 0.649175 | 0.151719 | 3 | 0 | 0.019099 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 332 | 0.008184 | 1.860335 | 2 | 6 | 0 | 1 | 0 | 0 | 0 | 2 | 9 | 2016-02-11T00:00:00 | 38 | false | [
"1602.03895",
"1710.05920",
"1708.07909",
"1408.0401",
"1712.03384",
"1407.2245",
"1705.02334",
"1409.5108"
] | [
0.19409287063598082,
0.18342603605454683,
0.1692455543665594,
0.1525223837642039,
0.14317258354779627,
0.1369695718972856,
0.131301242480531,
0.12375043128500476
] | false | not_addressed | 0 | 8 | intact | [] | None of the candidate papers directly investigate the orbital inclination of HAT-P-13c or its mutual inclination with HAT-P-13b. They are related to the broader topic of exoplanetary systems but do not address the specific question. | 1 | gpt-4o |
How might the capabilities of future telescopes like JWST and EChO to measure thermal phase curves of exoplanets influence the prevalence of false detections in exoplanet surveys? | control | {"claim_a": {"arxiv_id": "1110.3087", "sentence": "Future telescopes (JWST and EChO) will have the capability to measure thermal phase curves of exoplanets including hot rocky planets in transiting and non-transiting configurations, and at different wavelengths."}, "claim_b": {"arxiv_id": "1002.0886", "sentence": "Our ... | exoplanet_atmospheres-2012-020 | exoplanet_atmospheres | 2,012 | 2012-12-31T00:00:00 | random_pair | 27 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0.2405 | 0.159565 | 3 | 4 | 0.2 | 1.7 | 1.615549 | 0.8 | 0 | 0 | 0 | 0.2405 | 0.7595 | 0.132395 | 0 | 1 | 0.055249 | 0 | 0 | 0 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 0 | 0 | 332 | 0.008184 | 1.860335 | 2 | 6 | 0 | 1 | 0 | 0 | 0 | 1 | 5 | 2014-01-15T00:00:00 | 13 | false | [
"1401.3673",
"1406.6566",
"1711.07696",
"1307.2003",
"1706.06602",
"1703.00496",
"1705.07098",
"1412.8216"
] | [
0.19937659184838505,
0.15398426610904561,
0.14548018714728495,
0.1282260813078219,
0.12584735113793716,
0.11554588374182133,
0.1144639520801345,
0.11006702540088435
] | false | not_addressed | 0 | 8 | intact | [] | None of the candidate papers directly investigate the influence of future telescopes like JWST and EChO on the prevalence of false detections in exoplanet surveys. | 1 | gpt-4o |
In what ways does the temperature rise observed above the drop in sodium abundance at the 3mbar level correlate with the C/H and O/H ratios reported for WASP-12b? | control | {"claim_a": {"arxiv_id": "1109.3183", "sentence": "This scenario also satisfies the constraints on the C/H and O/H ratios reported for WASP-12b."}, "claim_b": {"arxiv_id": "1012.5938", "sentence": "We find a rise in temperature above the drop in sodium abundance at the 3mbar level."}} | exoplanet_atmospheres-2012-021 | exoplanet_atmospheres | 2,012 | 2012-12-31T00:00:00 | random_pair | 28 | 1 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 0 | 2 | 0.226389 | 0.16003 | 2 | 3 | 0.1 | 1.9 | 1.577973 | 0.7 | 0 | 0 | 0 | 0.226389 | 0.773611 | 0.137013 | 1 | 0 | 0.03696 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 332 | 0.008184 | 1.860335 | 2 | 6 | 0 | 1 | 0 | 0 | 0 | 0 | 1 | null | null | false | [
"1301.0968",
"1406.3261",
"1410.3702",
"1703.06716",
"1512.07197",
"1707.05790",
"1503.05582",
"1504.07655"
] | [
0.12610694267679004,
0.1198733978482892,
0.11891608554219137,
0.11113703427408164,
0.0991172965290078,
0.095667281206944,
0.0952321723117398,
0.09459665173995394
] | true | posed_but_open | 1 | 5 | intact | [
"1410.3702"
] | Paper 1410.3702 reports a tentative detection of sodium in the atmosphere of WASP-12b, which is relevant to the question of sodium abundance and its correlation with temperature and elemental ratios. However, it does not provide conclusive evidence on the correlation with C/H and O/H ratios, leaving the question open. | 0.9 | gpt-4o |
What is the nature of the atmospheric dynamics in exoplanets across various environments? | control | {} | exoplanet_atmospheres-2012-022 | exoplanet_atmospheres | 2,012 | 2012-12-31T00:00:00 | vague | 13 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0.139233 | 0.13063 | 0 | 1 | 0.1 | 3.4 | 1.854724 | 0.3 | 0 | 0 | 0 | 0.139233 | 0.860767 | 0.119689 | 0 | 1 | 0.136787 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 332 | 0.008184 | 1.860335 | 2 | 6 | 0 | 0 | 0 | 0 | 0 | 0 | 4 | null | null | false | [
"1309.6016",
"1701.02360",
"1608.08620",
"1608.03833",
"1409.7320",
"1711.02684",
"1407.4150",
"1612.05945"
] | [
0.13141195034354494,
0.13021551139624857,
0.12673999164720345,
0.12075397836287578,
0.11038345861853616,
0.10515878268678767,
0.10446136539446378,
0.09236389512847128
] | true | partially_addressed | 3 | 5 | intact | [
"1701.02360",
"1711.02684",
"1407.4150"
] | Papers 1701.02360, 1711.02684, and 1407.4150 contribute substantive new evidence on the atmospheric dynamics of exoplanets, including modeling of climates and atmospheric dynamics of rocky planets and hot Jupiters. These studies provide insights into the nature of atmospheric dynamics across different exoplanetary envi... | 1 | gpt-4o |
How might the calculated detection limits for minimum planetary mass and period inform our understanding of exoplanet formation theories? | control | {"arxiv_id": "1205.3723", "sentence": "Detection limits for these data,expressed in minimum planetary mass and period, are calculated."} | exoplanet_atmospheres-2012-023 | exoplanet_atmospheres | 2,012 | 2012-12-31T00:00:00 | untestable | 19 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 0 | 1 | 0.136903 | 0.117587 | 0 | 4 | 0 | 2 | 2 | 0.7 | 0 | 0 | 0 | 0.136903 | 0.863097 | 0.103552 | 0 | 1 | 0.066187 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 332 | 0.008184 | 1.860335 | 2 | 6 | 0 | 1 | 0 | 0 | 0 | 0 | 1 | null | null | false | [
"1308.2937",
"1509.07750",
"1506.03734",
"1602.05674",
"1307.2249",
"1402.0846",
"1603.03274",
"1608.06772"
] | [
0.12607090619720443,
0.11579351867243441,
0.11093375181023604,
0.1104453520749495,
0.10440173901001357,
0.10383403631543084,
0.09672055428753135,
0.0949691688981678
] | false | not_addressed | 0 | 8 | intact | [] | None of the candidate papers directly investigate the relationship between detection limits for planetary mass and period and exoplanet formation theories. They focus on specific exoplanet discoveries or related methodologies. | 1 | gpt-4o |
Could it be possible that the atmospheric composition of exoplanets is predominantly influenced by factors other than their metallicity? | control | {"arxiv_id": "1109.0582", "title": "The Optical and Near-Infrared Transmission Spectrum of the Super-Earth GJ1214b: Further Evidence for a Metal-Rich Atmosphere"} | exoplanet_atmospheres-2012-024 | exoplanet_atmospheres | 2,012 | 2012-12-31T00:00:00 | consensus_challenge | 19 | 0 | 0 | 0 | 1 | 0 | 1 | 0 | 0 | 1 | 1 | 0.121346 | 0.107091 | 0 | 4 | 0.1 | 1.8 | 1.077033 | 0.8 | 0 | 0 | 0 | 0.121346 | 0.878654 | 0.093127 | 0 | 1 | 0.042292 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 332 | 0.008184 | 1.860335 | 2 | 6 | 0 | 1 | 1 | 0 | 1 | 0 | 0 | null | null | false | [
"1401.6181",
"1401.5119",
"1612.01616",
"1609.05898",
"1703.02630",
"1708.09257",
"1312.3007",
"1711.10491"
] | [
0.10856234299131526,
0.1083476624935838,
0.10218901746233201,
0.09574430245367281,
0.0943004838523255,
0.09404947705523979,
0.09353247909224002,
0.09185920585284048
] | false | not_addressed | 0 | 0 | not_applicable | [] | No future paper reached the minimum relevance threshold. | 0.9 | auto_threshold |
What are the underlying reasons for the discrepancies between the gas and dust outer radii in protoplanetary disks, as indicated by millimeter observations, and how do these discrepancies relate to the photometric data and images of the debris disk around Vega? | evidence_tension | {"cluster": [{"arxiv_id": "1203.0318", "published": "2012-03-01", "sentence": "We present three new millimeter-wavelength observations that help to resolve the puzzling and contradictory observations."}, {"arxiv_id": "0905.3388", "published": "2009-05-20", "sentence": "Our new observations resolve the dust emission, an... | protoplanetary_disks-2012-000 | protoplanetary_disks | 2,012 | 2012-12-31T00:00:00 | null | 41 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 0 | 1 | 0.178281 | 0.152076 | 2 | 4 | 0.8 | 3.4 | 2.497999 | 0.3 | 4 | 4 | 1 | 0.178281 | 0.821719 | 0.137944 | 0 | 1 | 0.100865 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1,211 | 0.029851 | 1.388316 | 26 | 2 | 1 | 1 | 0 | 0 | 0 | 0 | 6 | null | null | false | [
"1301.1331",
"1311.5222",
"1511.07149",
"1412.4816",
"1510.08890",
"1307.3560",
"1310.5069",
"1307.1735"
] | [
0.16453323113584203,
0.13842988942227652,
0.1342600312191144,
0.13419869150142436,
0.12656795028499246,
0.12211166910260979,
0.11165698129839093,
0.110650188845755
] | false | not_addressed | 0 | 8 | intact | [] | None of the candidate papers directly investigate the discrepancies between gas and dust outer radii in protoplanetary disks or their relation to the debris disk around Vega. | 1 | gpt-4o |
What is the true distance of the star forming regions associated with the Li-depleted stars, and how does this distance affect the interpretation of their ages and the presence of crystalline silicates in protoplanetary disks? | evidence_tension | {"cluster": [{"arxiv_id": "astro-ph/0501307", "published": "2005-01-14", "sentence": "Although a distance 38% closer than that of Taurus-Auriga or a hotter temperature scale could reconcile this discrepancy at 21-25 Myr, similar discrepancies in other systems and the implications of an extremely old accreting Taurus-Au... | protoplanetary_disks-2012-001 | protoplanetary_disks | 2,012 | 2012-12-31T00:00:00 | null | 35 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 0 | 1 | 0.260855 | 0.185367 | 4 | 2 | 0.2 | 3.1 | 2.022375 | 0.4 | 4 | 4 | 1 | 0.260855 | 0.739145 | 0.159542 | 2 | 0 | 0.145836 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1,211 | 0.029851 | 1.388316 | 26 | 2 | 1 | 1 | 0 | 0 | 0 | 0 | 6 | null | null | false | [
"1412.4618",
"1703.05945",
"1505.05563",
"1707.03179",
"1406.2385",
"1304.4435",
"1501.07270",
"1610.09873"
] | [
0.17557865391758543,
0.13597216573179605,
0.13594258739519846,
0.1356871194771315,
0.13333145822659406,
0.12762838597777904,
0.11821869271858118,
0.1132085516522309
] | false | not_addressed | 0 | 8 | intact | [] | None of the candidate papers directly investigate the specific question of the true distance of star forming regions associated with Li-depleted stars or its impact on age interpretation and crystalline silicates in protoplanetary disks. | 1 | gpt-4o |
How do the inner disk sizes and mass accretion rates of young stellar objects (YSOs) compare to the predictions of magnetospheric accretion models and the standard model of inside-out collapse? | evidence_tension | {"cluster": [{"arxiv_id": "astro-ph/0501308", "published": "2005-01-14", "sentence": "Our measured inner disk sizes are larger than disk truncation radii predicted by magnetospheric accretion models, with larger discrepancies for sources with higher mass accretion rates."}, {"arxiv_id": "1103.5309", "published": "2011-... | protoplanetary_disks-2012-002 | protoplanetary_disks | 2,012 | 2012-12-31T00:00:00 | null | 30 | 0 | 0 | 0 | 1 | 0 | 1 | 0 | 0 | 0 | 1 | 0.324616 | 0.230734 | 14 | 3 | 0.2 | 3.7 | 2.282542 | 0.3 | 4 | 6 | 1 | 0.324616 | 0.675384 | 0.197433 | 2 | 0 | 0.132 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 1,211 | 0.029851 | 1.388316 | 26 | 2 | 1 | 1 | 2 | 0 | 1 | 3 | 43 | 2013-04-29T00:00:00 | 4 | false | [
"1401.0408",
"1402.3240",
"1304.7777",
"1507.05967",
"1401.6545",
"1602.04068",
"1712.00457",
"1605.03985"
] | [
0.22217671332622935,
0.19467279878133664,
0.18100103020344116,
0.1721367883555005,
0.1708199542980558,
0.16042070252284096,
0.15998263546747513,
0.15700135221750686
] | true | partially_addressed | 1 | 7 | intact | [
"1304.7777"
] | Paper 1304.7777 investigates YSOs in the Lynds 1641 cloud, deriving accretion rates and disk properties, which contributes evidence relevant to the question of how these compare to theoretical models. | 0.9 | gpt-4o |
What are the underlying mechanisms that determine the semi-major axes and eccentricities of extrasolar planets, given the discrepancies observed in their orbital elements compared to predictions from the core accretion model? | evidence_tension | {"cluster": [{"arxiv_id": "astro-ph/0501313", "published": "2005-01-15", "sentence": "However, the core accretion mechanism is not refined to the point of explaining orbital parameters such as their unexpected semi-major axes and eccentricities."}, {"arxiv_id": "0708.0335", "published": "2007-08-02", "sentence": "The e... | protoplanetary_disks-2012-003 | protoplanetary_disks | 2,012 | 2012-12-31T00:00:00 | null | 31 | 0 | 0 | 1 | 1 | 1 | 0 | 0 | 0 | 0 | 0 | 0.273303 | 0.2048 | 11 | 1 | 0.2 | 3.7 | 2.147091 | 0.3 | 2 | 2 | 1 | 0.273303 | 0.726697 | 0.180195 | 0 | 1 | 0.036849 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 1,211 | 0.029851 | 1.388316 | 26 | 2 | 1 | 1 | 0 | 0 | 0 | 0 | 15 | null | null | false | [
"1507.05209",
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"1312.7512",
"1710.03019",
"1504.01160",
"1704.03265",
"1512.08182",
"1606.04510"
] | [
0.1664029360265615,
0.15238149310966734,
0.15192340850029415,
0.15136804595317704,
0.14974562987318735,
0.14092327278600944,
0.1404317723352722,
0.14004037987364187
] | false | not_addressed | 0 | 8 | intact | [] | None of the candidate papers directly investigate the mechanisms determining the semi-major axes and eccentricities of extrasolar planets in relation to the core accretion model discrepancies. | 1 | gpt-4o |
What is the relationship between the observed PAH emission brightness toward HD100546 and the classification of T Tauri stars versus Class I stars in edge-on disk orientations? | evidence_tension | {"cluster": [{"arxiv_id": "astro-ph/0501582", "published": "2005-01-26", "sentence": "Part of the jet emission from edge-on systems is directly visible to us in the forbidden lines as well as in Halpha and He I, a finding which contradicts the present paradigm of a pure magnetospheric accretion origin for the formation... | protoplanetary_disks-2012-004 | protoplanetary_disks | 2,012 | 2012-12-31T00:00:00 | null | 27 | 1 | 0 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 1 | 0.229396 | 0.180862 | 5 | 3 | 0.2 | 3.8 | 1.989975 | 0.2 | 4 | 4 | 1 | 0.229396 | 0.770604 | 0.157528 | 0 | 1 | 0.089497 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1,211 | 0.029851 | 1.388316 | 26 | 2 | 1 | 1 | 0 | 0 | 0 | 0 | 8 | null | null | false | [
"1305.3138",
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"1302.7122",
"1608.00986",
"1612.09454",
"1512.04992",
"1402.0902",
"1511.03431"
] | [
0.14935947575106626,
0.1376800744276942,
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0.1328836978087612,
0.1277476343343246,
0.12768072294874613,
0.12516625243630553,
0.12285196091836294
] | false | not_addressed | 0 | 8 | intact | [] | None of the candidate papers directly investigate the relationship between PAH emission brightness toward HD100546 and the classification of T Tauri versus Class I stars in edge-on disk orientations. | 1 | gpt-4o |
What are the underlying physical processes that lead to the differences in temperature and evolutionary characteristics of debris disks around A stars compared to FGK stars, and how do these processes relate to the observed discrepancies in disk mass measurements and the population of misaligned hot Jupiters? | evidence_tension | {"cluster": [{"arxiv_id": "astro-ph/0503445", "published": "2005-03-21", "sentence": "This model also suggests that the disk is in a transient, excited dynamical state, as the observed dust creation rate applied over the age of the star is inconsistent with submillimeter mass measurements."}, {"arxiv_id": "1211.6365", ... | protoplanetary_disks-2012-005 | protoplanetary_disks | 2,012 | 2012-12-31T00:00:00 | null | 47 | 0 | 0 | 1 | 1 | 1 | 1 | 0 | 0 | 0 | 1 | 0.176269 | 0.158151 | 3 | 2 | 0.3 | 2.5 | 1.910497 | 0.6 | 4 | 7 | 1 | 0.176269 | 0.823731 | 0.146191 | 0 | 1 | 0.165733 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1 | 1,211 | 0.029851 | 1.388316 | 26 | 2 | 1 | 1 | 0 | 0 | 0 | 0 | 12 | null | null | false | [
"1612.04372",
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"1712.01035",
"1404.1954",
"1701.02890",
"1503.01320",
"1507.07967",
"1604.05191"
] | [
0.17632748341749005,
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0.1534384589639375,
0.13347222009586082,
0.13168403564044778,
0.1298406072547564
] | false | not_addressed | 0 | 8 | intact | [] | None of the candidate papers directly investigate the specific question of the underlying physical processes leading to differences in debris disks around A stars compared to FGK stars, nor do they address the discrepancies in disk mass measurements and the population of misaligned hot Jupiters. | 1 | gpt-4o |
What are the physical properties and size distribution of dust particles in protoplanetary disks around Herbig Ae/Be stars, and how do they affect the observed near-IR excess and spectral features, particularly in regions inward of 1 AU? | evidence_tension | {"cluster": [{"arxiv_id": "astro-ph/0506154", "published": "2005-06-07", "sentence": "The rim can produce the observed near-IR excess only if its dust has perfectly gray opacity, but such dust is in conflict with the observed 10$μ$m spectral feature."}, {"arxiv_id": "astro-ph/0602030", "published": "2006-02-01", "sente... | protoplanetary_disks-2012-006 | protoplanetary_disks | 2,012 | 2012-12-31T00:00:00 | null | 37 | 0 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 1 | 0.226706 | 0.198049 | 25 | 3 | 0.2 | 4.7 | 2.368544 | 0.2 | 4 | 7 | 1 | 0.226706 | 0.773294 | 0.18281 | 3 | 0 | 0.174039 | 0 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1,211 | 0.029851 | 1.388316 | 26 | 2 | 1 | 1 | 0 | 0 | 0 | 4 | 50 | 2013-03-23T00:00:00 | 3 | false | [
"1308.6777",
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"1303.5853",
"1311.5131",
"1305.3138",
"1405.4494",
"1510.07948",
"1601.07542"
] | [
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0.17618586181772738,
0.17380798926311952,
0.17326508891216233,
0.17026472505063936
] | false | not_addressed | 0 | 7 | intact | [] | None of the candidate papers directly investigate the physical properties and size distribution of dust particles in protoplanetary disks around Herbig Ae/Be stars or their effect on near-IR excess and spectral features inward of 1 AU. | 0.9 | gpt-4o |
How do the optically thick inner regions of protostellar disks influence the relationship between luminosity and interferometric inner radii, and what is their contribution to millimeter dust flux? | evidence_tension | {"cluster": [{"arxiv_id": "astro-ph/0506154", "published": "2005-06-07", "sentence": "Furthermore, this model also resolves the puzzling relationship noted by Monnier and Millan-Gabet (2002) between luminosity and the interferometric inner radii of disks."}, {"arxiv_id": "1006.3485", "published": "2010-06-17", "sentenc... | protoplanetary_disks-2012-007 | protoplanetary_disks | 2,012 | 2012-12-31T00:00:00 | null | 28 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 0 | 1 | 0.198415 | 0.175998 | 7 | 2 | 0.4 | 4.3 | 2.410394 | 0.4 | 3 | 6 | 1 | 0.198415 | 0.801585 | 0.163119 | 0 | 1 | 0.112228 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1,211 | 0.029851 | 1.388316 | 26 | 2 | 1 | 1 | 0 | 0 | 0 | 0 | 14 | null | null | false | [
"1512.02276",
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"1311.5131",
"1404.0709",
"1709.06514",
"1706.08977",
"1612.06311",
"1705.06888"
] | [
0.1590858487785305,
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0.14872869784289602,
0.1408688698080804,
0.13889338575405102,
0.137767487069566,
0.132690094585213
] | true | partially_addressed | 1 | 7 | intact | [
"1706.08977"
] | Paper 1706.08977 provides empirical evidence of a correlation between millimeter continuum sizes and luminosities in protoplanetary disks, contributing to understanding the influence of optically thick inner regions on these properties. However, it does not fully resolve the question of their contribution to millimeter... | 0.9 | gpt-4o |
What are the physical properties and composition of the debris disks identified around the stars in the studies referenced, and how do they differ from the expected characteristics of stellar or substellar companions? | evidence_tension | {"cluster": [{"arxiv_id": "astro-ph/0509188", "published": "2005-09-07", "sentence": "Combining infrared photometric and spectroscopic observations, we show that the excess radiation cannot be explained by a stellar or substellar companion, and is likely to be caused by a debris disk."}, {"arxiv_id": "astro-ph/0603774"... | protoplanetary_disks-2012-008 | protoplanetary_disks | 2,012 | 2012-12-31T00:00:00 | null | 33 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0.12752 | 0.123583 | 0 | 2 | 0.1 | 1.8 | 2.088061 | 0.7 | 4 | 7 | 1 | 0.12752 | 0.87248 | 0.117733 | 0 | 1 | 0.12266 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1,211 | 0.029851 | 1.388316 | 26 | 2 | 1 | 1 | 0 | 0 | 0 | 0 | 13 | null | null | false | [
"1710.04185",
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"1501.03813",
"1302.5367",
"1502.05412",
"1503.01320",
"1604.06456",
"1305.5107"
] | [
0.17675521872971614,
0.17142716340888853,
0.1678456117783497,
0.14833784851444198,
0.14648968230216464,
0.1464672790252253,
0.1423074614866761,
0.13590649644451358
] | false | not_addressed | 0 | 8 | intact | [] | None of the candidate papers directly investigate the physical properties and composition of debris disks or compare them to stellar or substellar companions. They focus on related topics such as planet detection, stellar multiplicity, and substellar companions. | 1 | gpt-4o |
What are the physical characteristics and evolutionary status of BP Psc that contribute to its classification as a puzzling late-type, emission-line field star with large infrared excess, and how do these characteristics compare to the low mass stars (2.4 to 2.8 solar masses) discussed in the context of Hubrig et al.'s... | evidence_tension | {"cluster": [{"arxiv_id": "astro-ph/0509295", "published": "2005-09-12", "sentence": "The low masses inferred for these objects (2.6, 2.8 and 2.4 solar masses) represent additional contradictions to the hypothesis of Hubrig et al."}, {"arxiv_id": "1110.5755", "published": "2011-10-26", "sentence": "This discrepancy is ... | protoplanetary_disks-2012-009 | protoplanetary_disks | 2,012 | 2012-12-31T00:00:00 | null | 52 | 0 | 2 | 0 | 1 | 0 | 1 | 0 | 0 | 0 | 3 | 0.284791 | 0.179916 | 2 | 3 | 0.3 | 4 | 2.366432 | 0.2 | 3 | 6 | 1 | 0.284791 | 0.715209 | 0.148629 | 0 | 1 | 0.114849 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1,211 | 0.029851 | 1.388316 | 26 | 2 | 1 | 1 | 0 | 0 | 0 | 1 | 5 | 2016-10-20T00:00:00 | 46 | false | [
"1610.06609",
"1701.06568",
"1704.08133",
"1608.04480",
"1304.4435",
"1501.03813",
"1712.02819",
"1405.7378"
] | [
0.21964052651470986,
0.15626261863912963,
0.14604459614658807,
0.12532698919256235,
0.12225186460839566,
0.11501748028156046,
0.11149446100971737,
0.10980677133828581
] | true | posed_but_open | 1 | 7 | intact | [
"1610.06609"
] | The paper [1610.06609] directly investigates BP Psc, discussing its classification as either a pre-main sequence T Tauri star or a post-main sequence G giant, but does not provide a definitive resolution, leaving the question open. | 1 | gpt-4o |
What are the precise mechanisms and conditions that lead to the formation of planetesimals from dust in protoplanetary disks? | direct_llm | {"n_titles_shown": 60} | protoplanetary_disks-2012-010 | protoplanetary_disks | 2,012 | 2012-12-31T00:00:00 | null | 19 | 0 | 0 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0.147274 | 0.142502 | 0 | 1 | 0 | 3.2 | 1.720465 | 0.3 | 0 | 0 | 0 | 0.147274 | 0.852726 | 0.135235 | 0 | 1 | 0.137341 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1,211 | 0.029851 | 1.388316 | 26 | 2 | 1 | 1 | 0 | 0 | 0 | 0 | 16 | null | null | false | [
"1403.6552",
"1404.5018",
"1409.7041",
"1407.8211",
"1307.0463",
"1512.04996",
"1607.05734",
"1610.09643"
] | [
0.16730544630672928,
0.16314427605287074,
0.15378804139773167,
0.1498560298367576,
0.14965105670742376,
0.14798236375574944,
0.14772880893304402,
0.14527386962633254
] | true | partially_addressed | 3 | 5 | intact | [
"1403.6552",
"1607.05734",
"1610.09643"
] | Papers 1403.6552, 1607.05734, and 1610.09643 contribute substantive new evidence on the mechanisms and conditions for planetesimal formation, such as gravitational instability and pebble drift, but do not fully settle the question. They explore specific conditions and processes that could lead to planetesimal formation... | 0.9 | gpt-4o |
How do the dynamics of gas and dust in protoplanetary disks influence the migration patterns of forming planets, particularly in the context of different disk environments? | direct_llm | {"n_titles_shown": 60} | protoplanetary_disks-2012-011 | protoplanetary_disks | 2,012 | 2012-12-31T00:00:00 | null | 26 | 0 | 0 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0.184014 | 0.165375 | 4 | 3 | 0 | 2.8 | 2.135416 | 0.6 | 0 | 0 | 0 | 0.184014 | 0.815986 | 0.153118 | 0 | 1 | 0.09156 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1,211 | 0.029851 | 1.388316 | 26 | 2 | 1 | 1 | 0 | 0 | 0 | 0 | 11 | null | null | false | [
"1611.02928",
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"1311.1819",
"1307.5916",
"1506.00430",
"1310.7092",
"1512.05920",
"1612.03174"
] | [
0.1688346345712915,
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0.14367044951135904,
0.13972873285504614,
0.1294009248163844,
0.1287200217347356,
0.12862838899859716,
0.12702309354286645
] | true | partially_addressed | 2 | 5 | intact | [
"1506.00430",
"1512.05920"
] | Papers 1506.00430 and 1512.05920 contribute substantive new evidence on the dynamics of gas and dust in protoplanetary disks and their influence on planet migration, particularly through the study of grain accumulation and toroidal vortices. However, the question is not fully settled. | 0.9 | gpt-4o |
What role do magnetic fields play in the evolution and stability of protoplanetary disks, and how do they affect planet formation processes? | direct_llm | {"n_titles_shown": 60} | protoplanetary_disks-2012-012 | protoplanetary_disks | 2,012 | 2012-12-31T00:00:00 | null | 22 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0.203609 | 0.194354 | 31 | 0 | 0 | 3.4 | 1.74356 | 0.4 | 0 | 0 | 0 | 0.203609 | 0.796391 | 0.184107 | 3 | 0 | 0.106913 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1,211 | 0.029851 | 1.388316 | 26 | 2 | 1 | 1 | 0 | 0 | 0 | 7 | 49 | 2014-02-09T00:00:00 | 14 | false | [
"1402.7130",
"1409.2878",
"1503.02403",
"1609.02085",
"1707.04110",
"1402.1903",
"1711.08636",
"1503.04901"
] | [
0.28595000637254914,
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0.21896627909251937,
0.20610295867353806,
0.2008578536862443,
0.19451950601516124,
0.1859328240786795,
0.16490638645996206
] | true | partially_addressed | 1 | 7 | intact | [
"1609.02085"
] | Paper 1609.02085 directly investigates the influence of magnetic fields on the evolution of protoplanetary disks and planet formation processes through simulations and observations, providing substantive new evidence on the question. | 0.9 | gpt-4o |
How does the presence of binary stars impact the formation and evolution of protoplanetary disks and the subsequent formation of planets within those systems? | direct_llm | {"n_titles_shown": 60} | protoplanetary_disks-2012-013 | protoplanetary_disks | 2,012 | 2012-12-31T00:00:00 | null | 24 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0.227365 | 0.218104 | 41 | 2 | 0 | 2.7 | 1.486607 | 0.4 | 0 | 0 | 0 | 0.227365 | 0.772635 | 0.203126 | 1 | 0 | 0.166035 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1,211 | 0.029851 | 1.388316 | 26 | 2 | 1 | 1 | 0 | 0 | 0 | 4 | 50 | 2015-01-04T00:00:00 | 25 | false | [
"1509.05217",
"1703.04304",
"1501.00617",
"1604.03121",
"1507.08215",
"1311.2942",
"1501.03813",
"1610.05842"
] | [
0.22762057229506613,
0.21280369818883937,
0.20310157455019762,
0.18108922343474054,
0.17698032852411547,
0.1715238868365515,
0.16962493474895637,
0.16588349003140956
] | true | partially_addressed | 4 | 4 | intact | [
"1703.04304",
"1501.00617",
"1604.03121",
"1610.05842"
] | Papers 1703.04304, 1501.00617, 1604.03121, and 1610.05842 provide substantive evidence on how binary stars impact protoplanetary disks and planet formation, including effects on disk turbulence, truncation, planet scattering, and coevolution of binaries and disks. However, the question is not fully settled. | 1 | gpt-4o |
What are the effects of varying chemical compositions and temperature gradients within protoplanetary disks on the formation and diversity of planetary systems? | direct_llm | {"n_titles_shown": 60} | protoplanetary_disks-2012-014 | protoplanetary_disks | 2,012 | 2012-12-31T00:00:00 | null | 22 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 0 | 1 | 0.203977 | 0.17955 | 7 | 2 | 0 | 1.8 | 1.83303 | 0.8 | 0 | 0 | 0 | 0.203977 | 0.796023 | 0.162882 | 3 | 0 | 0.104137 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1,211 | 0.029851 | 1.388316 | 26 | 2 | 1 | 1 | 0 | 0 | 0 | 0 | 20 | null | null | false | [
"1405.3253",
"1606.09174",
"1611.09658",
"1312.4293",
"1407.7271",
"1612.03174",
"1611.00741",
"1312.3085"
] | [
0.1674279224345523,
0.16202135306852497,
0.16112889173871642,
0.15803799928629336,
0.15749195266094712,
0.14611679259935786,
0.1454125656098754,
0.13077555525183573
] | true | partially_addressed | 3 | 4 | intact | [
"1405.3253",
"1606.09174",
"1611.00741"
] | Papers 1405.3253, 1606.09174, and 1611.00741 directly investigate the effects of chemical compositions and temperature gradients in protoplanetary disks on planet formation and diversity. They provide models and evidence on how these factors influence planetesimal and planetary compositions, contributing substantive ne... | 1 | gpt-4o |
What are the dominant ions below the transition and how do they depend on the abundances of heavy elements? | future_work | {"statement": {"arxiv_id": "1105.3453", "published": "2011-05-17", "sentence": "The nature of the dominant ions below the transition depends sensitively on the poorly constrained abundances of the heavy elements."}} | protoplanetary_disks-2012-015 | protoplanetary_disks | 2,012 | 2012-12-31T00:00:00 | null | 19 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0.354247 | 0.233938 | 6 | 3 | 0.2 | 1.6 | 0.916515 | 0.8 | 0 | 0 | 0 | 0.354247 | 0.645753 | 0.183694 | 3 | 0 | 0.063218 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1,211 | 0.029851 | 1.388316 | 26 | 2 | 1 | 1 | 0 | 0 | 0 | 1 | 11 | 2017-05-25T00:00:00 | 53 | false | [
"1705.09320",
"1606.04510",
"1606.04162",
"1708.08942",
"1512.08182",
"1509.02741",
"1607.03701",
"1702.07522"
] | [
0.18546999377047418,
0.17223282203894474,
0.16876653468484842,
0.16226891052938786,
0.15832753855233136,
0.1446571517181861,
0.13448278954578824,
0.13033480667982222
] | false | not_addressed | 0 | 8 | intact | [] | None of the candidate papers directly investigate the dominant ions below the transition or their dependence on heavy element abundances. They are related to planetary formation and ionization processes but do not address the specific question. | 1 | gpt-4o |
What are the implications of the 'concurrent collapse' hypothesis for poorly understood phenomena in planet formation? | future_work | {"statement": {"arxiv_id": "0802.4099", "published": "2008-02-27", "sentence": "This 'concurrent collapse' hypothesis avoids theoretical difficulties associated with the conventional model and suggests satisfying explanations for various poorly understood phenomena."}} | protoplanetary_disks-2012-016 | protoplanetary_disks | 2,012 | 2012-12-31T00:00:00 | null | 16 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0.4655 | 0.187193 | 1 | 3 | 0.2 | 3.1 | 1.813836 | 0.5 | 0 | 0 | 0 | 0.4655 | 0.5345 | 0.141495 | 1 | 0 | 0.07662 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1,211 | 0.029851 | 1.388316 | 26 | 2 | 1 | 0 | 0 | 0 | 0 | 0 | 1 | null | null | false | [
"1611.02928",
"1403.0168",
"1307.4864",
"1601.03608",
"1401.0408",
"1505.01842",
"1303.6442",
"1302.1389"
] | [
0.14978215909133225,
0.10893590130689731,
0.09940180044040492,
0.09817254012275417,
0.09733067425209636,
0.09722479139049872,
0.09503133965678666,
0.09308732406618142
] | false | not_addressed | 0 | 7 | intact | [] | None of the candidate papers directly investigate the 'concurrent collapse' hypothesis or its implications for planet formation phenomena. They are either adjacent or unrelated. | 1 | gpt-4o |
What are the reasons for the discrepancies in the derived magnitude of turbulence between local and global simulations of magneto-rotationally unstable disks? | future_work | {"statement": {"arxiv_id": "0907.1897", "published": "2009-07-10", "sentence": "Discrepancies in the derived magnitude of turbulence between local and global simulations of magneto-rotationally unstable disks remains an open issue, with important consequences for planet formation scenarios."}} | protoplanetary_disks-2012-017 | protoplanetary_disks | 2,012 | 2012-12-31T00:00:00 | null | 22 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 0 | 1 | 0.290753 | 0.187626 | 4 | 0 | 0.2 | 2.6 | 1.56205 | 0.5 | 0 | 0 | 0 | 0.290753 | 0.709247 | 0.156067 | 0 | 1 | 0.033496 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 1,211 | 0.029851 | 1.388316 | 26 | 2 | 1 | 1 | 0 | 0 | 1 | 1 | 5 | 2013-04-16T00:00:00 | 4 | false | [
"1304.4647",
"1403.7607",
"1510.01375",
"1310.5865",
"1607.00323",
"1607.01792",
"1304.6037",
"1501.02808"
] | [
0.2003180086441371,
0.16026626463353605,
0.13410474223185076,
0.13212978069954617,
0.12239607195998566,
0.11817572938435636,
0.10907443564722999,
0.10742711597118548
] | false | not_addressed | 0 | 8 | intact | [] | None of the candidate papers directly investigate the discrepancies in turbulence magnitude between local and global simulations of magneto-rotationally unstable disks. | 1 | gpt-4o |
What is the nature of the circumstellar environment of T Tauri, and why is it elusive? | future_work | {"statement": {"arxiv_id": "0712.1595", "published": "2007-12-10", "sentence": "Although T Tauri is one of the most studied young objects in astronomy, the nature of its circumstellar environment remains elusive due, in part, to the small angular separation of its three components (North-South and South a-b are separat... | protoplanetary_disks-2012-018 | protoplanetary_disks | 2,012 | 2012-12-31T00:00:00 | null | 16 | 0 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0.181059 | 0.130472 | 1 | 2 | 0.1 | 4.1 | 1.640122 | 0.3 | 0 | 0 | 0 | 0.181059 | 0.818941 | 0.118361 | 1 | 0 | 0.061193 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1,211 | 0.029851 | 1.388316 | 26 | 2 | 1 | 0 | 0 | 0 | 0 | 0 | 5 | null | null | false | [
"1302.5357",
"1311.4832",
"1504.05198",
"1709.00420",
"1602.04665",
"1512.09027",
"1509.05354",
"1308.6308"
] | [
0.16147047599908104,
0.15749031049822157,
0.1426824299581221,
0.13247952069854,
0.12340284190911302,
0.11056423893700863,
0.10623165532190669,
0.10335310693270464
] | true | partially_addressed | 2 | 5 | intact | [
"1311.4832",
"1602.04665"
] | Paper [1311.4832] provides direct imaging of the circumstellar environment of a T Tauri star, contributing evidence on its structure. Paper [1602.04665] investigates wind dynamics and circumstellar extinction variations, offering insights into the elusive nature of the environment. Together, they contribute substantive... | 0.9 | gpt-4o |
What is the precise location of the water ice condensation front ('snow line') in the protosolar nebula? | future_work | {"statement": {"arxiv_id": "1012.0727", "published": "2010-12-03", "sentence": "The precise location of the water ice condensation front ('snow line') in the protosolar nebula has been a debate for a long time."}} | protoplanetary_disks-2012-019 | protoplanetary_disks | 2,012 | 2012-12-31T00:00:00 | null | 17 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0.433148 | 0.326754 | 13 | 0 | 0 | 2 | 2.04939 | 0.6 | 0 | 0 | 0 | 0.433148 | 0.566852 | 0.254641 | 2 | 0 | 0.084534 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1,211 | 0.029851 | 1.388316 | 26 | 2 | 1 | 1 | 0 | 1 | 1 | 15 | 43 | 2013-01-23T00:00:00 | 1 | false | [
"1607.03757",
"1402.5333",
"1505.03516",
"1411.7618",
"1708.03360",
"1407.2568",
"1512.02414",
"1710.00009"
] | [
0.24270555996829188,
0.23652473801386587,
0.22646045963772882,
0.221487033508212,
0.20799672184774526,
0.20729376281511416,
0.20301061571920143,
0.20140213345024774
] | false | not_addressed | 0 | 8 | intact | [] | None of the candidate papers directly investigate the precise location of the water ice condensation front in the protosolar nebula. They discuss related topics such as snow lines in other contexts or theoretical implications, but do not provide direct evidence or analysis for the specific question posed. | 1 | gpt-4o |
How does the presence of gas phase CO below its freezing temperature in circumstellar disks relate to the detection of radio pulsars in these systems using the Green Bank Telescope? | control | {"claim_a": {"arxiv_id": "0812.1714", "sentence": "We attempt to understand the presence of gas phase CO below its freezing temperature in circumstellar disks."}, "claim_b": {"arxiv_id": "1106.5550", "sentence": "Here we present an attempt to detect radio pulsars in both systems with the Green Bank Telescope."}} | protoplanetary_disks-2012-020 | protoplanetary_disks | 2,012 | 2012-12-31T00:00:00 | random_pair | 30 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 0 | 1 | 0.190258 | 0.129306 | 1 | 2 | 0.3 | 3.7 | 2.282542 | 0.3 | 0 | 0 | 0 | 0.190258 | 0.809742 | 0.109739 | 0 | 1 | 0.061367 | 1 | 0 | 0 | 1 | 1 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 1,211 | 0.029851 | 1.388316 | 26 | 2 | 1 | 1 | 0 | 0 | 0 | 1 | 4 | 2014-02-16T00:00:00 | 14 | false | [
"1402.3750",
"1507.06982",
"1609.06409",
"1512.05836",
"1604.08286",
"1701.02049",
"1705.08444",
"1706.05562"
] | [
0.1849692323464937,
0.16112427699187676,
0.15298163802260925,
0.1305184690537211,
0.11601260695714645,
0.11451168938325018,
0.09883099566681414,
0.09357364382531333
] | false | not_addressed | 0 | 8 | intact | [] | None of the candidate papers directly investigate the relationship between gas phase CO below its freezing temperature in circumstellar disks and the detection of radio pulsars using the Green Bank Telescope. | 1 | gpt-4o |
What are the implications of gravitational collapse in magnetised discs for the orbital dynamics of Moon- to Mars-sized objects in a circumprimary disk influenced by a Jovian-type planet and a secondary star? | control | {"claim_a": {"arxiv_id": "astro-ph/0702706", "sentence": "We consider a circumprimary disk of Moon- to Mars-sized objects and numerically integrate the orbits of these bodies at the presence of the Jovian-type planet of the system and for different values of the mass, semimajor axis, and orbital eccentricity of the sec... | protoplanetary_disks-2012-021 | protoplanetary_disks | 2,012 | 2012-12-31T00:00:00 | random_pair | 32 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0.303147 | 0.18994 | 4 | 0 | 0.1 | 2.9 | 1.445683 | 0.3 | 0 | 0 | 0 | 0.303147 | 0.696853 | 0.163021 | 0 | 1 | 0.066709 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1,211 | 0.029851 | 1.388316 | 26 | 2 | 1 | 0 | 0 | 0 | 0 | 0 | 10 | null | null | false | [
"1405.5056",
"1312.3959",
"1509.04859",
"1406.2697",
"1611.02928",
"1508.02879",
"1607.03038",
"1402.0037"
] | [
0.16814265542894719,
0.15969441376496218,
0.1501932211687036,
0.13790535688403702,
0.1335490146780497,
0.12533581896849255,
0.12479465310287738,
0.12392330579264497
] | false | not_addressed | 0 | 8 | intact | [] | None of the candidate papers directly investigate the implications of gravitational collapse in magnetised discs for the orbital dynamics of Moon- to Mars-sized objects in a circumprimary disk influenced by a Jovian-type planet and a secondary star. | 1 | gpt-4o |
What is the nature of the processes governing the formation and evolution of protoplanetary disks and their role in planet formation? | control | {} | protoplanetary_disks-2012-022 | protoplanetary_disks | 2,012 | 2012-12-31T00:00:00 | vague | 21 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0.280594 | 0.196866 | 7 | 1 | 0 | 3.1 | 2.022375 | 0.5 | 0 | 0 | 0 | 0.280594 | 0.719406 | 0.172996 | 2 | 0 | 0.132443 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1,211 | 0.029851 | 1.388316 | 26 | 2 | 1 | 0 | 0 | 0 | 0 | 0 | 11 | null | null | false | [
"1402.1354",
"1409.7102",
"1611.09658",
"1708.09345",
"1308.1791",
"1510.08021",
"1311.1819",
"1402.7086"
] | [
0.17979651821694695,
0.16958573306450941,
0.16664763287428072,
0.15486403335125987,
0.15154455699639807,
0.14367445730247977,
0.13732985776707518,
0.13323789024796598
] | true | partially_addressed | 5 | 3 | intact | [
"1402.1354",
"1611.09658",
"1708.09345",
"1308.1791",
"1311.1819"
] | The direct candidates provide substantive new evidence on various aspects of protoplanetary disk formation and evolution, such as dust evolution, gas disk chemistry, and disk dispersal, contributing to a partial understanding of the processes involved in planet formation. | 0.9 | gpt-4o |
How might the proposed model of disc-planet interaction influence our understanding of the fundamental characteristics of disc masses and accretion rates in the context of disc clearing? | control | {"arxiv_id": "astro-ph/0611821", "sentence": "Lastly, we consider a simple model of the disc-planet interaction, and suggest that observations of disc masses and accretion rates provide a straightforward means of discriminating between different models of disc clearing."} | protoplanetary_disks-2012-023 | protoplanetary_disks | 2,012 | 2012-12-31T00:00:00 | untestable | 27 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 0 | 1 | 0.314612 | 0.206276 | 8 | 2 | 0 | 3.1 | 2.118962 | 0.5 | 0 | 0 | 0 | 0.314612 | 0.685388 | 0.17893 | 13 | 0 | 0.057631 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 1,211 | 0.029851 | 1.388316 | 26 | 2 | 1 | 1 | 0 | 0 | 1 | 1 | 31 | 2015-04-20T00:00:00 | 28 | false | [
"1504.05198",
"1609.04527",
"1405.5056",
"1512.02234",
"1611.07376",
"1309.0508",
"1405.3283",
"1310.4203"
] | [
0.1830183529476937,
0.17603222628529439,
0.1753424538124758,
0.169075429853697,
0.1598355041812046,
0.15813083276069742,
0.1557913442638957,
0.1546841301170474
] | false | not_addressed | 0 | 8 | intact | [] | None of the candidate papers directly investigate the proposed model of disc-planet interaction's influence on disc masses and accretion rates in the context of disc clearing. | 1 | gpt-4o |
Could the rapid disappearance of warm, dusty circumstellar disks suggest that the mechanisms of planet formation are fundamentally different from the currently accepted models? | control | {"arxiv_id": "1207.1162", "title": "Rapid disappearance of a warm, dusty circumstellar disk"} | protoplanetary_disks-2012-024 | protoplanetary_disks | 2,012 | 2012-12-31T00:00:00 | consensus_challenge | 24 | 0 | 0 | 1 | 1 | 1 | 0 | 0 | 0 | 1 | 0 | 0.223928 | 0.130071 | 1 | 3 | 0 | 2.6 | 2.332381 | 0.6 | 0 | 0 | 0 | 0.223928 | 0.776072 | 0.108668 | 0 | 1 | 0.066334 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 1,211 | 0.029851 | 1.388316 | 26 | 2 | 1 | 1 | 0 | 0 | 1 | 0 | 1 | null | null | false | [
"1604.03775",
"1303.2393",
"1405.5284",
"1711.03548",
"1312.3835",
"1608.05410",
"1607.03115",
"1407.8211"
] | [
0.1254161019294976,
0.10963473753616249,
0.10271656214240724,
0.09630833683797267,
0.09332070977672886,
0.09198482138612778,
0.08983448804539108,
0.0896085879243406
] | true | partially_addressed | 1 | 7 | intact | [
"1608.05410"
] | Paper 1608.05410 provides evidence that the rapid disappearance of warm, dusty circumstellar disks may be linked to a quicker or different process of rocky planet formation than previously thought, partially addressing the question. | 0.9 | gpt-4o |
What are the underlying physical mechanisms causing the observed radii of low-mass stars in eclipsing binaries to be approximately 10 percent larger than the predictions made by stellar structure models? | evidence_tension | {"cluster": [{"arxiv_id": "astro-ph/0511431", "published": "2005-11-15", "sentence": "However, even in these small numbers the detailed comparison of the observed masses and radii with theoretical predictions has revealed large disagreements."}, {"arxiv_id": "astro-ph/0701702", "published": "2007-01-24", "sentence": "T... | stellar_activity-2012-000 | stellar_activity | 2,012 | 2012-12-31T00:00:00 | null | 30 | 0 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 0 | 2 | 0.308649 | 0.221368 | 7 | 1 | 0.6 | 2.8 | 2.521904 | 0.4 | 4 | 3 | 1 | 0.308649 | 0.691351 | 0.18533 | 0 | 1 | 0.070755 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 519 | 0.012793 | 1.89781 | 4 | 1 | 1 | 1 | 0 | 0 | 1 | 1 | 9 | 2015-11-21T00:00:00 | 35 | false | [
"1511.06900",
"1707.07001",
"1308.1320",
"1608.04978",
"1404.0683",
"1706.02401",
"1605.03985",
"1601.05646"
] | [
0.20336989022122595,
0.17506238456723824,
0.15228730581342723,
0.1458260471116458,
0.12841084418441326,
0.12521015932418947,
0.12200291493575328,
0.12177192638358995
] | true | partially_addressed | 3 | 5 | intact | [
"1707.07001",
"1404.0683",
"1706.02401"
] | Papers 1707.07001, 1404.0683, and 1706.02401 provide evidence on the role of magnetic activity and starspots in causing the observed radius inflation in low-mass stars, contributing to the understanding of the underlying mechanisms but not fully resolving the question. | 0.9 | gpt-4o |
What are the specific roles of stellar activity and metallicity in reconciling the discrepancies between theoretical and observed stellar radii in M-type stars and low-mass stars as indicated by eclipsing binaries? | evidence_tension | {"cluster": [{"arxiv_id": "astro-ph/0511431", "published": "2005-11-15", "sentence": "I review all the observational evidence on the properties of M-type stars and discuss a possible scenario based on stellar activity to explain the observed discrepancies."}, {"arxiv_id": "0711.3523", "published": "2007-11-22", "senten... | stellar_activity-2012-001 | stellar_activity | 2,012 | 2012-12-31T00:00:00 | null | 31 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 0 | 1 | 0.293213 | 0.214119 | 11 | 1 | 1 | 3.2 | 2.357965 | 0.3 | 4 | 5 | 1 | 0.293213 | 0.706787 | 0.18476 | 0 | 1 | 0.092644 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 519 | 0.012793 | 1.89781 | 4 | 1 | 1 | 1 | 0 | 0 | 1 | 0 | 8 | null | null | false | [
"1710.02524",
"1407.4249",
"1308.1320",
"1707.04335",
"1707.07001",
"1706.02401",
"1505.02860",
"1402.3027"
] | [
0.1485818821837314,
0.14414495397961646,
0.1404814758469043,
0.1342129327617046,
0.12895061049061443,
0.12260213579105717,
0.12187750621893187,
0.12103597032835427
] | true | partially_addressed | 3 | 2 | intact | [
"1707.07001",
"1706.02401",
"1505.02860"
] | Papers 1707.07001, 1706.02401, and 1505.02860 provide evidence on the roles of magnetic activity and metallicity in explaining the discrepancies in stellar radii of low-mass stars, contributing to the understanding of the question but not fully resolving it. | 0.9 | gpt-4o |
What are the characteristics of the plasma components present in the X-ray spectrum of the source with 345 counts, and how do they relate to the frequency change observed over time in relation to CME-driven shocks? | evidence_tension | {"cluster": [{"arxiv_id": "astro-ph/0511781", "published": "2005-11-29", "sentence": "Its X-ray spectrum, while only containing 345 counts, is inconsistent with a single-temperature component solar-abundance coronal plasma model, but implies either the presence of two or more plasma components, non-solar abundances, or... | stellar_activity-2012-002 | stellar_activity | 2,012 | 2012-12-31T00:00:00 | null | 36 | 0 | 1 | 1 | 0 | 0 | 1 | 0 | 0 | 0 | 2 | 0.173793 | 0.13965 | 1 | 0 | 0.3 | 3.5 | 2.109502 | 0.3 | 2 | 2 | 1 | 0.173793 | 0.826207 | 0.122255 | 1 | 0 | 0.14907 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 519 | 0.012793 | 1.89781 | 4 | 1 | 1 | 1 | 0 | 1 | 1 | 0 | 2 | null | null | false | [
"1607.06287",
"1703.05652",
"1709.05184",
"1404.4359",
"1509.09131",
"1508.01267",
"1512.04098",
"1702.04122"
] | [
0.12633033514506153,
0.12282532378335626,
0.11931436929087673,
0.11919854049623962,
0.11408846501310707,
0.11244393888519293,
0.10985837882822734,
0.10700135521976435
] | false | not_addressed | 0 | 5 | intact | [] | None of the candidate papers directly investigate the specific characteristics of the plasma components in the X-ray spectrum of the source with 345 counts or their relation to frequency changes over time in relation to CME-driven shocks. | 0.9 | gpt-4o |
What is the quantitative impact of chromospheric activity on the radius and temperature discrepancies observed in the secondary components of solar-type binaries, specifically in relation to the predicted values from current stellar evolution models? | evidence_tension | {"cluster": [{"arxiv_id": "astro-ph/0512072", "published": "2005-12-02", "sentence": "Current stellar evolution models agree well with the properties of the primary, but show a very large discrepancy in the radius of the secondary: the predicted values are about 10% smaller than observed (a 5-sigma effect)."}, {"arxiv_... | stellar_activity-2012-003 | stellar_activity | 2,012 | 2012-12-31T00:00:00 | null | 34 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 0 | 1 | 0.244144 | 0.229822 | 7 | 0 | 0.8 | 3.8 | 2.4 | 0.3 | 4 | 7 | 1 | 0.244144 | 0.755856 | 0.189416 | 0 | 1 | 0.095012 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 519 | 0.012793 | 1.89781 | 4 | 1 | 1 | 1 | 0 | 1 | 1 | 0 | 3 | null | null | false | [
"1710.02524",
"1706.02401",
"1410.1514",
"1705.04708",
"1611.01402",
"1412.5327",
"1608.04978",
"1407.4249"
] | [
0.15844247944094528,
0.14615547172674703,
0.13256939871517648,
0.11620934307186088,
0.11505097454317105,
0.1130400014790488,
0.11241055688310166,
0.1099032791257854
] | false | not_addressed | 0 | 6 | intact | [] | None of the candidate papers directly investigate the quantitative impact of chromospheric activity on radius and temperature discrepancies in solar-type binaries. | 1 | gpt-4o |
What are the implications of adopting lower mixing length parameters (l/H_p) on the evolutionary models of solar-type stars, particularly for stars with masses close to the Sun, such as the one referenced in astro-ph/0512072, and how do these models account for discrepancies in radius and mass relationships? | evidence_tension | {"cluster": [{"arxiv_id": "astro-ph/0512072", "published": "2005-12-02", "sentence": "These discrepancies are quite remarkable given that the star is only 7% less massive than the Sun, the calibration point of all stellar models."}, {"arxiv_id": "1202.4851", "published": "2012-02-22", "sentence": "Models adopting signi... | stellar_activity-2012-004 | stellar_activity | 2,012 | 2012-12-31T00:00:00 | null | 47 | 0 | 1 | 0 | 1 | 0 | 1 | 0 | 0 | 0 | 2 | 0.30906 | 0.202095 | 2 | 0 | 0.7 | 3.1 | 2.385372 | 0.4 | 4 | 7 | 1 | 0.30906 | 0.69094 | 0.154502 | 0 | 1 | 0.080907 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 519 | 0.012793 | 1.89781 | 4 | 1 | 1 | 1 | 0 | 0 | 1 | 0 | 5 | null | null | false | [
"1306.3490",
"1705.09668",
"1611.01402",
"1707.02165",
"1408.3475",
"1602.07815",
"1707.07001",
"1611.04329"
] | [
0.14599747243393935,
0.13835296341162176,
0.12928279753760796,
0.12582833440152208,
0.12047618795958863,
0.11973417060688288,
0.11781600875415198,
0.11285352670922032
] | false | not_addressed | 0 | 8 | intact | [] | None of the candidate papers directly investigate the implications of adopting lower mixing length parameters on evolutionary models of solar-type stars or address discrepancies in radius and mass relationships. | 1 | gpt-4o |
What are the underlying causes of the discrepancy in the X-ray Luminosity Functions between the Cep OB3b and the Orion Nebula Cluster, and how does the unexpected brightening of X-ray emission in March/April 2007 relate to these differences? | evidence_tension | {"cluster": [{"arxiv_id": "astro-ph/0601405", "published": "2006-01-18", "sentence": "Second, we find a discrepancy between the X-ray Luminosity Functions of the Cep OB3b and the Orion Nebula Cluster."}, {"arxiv_id": "1011.4062", "published": "2010-11-17", "sentence": "Unexpectedly, we find that the X-ray emission asso... | stellar_activity-2012-005 | stellar_activity | 2,012 | 2012-12-31T00:00:00 | null | 38 | 2 | 1 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 4 | 0.313211 | 0.185351 | 2 | 2 | 0.4 | 4.5 | 2.247221 | 0.3 | 3 | 4 | 1 | 0.313211 | 0.686789 | 0.144137 | 0 | 1 | 0.058902 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 519 | 0.012793 | 1.89781 | 4 | 1 | 1 | 1 | 0 | 0 | 1 | 0 | 2 | null | null | false | [
"1603.06144",
"1512.07000",
"1611.02141",
"1410.8554",
"1612.06570",
"1309.6970",
"1706.00833",
"1710.09385"
] | [
0.1500494260902145,
0.1405096016598483,
0.09568236598970556,
0.09207469745107127,
0.08913138936194527,
0.08422908627781253,
0.08383235583020474,
0.08297770790354465
] | false | not_addressed | 0 | 8 | intact | [] | None of the candidate papers directly investigate the discrepancy in X-ray Luminosity Functions between Cep OB3b and the Orion Nebula Cluster or the 2007 X-ray emission event. | 1 | gpt-4o |
What are the sources of the 'anomalously' high 6-Li and 7-Li abundances in the Galaxy if they cannot be explained by galactic cosmic-ray interactions in the interstellar medium? | evidence_tension | {"cluster": [{"arxiv_id": "astro-ph/0610756", "published": "2006-10-25", "sentence": "They cannot be explained by galactic cosmic-ray interactions in the interstellar medium either."}, {"arxiv_id": "0801.1777", "published": "2008-01-11", "sentence": "Although this nucleosynthesis is not significant for the chemical evo... | stellar_activity-2012-006 | stellar_activity | 2,012 | 2012-12-31T00:00:00 | null | 28 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 2 | 0.386814 | 0.268264 | 6 | 1 | 0.3 | 2.8 | 2.039608 | 0.4 | 2 | 2 | 1 | 0.386814 | 0.613186 | 0.20104 | 1 | 0 | 0.17037 | 0 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 519 | 0.012793 | 1.89781 | 4 | 1 | 1 | 1 | 0 | 0 | 1 | 2 | 8 | 2015-05-22T00:00:00 | 29 | false | [
"1505.06050",
"1609.05793",
"1306.3209",
"1706.09684",
"1710.05930",
"1509.00892",
"1611.03659",
"1703.10421"
] | [
0.22708789437371463,
0.19992627896933754,
0.17693976695447144,
0.1559175454834714,
0.14907764036624274,
0.14423210768207745,
0.13996507358591195,
0.12466040805990901
] | false | not_addressed | 0 | 8 | intact | [] | None of the candidate papers directly investigate the sources of anomalously high 6-Li and 7-Li abundances in the Galaxy or provide evidence that addresses this specific question. | 1 | gpt-4o |
What is the relationship between the total irradiance variation of the Sun and the chromospheric activity levels of stars with similar characteristics, and how does this relationship compare to the neon abundance discrepancies observed in the Sun versus other stars? | evidence_tension | {"cluster": [{"arxiv_id": "astro-ph/0703408", "published": "2007-03-15", "sentence": "The Sun's total irradiance variation, scaled to the b and y filter photometry, still appears to be somewhat smaller than stars in our limited sample with similar mean chromospheric activity, but we now regard this discrepancy as proba... | stellar_activity-2012-007 | stellar_activity | 2,012 | 2012-12-31T00:00:00 | null | 40 | 0 | 0 | 0 | 1 | 0 | 1 | 0 | 0 | 0 | 1 | 0.221585 | 0.195201 | 6 | 3 | 0.4 | 3.5 | 2.247221 | 0.4 | 2 | 1 | 1 | 0.221585 | 0.778415 | 0.166332 | 0 | 1 | 0.090813 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 519 | 0.012793 | 1.89781 | 4 | 1 | 1 | 1 | 0 | 0 | 1 | 2 | 14 | 2013-03-09T00:00:00 | 3 | false | [
"1303.2245",
"1407.4249",
"1605.08578",
"1508.02164",
"1406.2383",
"1508.00258",
"1412.3935",
"1607.01279"
] | [
0.2588641560728166,
0.22049419558124356,
0.1610190533852527,
0.15594402088025505,
0.15228073526504307,
0.1506660124086884,
0.14583329813520463,
0.13629329128846657
] | true | partially_addressed | 1 | 7 | intact | [
"1303.2245"
] | Paper 1303.2245 investigates the relationship between solar irradiance variability and chromospheric activity in Sun-like stars, providing evidence that the Sun is less variable than expected from empirical relationships. This partially addresses the question by contributing evidence on part of the relationship in ques... | 0.9 | gpt-4o |
What are the underlying causes of the significant discrepancies in distance estimates for approximately one third of the binary systems in the sample, and how do these discrepancies relate to the observed departure from linearity in the eclipse times of QS Vir? | evidence_tension | {"cluster": [{"arxiv_id": "0707.4107", "published": "2007-07-27", "sentence": "Approximately one third of the systems in our sample show a significant discrepancy between the two distance estimates."}, {"arxiv_id": "1005.3958", "published": "2010-05-21", "sentence": "We detect a large (~ 250 sec) departure from lineari... | stellar_activity-2012-008 | stellar_activity | 2,012 | 2012-12-31T00:00:00 | null | 42 | 0 | 0 | 1 | 0 | 0 | 1 | 0 | 0 | 0 | 1 | 0.235335 | 0.151105 | 3 | 3 | 0.6 | 2.6 | 2.154066 | 0.5 | 3 | 3 | 1 | 0.235335 | 0.764665 | 0.11859 | 0 | 1 | 0.065269 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 519 | 0.012793 | 1.89781 | 4 | 1 | 1 | 1 | 0 | 0 | 1 | 0 | 1 | null | null | false | [
"1306.0512",
"1505.02860",
"1301.3435",
"1508.02164",
"1606.05497",
"1703.02711",
"1407.4249",
"1710.02524"
] | [
0.1419781182371874,
0.10441755708180236,
0.10380797075050371,
0.0994958731350116,
0.0973563108170122,
0.09202927103724207,
0.0916847518360434,
0.08645676986718455
] | false | not_addressed | 0 | 7 | intact | [] | None of the candidate papers directly investigate the specific discrepancies in distance estimates for binary systems or the eclipse times of QS Vir. They are either adjacent, discussing related topics in binary systems or unrelated. | 1 | gpt-4o |
How do the dynamo fields of fully-convective stars influence the axisymmetry of their magnetic activity, and what is the relationship between these fields and the observed fluctuations in the Galactic magnetic field strength? | evidence_tension | {"cluster": [{"arxiv_id": "0711.1418", "published": "2007-11-09", "sentence": "This result is at odds with various theoretical predictions, suggesting that dynamo fields of fully-convective stars should be mostly non-axisymmetric unless they succeed at triggering significant differential rotation."}, {"arxiv_id": "1205... | stellar_activity-2012-009 | stellar_activity | 2,012 | 2012-12-31T00:00:00 | null | 33 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0.202716 | 0.179796 | 5 | 2 | 0.2 | 2.4 | 1.959592 | 0.5 | 2 | 5 | 1 | 0.202716 | 0.797284 | 0.162192 | 0 | 1 | 0.056755 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 519 | 0.012793 | 1.89781 | 4 | 1 | 1 | 1 | 0 | 0 | 1 | 6 | 37 | 2013-09-26T00:00:00 | 9 | false | [
"1610.02721",
"1606.00380",
"1609.07761",
"1309.7126",
"1707.04335",
"1309.6970",
"1408.1802",
"1509.00192"
] | [
0.23022660432349917,
0.22176603709718723,
0.2204175480608581,
0.21521068834738288,
0.21145011287628207,
0.20398112636926063,
0.17982904125137225,
0.1743341853362173
] | false | not_addressed | 0 | 7 | intact | [] | None of the candidate papers directly investigate the influence of dynamo fields of fully-convective stars on axisymmetry or their relationship with Galactic magnetic field fluctuations. | 1 | gpt-4o |
What are the precise mechanisms that govern the initiation and dynamics of coronal mass ejections (CMEs) in different types of stars, and how do these mechanisms vary with stellar age and magnetic activity? | direct_llm | {"n_titles_shown": 60} | stellar_activity-2012-010 | stellar_activity | 2,012 | 2012-12-31T00:00:00 | null | 33 | 0 | 0 | 1 | 1 | 1 | 1 | 0 | 0 | 0 | 1 | 0.161317 | 0.155971 | 4 | 0 | 0 | 2 | 1.48324 | 0.6 | 0 | 0 | 0 | 0.161317 | 0.838683 | 0.139636 | 0 | 1 | 0.065513 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 519 | 0.012793 | 1.89781 | 4 | 1 | 1 | 1 | 0 | 0 | 0 | 0 | 7 | null | null | false | [
"1611.05047",
"1612.06643",
"1704.06689",
"1309.3718",
"1308.0645",
"1707.00073",
"1403.0006",
"1611.02029"
] | [
0.15417933557741667,
0.13064047078935756,
0.12601253515201175,
0.12462569917636765,
0.12368128230926718,
0.12287038444106457,
0.12104027435851736,
0.116524591570692
] | false | not_addressed | 0 | 8 | intact | [] | None of the candidate papers directly investigate the mechanisms of CMEs in different types of stars or their variation with stellar age and magnetic activity. They are related to CMEs or stellar magnetic activity but do not address the specific question posed. | 1 | gpt-4o |
Scientific Question Outcomes
980 astronomy research questions, frozen at five historical cutoffs, each labelled with what the following five years of literature actually did with it.
Systems that propose research questions are usually evaluated by asking a person or a model how good the questions sound. This dataset supplies the alternative: questions frozen using only pre-cutoff literature, and outcome labels drawn from the literature published afterwards. It is, to our knowledge, the only public dataset that attaches future-outcome labels to questions — rather than to papers — across multiple historical cutoffs and with controlled generation sources.
What is in it
Each question was generated from the arXiv astro-ph record available strictly before its cutoff (2012, 2014, 2016, 2018, or 2020), across eight subfields, from four distinct sources:
| Source | n | Addressed within 5 years |
|---|---|---|
| Evidence-tension mining | 374 | 0.47 |
| Direct LLM elicitation | 200 | 0.88 |
| Author-stated future work | 196 | 0.51 |
| Weak/negative controls | 200 | 0.32 |
| Prior evidence-graph system | 10 | 0.20 |
The negative controls are deliberately weak questions — random claim pairings, vague questions, untestable questions, evidence-free contrarian questions — phrased by the same model so that surface style cannot separate them from real candidates. They exist so that any engagement metric computed on this data has a priced chance level. Without them, a model can only learn that question-shaped sentences succeed.
The direct-LLM rate of 0.88 should not be read as generator quality. A model asked in hindsight for the important open questions of 2016 may simply recall what 2017–2021 worked on; this is a documented leakage channel, not a result.
Configurations
default — 980 rows. Question text, provenance, a cutoff-time feature
record in six groups, and the outcome label.
structure — 374 rows, the tension-mined subset. Structural properties of
the evidence cluster each question was generated from: cluster breadth, tension
typology, quantification, instrument structure, and cross-cutoff recurrence.
second_judge — 200 rows. An independent second model's labels on all
premise-refuted cases plus a 20% random sample, for label-reliability work.
Fields
Question and provenance — question_id, question, subfield,
cutoff_year, cutoff_date, source, control_subtype, source_material
(verbatim generating evidence: sentences, arXiv ids, dates).
Features, all computed at cutoff time, by prefix:
| Prefix | Group | Examples |
|---|---|---|
txt_ |
text structure | entity count, causal/comparative language, specificity |
ev_ |
evidence context | similarity mass, instrument diversity, tension density |
nov_ |
novelty | nearest-neighbour distance, concept-pair novelty, review overlap |
fal_ |
falsifiability | observable, competing hypotheses, quantitative test |
tra_ |
tractability | operational vs. future facilities, archival data |
env_ |
field environment | publication volume, growth, next-facility proximity |
str_ |
evidence structure | cluster breadth, tension type, recurrence (structure config) |
Labels — addressed (bool), answer_status (answered /
partially_addressed / posed_but_open / premise_refuted / not_addressed),
premise_status, future_paper_count, first_follow_up_date,
lead_time_months, review_recognition, supporting_ids, rationale,
confidence, judge_model.
How the labels were made
Three tiers. First, automatic retrieval of future papers from each question's
subfield over its five-year future window. Second, a strict judge that sees
the question and its top-8 retrieved future records but never the generation
source; it classifies every candidate as direct, adjacent, or unrelated
before assigning an outcome, and addressed requires at least one direct
candidate. Third, an independent second model re-judges all premise-refuted
cases plus a 20% random sample.
The strictness matters. A first-pass lenient judge called 94% of questions addressed by accepting topical overlap; the per-candidate rubric brings it to 52.7% and restores variance to every downstream analysis.
Limitations — please read before using
- Labels are rater-relative. Second-judge agreement on
addressedis 63.5% (κ = 0.21). The companion protocol paper's seven-rater study found two independent human annotators agreed at only κ = 0.17 on an analogous taxonomy, while frontier models agreed with each other at κ = 0.60 — so certifying such a judge by model–model agreement overstates reliability roughly threefold. Absolute rates should never be quoted without the rater attached; comparisons under a fixed judge are the currency this data supports. not_addressedis a lower bound. Retrieval is abstract-level TF-IDF and can miss engagement, especially for narrow object-level questions.- Parametric leakage is present in one source. See the direct-LLM note above. Source is a covariate in every analysis in the accompanying paper.
- Rare outcomes are rare. 8 answered and 4 premise-refuted in total; the five-way status taxonomy is underpowered at this n.
- One domain. Astronomy only. Cross-subfield transfer is demonstrated; cross-science generality is not.
Loading
from datasets import load_dataset
ds = load_dataset("huiluckylucky/scientific-question-outcomes")
structure = load_dataset("huiluckylucky/scientific-question-outcomes", "structure")
Papers and code
- Question discovery framework — arXiv:2608.09968
- Backtesting protocol and benchmark — arXiv:2608.16795
- This dataset and its predictor analysis — paper pending; pipeline, judge rationales, and all results at github.com/nonameisready/scientific-question-outcome-prediction-indicators
Citation
@misc{mao2026questionoutcomes,
author = {Hui Mao},
title = {Scientific Question Outcomes: 980 Research Questions with
Five-Year Historical Outcome Labels},
year = {2026},
url = {https://huggingface.co/datasets/huiluckylucky/scientific-question-outcomes}
}
License: Apache-2.0.
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