Identifier stringlengths 37 82 | Paragraph stringlengths 1.95k 9.23k | Citation Text list | Functions Text list | Functions Label list | Citation Start End list | Functions Start End list |
|---|---|---|---|---|---|---|
2017AandA...599A..13Y__Bučík_et_al._(2009)_Instance_1 | Figure 2 shows solar wind plasma and magnetic field measurements for a CIR that occurred between July 26 and 27, 2003 (days of year 207–208). Following Chotoo et al. (2000), Richardson et al. (1993), we marked four regions in the plot: the slow wind region (S), the compressed slow wind region (S′), the compressed fast ... | [
"Bučík et al. (2009)"
] | [
"found that CIR boundaries can be well defined when the total pressure exceeds 50 pPa (indicated by the horizontal dashed line in Fig. 2), which is slightly higher than that in the background solar wind, which typically is 20−30 pPa, according to Jian et al. (2006)."
] | [
"Uses"
] | [
[
866,
885
]
] | [
[
886,
1151
]
] |
2021MNRAS.506.5468Z__Begeman,_Broeils_&_Sanders_1991_Instance_1 | Since the free-fall time-scale tff depends on the gravity law, we study how changing the gravity law affects the value of n in the KS law. Our main aim in this paper is to derive for the first time the KS law from a basic description in the framework of Milgromian dynamics (MOND; Milgrom 1983; Famaey & McGaugh 2012). M... | [
"Begeman, Broeils & Sanders 1991"
] | [
"Within the classical MOND framework, the Newtonian gravitational acceleration gN is replaced in the spherically symmetric case by $g=\\sqrt{g_{\\rm {N}} a_0}$ when the gravitational acceleration is far smaller than the critical acceleration a0 = 1.2 × 10−10 m s−2"
] | [
"Background"
] | [
[
925,
956
]
] | [
[
662,
923
]
] |
2020AandA...644A.108V__Birrer_&_Amara_2018_Instance_1 | The most commonly used technique to create a mock lens system from simulated galaxies is to extract a mass map from a particle-based simulation and use it to calculate lensing quantities (i.e. lensing potential and its first and second derivatives) needed to emulate the gravitationally lensed images. For this purpose, ... | [
"Birrer & Amara 2018"
] | [
"Different types of software, such as lenstronomy",
"can handle the inference of lensing quantities from mass maps using fast Fourier transform convolution."
] | [
"Background",
"Background"
] | [
[
624,
643
]
] | [
[
574,
622
],
[
747,
850
]
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2021AandA...648A.120R__Shimajiri_et_al._2014_Instance_1 | We derived the mean values of the 13CO/C18O abundance ratio for the three star-forming regions, obtaining values of 13CO/C18O = 10.9 ± 7.5 for Taurus, 13CO/C18O = 17.3 ± 11.5 for Perseus, and 13CO/C18O = 23.7 ± 10.4 for Orion. The expected value is 13CO/C18O = 7.5−9.8, assuming 12C/13C = 57−67 and 16O/18O = 500−600 (Ge... | [
"Shimajiri et al. 2014"
] | [
"As mentioned in Sect. 5.7, the 13CO/C18O abundance ratio increases in regions of enhanced UV field"
] | [
"Uses"
] | [
[
481,
502
]
] | [
[
381,
479
]
] |
2021AandA...653A.111R__Jones_et_al._(2021)_Instance_2 | As done by Le Fèvre et al. (2020), we visually inspect the ancillary data, the intensity maps, the velocity and velocity dispersion fields presented in Sect. 3.1 to search for the presence of multiple components or disturbed morphology near the position of the targets. The channel maps, the spectra and the PVDs are che... | [
"Jones et al. (2021)"
] | [
"This category is similar to the ‘uncertain’ (UNC) class introduced in",
"that, based on the results of the 3DBarolo fits, contains sources they are unable to classify because of the low S/N and/or spectral resolution, or contrasting evidence in their classification criteria."
] | [
"Similarities",
"Similarities"
] | [
[
1590,
1609
]
] | [
[
1520,
1589
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[
1610,
1812
]
] |
2020MNRAS.499.4394M__Bate_et_al._2014_Instance_1 | For these four remaining FHSC candidates (L1451-mm, MC35-mm, SM1N, and Oph A-N6) that have been observed at intermediate scales (few 100 au to few 1000 au) a final confirmation of their true evolutionary state requires higher resolution observations. For L1451-mm, the compact outflow needs to be resolved to investigate... | [
"Bate et al. 2014"
] | [
"An additional goal of high-resolution observations for L1451-mm and the remaining youngest candidates should be to investigate the temperature and density profiles of the envelope at scales from few au to 100 au. This is because simulations show that the temperature remains lower than ∼30 K even at several tens of... | [
"Future Work"
] | [
[
882,
898
]
] | [
[
533,
880
]
] |
2015MNRAS.451.4290S__Torrey_et_al._2014_Instance_1 | Hydrodynamical simulations of evolving galaxies allow us to calibrate these diagnostics by measuring their observability given a set of formation scenarios and physical processes (e.g. Jonsson et al. 2006; Rocha et al. 2007; Lotz et al. 2008a; Bush et al. 2010; Narayanan et al. 2010; Hayward et al. 2013; Snyder et al. ... | [
"Torrey et al. 2014"
] | [
"The quality and breadth of these experiments are limited by the availability of computational resources and the fidelity of models for galaxy physics such as",
"It has only recently become widespread to model the formation of galaxies ab initio",
"and the realism continues to improve"
] | [
"Motivation",
"Motivation",
"Motivation"
] | [
[
868,
886
]
] | [
[
345,
502
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[
566,
649
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[
788,
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]
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2021MNRAS.508.2583Z___2016_Instance_1 | Located in the star-forming region ρ-Ophiuchi, inside the dark cloud L1689N and at a distance of 141 pc (Dzib et al. 2018), IRAS16293−2422 is a well-studied Young Stellar Object (YSO) classified as a Class 0 source with less than 104 yr (Andre, Ward-Thompson & Barsony 1993), and represents one of the very early stages ... | [
"Jørgensen et al.",
"2016"
] | [
"It was the first source identified as a hot corino",
"based on the detection of Complex Organic Molecules (COMs) in the source, which was later supported by follow-up studies"
] | [
"Background",
"Background"
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[
639,
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[
662,
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[
348,
398
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[
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565
]
] |
2021AandA...647A.140C__Gianninas_et_al._2016_Instance_2 | In recent years, numerous low-mass and ELM WDs have been detected in the context of relevant surveys, such as the SDSS, ELM, SPY and WASP (see, e.g., Koester et al. 2009; Brown et al. 2010, 2016, 2020; Kilic et al. 2011, 2012; Gianninas et al. 2015; Kosakowski et al. 2020). The discovery of their probable precursors, n... | [
"Gianninas et al. 2016"
] | [
"In the case of pre-ELMVs,",
"and nonradial p- and g-mode pulsations",
"revealed that the excitation is probably due to the κ − γ mechanism, acting mainly in the zone of the second partial ionization of He, with a weaker contribution from the region of the first partial ionization of He and the partial ionizati... | [
"Background",
"Background",
"Background"
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[
1988,
2009
]
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[
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[
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1965
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[
2033,
2281
]
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2018MNRAS.477.3520L__Abolfathi_et_al._2018_Instance_1 | Over time, the data releases have treated the Balmer line regions in different ways. The presence of the artificial curvature was first reported by Busca et al. (2013) in the context of the DR9 data release. To minimize this effect, a different scheme was used in DR12 (Alam et al. 2015, see their table 2) by using a li... | [
"Abolfathi et al. 2018"
] | [
"Surprisingly, we observe that this data reduction change was only applied to the Balmer β, γ, and δ lines but not applied to the Balmer α line. For the latter one, the original iterative spline interpolation scheme has been used all along. As a result, an absorption-like feature at the location of Balmer α is foun... | [
"Compare/Contrast"
] | [
[
813,
834
]
] | [
[
428,
811
]
] |
2018ApJ...869..121M__Manfroid_et_al._2009_Instance_1 | An example of a low [14N/15N] value is potentially interesting for understanding the origins of material in our own solar system. The observed value in N2 of ∼200 is lower than values measured for both atmospheres of Earth and Venus (∼270; Junk & Svec 1958; Hoffman et al. 1979) and inferred for the protosolar nebula (∼... | [
"Manfroid et al. 2009"
] | [
"It is more similar to the extremely low values of [14N/15N] found in primitive solar system material, like cometary CN and HCN"
] | [
"Similarities"
] | [
[
588,
608
]
] | [
[
404,
530
]
] |
2020AandA...639A..88C__Chatzistergos_et_al._2019b_Instance_1 | To overcome these limitations, in our previous paper (Chatzistergos et al. 2018b, Paper I, hereafter) we introduced a novel approach to process the historical and modern Ca II K observations, to perform their photometric calibration, to compensate for the intensity centre-to-limb variation (CLV, hereafter), and to acco... | [
"Chatzistergos et al. 2019b"
] | [
"More importantly, we showed that, as long as the archives are consistent with each other, for example, they are centred at the same wavelength and employing the same bandwidth for the observations, the method can be used to derive accurate information on the evolution of plage areas without the need of any adjustm... | [
"Background",
"Background"
] | [
[
907,
933
]
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[
544,
905
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[
935,
956
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] |
2022ApJ...931...70B__Gabrielse_et_al._2012_Instance_1 | RFs can propagate from the magnetotail to Earth over a long distance more than 10 R
E together with BBFs behind them (Runov et al. 2009; Cao et al. 2010). Studies have suggested that RFs are crucial regions for particle acceleration, pitch-angle evolution, wave–particle interactions, and electromagnetic energy conversi... | [
"Gabrielse et al. 2012"
] | [
"The energetic plasma in the vicinity of RFs plays a key role in connecting the magnetotail with the inner magnetosphere because they carry a large amount of energy and can be injected into the inner magnetosphere to affect the ring current and radiation belt"
] | [
"Motivation"
] | [
[
1364,
1385
]
] | [
[
1104,
1362
]
] |
2022MNRAS.511.1714T__Peñarrubia_et_al._2005_Instance_1 | While these similar characteristics suggest that the OA and C could have a relationship, the nature of this relationship is not clear. Kawata, Thom & Gibson (2003) used numerical simulations to investigate whether Complex C could have been produced by the passage of a satellite galaxy through the Milky Way disc, and wh... | [
"Peñarrubia et al. 2005"
] | [
"The most well-known stellar stream in this region is the Monoceros Ring (e.g."
] | [
"Background"
] | [
[
946,
968
]
] | [
[
847,
924
]
] |
2021MNRAS.506.1045M__Marshall_et_al._2013_Instance_1 | Discovered in 1977 from its bright H α emission (Stephenson & Sanduleak 1977), SS433’s defining characteristics are undoubtedly the helical motion of highly collimated jets of plasma launched from its innermost regions, and mass-loaded, non-polar outflows (Fabian & Rees 1979; Margon et al. 1979) which together inflate ... | [
"Marshall et al. 2013"
] | [
"while the baryon content is revealed by emission lines ranging from H and He lines in the optical through to highly ionized Fe lines in the X-rays"
] | [
"Background"
] | [
[
716,
736
]
] | [
[
548,
694
]
] |
2020MNRAS.498..385J__Chomiuk_&_Povich_2011_Instance_1 | In Fig. 9, we show the total galactic star formation rate as a function of simulation time t for each isolated disc galaxy. Following the initial vertical collapse of the disc and the subsequent star formation ‘burst’ from t ∼ 30 Myr to t ∼ 250 Myr, the SFR settles down to a rate of ∼2–4 M⊙ yr−1. We make absolutely sur... | [
"Chomiuk & Povich 2011"
] | [
"These values are consistent with the current observed SFR in the Milky Way"
] | [
"Similarities"
] | [
[
708,
729
]
] | [
[
583,
657
]
] |
2022ApJ...928..167Z__Krüger_&_Foucart_2020_Instance_1 | Compared with BNS mergers, which would definitely eject a certain amount of materials to produce EM signals, some NSBH binaries may not tidally disrupt the NS component and, hence, would not make bright EM counterparts such as sGRBs and kilonovae.
9
9
During the final merger phase for plunging NSBH binaries, some wea... | [
"Krüger & Foucart 2020"
] | [
"The tidal disruption probability of NSBH mergers and the brightness of NSBH EM signals are determined by the BH mass, BH spin, NS mass, and NS equation of state (EoS; e.g."
] | [
"Uses"
] | [
[
837,
858
]
] | [
[
498,
669
]
] |
2019ApJ...877...33Z__Dunn_et_al._2010_Instance_1 | To investigate the emission-line properties in the blue system, we employed the photoionization code Cloudy (Version 17.01, Ferland et al. 2017) and applied the measured emission-line ratios to these models to simulate the possible physical conditions and processes in the medium. The simple model is a slab-shaped gas w... | [
"Dunn et al. 2010"
] | [
"This UV-soft SED is regarded as more realistic for radio-quiet quasars than the other available SEDs provided by Cloudy (see the detailed discussion in Section 4.2 of"
] | [
"Uses"
] | [
[
1376,
1392
]
] | [
[
1209,
1375
]
] |
2021MNRAS.500.3438O__Vidotto_et_al._2014b_Instance_1 | In addition to the wind models of λ And, we also present here the first full surface magnetic field observations of this star, finding a strong magnetic field for such an evolved star. These observations, carried out with the NARVAL spectropolarimeter, allow us to constrain the surface magnetic field of λ And. These de... | [
"Vidotto et al. 2014b"
] | [
"Usually, we see a decay in magnetic field strength as solar-type stars evolve, as their activity decreases along with their rotation",
"However, this subgiant star seems to have a relatively strong large-scale magnetic field compared to the Sun. The exact process through which this star would reach this stage in... | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
593,
613
]
] | [
[
443,
575
],
[
635,
869
]
] |
2022MNRAS.509.3599T__Matteo,_Springel_&_Hernquist_2005_Instance_1 | The typical value of the mass outflow rate for sources accreting below or close to the Eddington limit is $\dot{M}_{\rm out} \gtrsim 5\!-\!10{{\ \rm per\ cent}} \,\dot{M}_{\rm acc}$, for both UFOs and non-UFOs (Tombesi et al. 2012). In this scenario, even for the UFOs with the lowest allowed velocity, the mechanical po... | [
"Di Matteo, Springel & Hernquist 2005"
] | [
"Theoretical works",
"showed that, in order to have a significant feedback impact in the environment surrounding an AGN, it is required a minimum ratio between the mechanical power of the outflow and the bolometric luminosity of ${\\sim}0.5{{\\ \\rm per\\ cent}}$.",
"Instead, the lower limits are below the mini... | [
"Uses",
"Uses",
"Uses"
] | [
[
815,
851
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[
796,
813
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[
914,
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[
2044,
2495
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2020ApJ...892...68N__Laurikainen_et_al._2004_Instance_1 | We also examine our
measurement of NGC 3504 in the context of the empirical compilations of
and
scaling relations (Kormendy & Ho 2013; McConnell et al. 2013; Scott et al. 2013; Saglia et al. 2016) in Figure 16. The stellar-bulge velocity dispersion of NGC 3504 is determined from Ho et al. (2009), w... | [
"Laurikainen et al. 2004"
] | [
"For a sanity check, we estimate the bulge mass of NGC 3504 using our H-band MGE model and adapting the effective radius of the bulge derived from the bulge-disk-bar decomposition model"
] | [
"Uses"
] | [
[
568,
591
]
] | [
[
382,
566
]
] |
2018ApJ...861...28S__Temmer_et_al._2011_Instance_1 | In addition, the graduated cylindrical shell (GCS) model, which was developed by Thernisien et al. (2006, 2009) and Thernisien (2011), is applied to obtain the three-dimensional parameters of these CMEs. Figure 5 shows the fitting results of these CMEs. Seen from these images, the GCS model can well represent the topol... | [
"Temmer et al. 2011"
] | [
"However, previous results show that fast CME would decelerate during their propagation in interplanetary space (e.g.,"
] | [
"Compare/Contrast"
] | [
[
921,
939
]
] | [
[
740,
857
]
] |
2018AandA...613A...3Q__Kelly_et_al._2017_Instance_1 | As a prototypical Seyfert 2 galaxy with starburst at a distance of 14.4 Mpc (1″ = 72 pc, Bland-Hawthorn et al. 1997), NGC 1068 was observed at radio (Greenhill et al. 1996), millimeter (Schinnerer et al. 2000), infrared (Jaffe et al. 2004), optical (Antonucci & Miller 1985), UV (Antonucci et al. 1994), and X-ray (Kinkh... | [
"Kelly et al. 2017"
] | [
"Moreover, several molecules were detected and resolved toward NGC 1068 with interferometers in the past few years"
] | [
"Background"
] | [
[
1309,
1326
]
] | [
[
1174,
1287
]
] |
2016MNRAS.461..666K__Joshi_et_al._2011_Instance_2 | C-statistic (e.g. Jang & Miller 1997) is the most commonly used and the one-way analysis of variance (ANOVA; de Diego 2010) the most powerful test for verifying the presence of variability in a DLC. However, we did not employ either of these tests because, de Diego (2010) has questioned the validity of the C-test by ar... | [
"Joshi et al. 2011"
] | [
"The Fκ-test is preferred when the magnitude difference between the object and comparison stars is large"
] | [
"Compare/Contrast"
] | [
[
1147,
1164
]
] | [
[
1042,
1145
]
] |
2019AandA...630A...2H__Kofman_et_al._(2015)_Instance_1 | Several laboratory experiments have been performed to determine the mechanical properties of possible building blocks of comets. In particular, Güttler et al. (2009), Schräpler et al. (2015), Lorek et al. (2016), and Katsuragi & Blum (2017) investigated how the compressibility of ice layers and different dust structure... | [
"Kofman et al. (2015)"
] | [
"derived values of 0.15–0.25",
"The corresponding range is depicted in Fig. 6 by the horizontal bar shaded in blue. As thevolume filling factor is known, the laboratory measurements can be used to determine the most likely material of the surface."
] | [
"Uses",
"Uses"
] | [
[
624,
644
]
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[
645,
672
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[
775,
990
]
] |
2020AandA...637A..44N__Kraus_(2018)_Instance_3 | Among the existing IACT systems, HESS has the largest FoV and hence provides the highest sensitivity for the diffuse γ-ray flux. Its electron spectrum analysis technique could be directly used to obtain a measurement of the diffuse Galactic γ-ray flux above energies of several TeV in the Galactic Ridge (|l| 30°, |b| ... | [
"Kraus (2018)"
] | [
"are at the levels of >4σ for the analysis of"
] | [
"Compare/Contrast"
] | [
[
1345,
1357
]
] | [
[
1300,
1344
]
] |
2020MNRAS.491..903W__Rosotti_et_al._2014_Instance_1 | The process of planet formation is strongly dependent on the stellar birth environment. The majority of stars exist in clusters or associations within their first few Myr of evolution (Lada & Lada 2003; Longmore et al. 2014; Krumholz, McKee & Bland-Hawthorn 2019), during which time they also host protoplanetary discs (... | [
"Rosotti et al. 2014"
] | [
"Multiple feedback mechanisms influence disc evolution. In sufficiently dense environments, star–disc encounters can truncate the disc and induce increased accretion rates"
] | [
"Background"
] | [
[
754,
773
]
] | [
[
378,
548
]
] |
2021AandA...647A.132K__Kouloumvakos_et_al._2015_Instance_1 | Studies of SEP events are important for different reasons. On one hand, solar eruptive events are well-observed processes of energetic-particle acceleration (Vainio & Afanasiev 2018), which can be studied in detail using a multi-messenger approach, complementing particle data with observations in different wavelengths ... | [
"Kouloumvakos et al. 2015"
] | [
"Accordingly, numerous studies were focused on peak fluxes of SEPs and corresponding acceleration and transport processes (e.g.,"
] | [
"Background"
] | [
[
766,
790
]
] | [
[
638,
765
]
] |
2015MNRAS.450.4364N__Wu_et_al._2004_Instance_1 | Low- and intermediate-mass stars are formed by the gravitational collapse of the parental giant molecular cloud (GMC), followed by the accretion process (Palla 1996). During the accretion phase, material is ejected as well via collimated bipolar jets. However, when a YSO reaches 8 M⊙, the radiative flux becomes so inte... | [
"Wu et al. 2004"
] | [
"A process that constrains the outcoming radiation field to narrower angles may leave some room for the accretion process to continue in some directions. This seems to be the case for the outflows driven by young stars from a very broad mass range, as previous reported by several authors"
] | [
"Compare/Contrast"
] | [
[
874,
888
]
] | [
[
498,
785
]
] |
2016AandA...589A..44G__within_2000_Instance_1 | W51e2 is the strongest and best-studied HC HII region in the W51 Main cluster, and it is believed to be powered by an O8-type young star (e.g., Shi et al. 2010a). A number of interferometric studies conducted with varying angular resolutions, at centimetre (cm) and (sub)millimetre (mm) bands, identified molecular and i... | [
"Zhang & Ho 1997"
] | [
"VLA observations of the NH3 inversion lines (1, 1) and (2, 2) seen in absorption (1\\hbox{$\\farcs$}.̋1 beamsize) revealed radial infall on scales larger than 5000 AU toward the W51e2 core"
] | [
"Background"
] | [
[
564,
579
]
] | [
[
376,
562
]
] |
2021ApJ...920..139M__in_2002_Instance_1 | Cepheus X-4 was discovered as a transient source using the X-ray telescope of the OSO-7 satellite during 1972 June–July (Ulmer et al. 1973). Ginga observed the source during the 1988 March outburst and detected a spin period of 66.25 s for its neutron star for the first time (Koyama et al. 1991). Spectroscopic studies ... | [
"McBride et al. 2007"
] | [
"The RXTE observed another outburst in 2002 and re-established its cyclotron resonance feature corresponding to a centroid energy at 30.7 ± 1.8 keV (as established earlier by Ginga), which did not show a significant dependence on X-ray luminosity, although the continuum became harder with increasing source luminosi... | [
"Compare/Contrast"
] | [
[
2379,
2398
]
] | [
[
2060,
2377
]
] |
2022MNRAS.512..439C__Lian_et_al._2021_Instance_2 | It is still unclear whether this incompatibility is evidence against the spatially flat ΛCDM model or is caused by unidentified systematic errors in one of the established cosmological probes or by evolution of the parameters themselves with the redshift (Dainotti et al. 2021b, 2022). Newer, alternate cosmological prob... | [
"Lian et al. 2021"
] | [
"QSO flux measurements that reach to z ∼ 7.5"
] | [
"Background"
] | [
[
1125,
1141
]
] | [
[
947,
990
]
] |
2021AandA...647A..35B__Laffon_et_al._(2010)_Instance_2 | When we now compare the photodesorption yields at 541 eV between fluences 5 × 1015 photon cm−2 and at 3 × 1017 photon cm−2 in Fig. 2, the CO2 photodesorption first increases from 2.6 × 10−2 molecule/photon to 7.3 × 10−2 molecule/photon. We also observed this phenomenon for CO photodesorption yield (the data are not sh... | [
"Laffon et al. (2010)"
] | [
"the absorbed doses used in our fixed energy experiments change from ~ 2 to ~ 15 MGy, whichis quite similar to the absorbed doses in"
] | [
"Similarities"
] | [
[
1611,
1631
]
] | [
[
1479,
1610
]
] |
2022MNRAS.515.5267B__Landau_&_Lifshitz_1959_Instance_1 | Recent studies have shown that one can use energy balance arguments that include the large-scale magnetic field, ${\mathrm{{\boldsymbol {\mathit {B}}}}_0}$, to derive scaling laws between the Alfvénic and kinetic fluid quantities (Federrath 2016; Beattie et al. 2020; Skalidis & Tassis 2021; S+2021). The dimensionless m... | [
"Landau & Lifshitz 1959"
] | [
"In the linear perturbation theory limit of the MHD equations, δB2 includes contributions from shear Alfvén, fast and slow magnetosonic compressive eigenmodes (e.g."
] | [
"Uses"
] | [
[
1178,
1200
]
] | [
[
1014,
1177
]
] |
2020AandA...641A.155V__Puglisi_et_al._2019_Instance_2 | The scenario presented above has been formulated in various flavors to individually explain several of the properties reported here. The main addition of this work, namely the excitation of CO in distant main-sequence and starburst galaxies, fits in the general picture that we sketched. The ensemble of properties and c... | [
"Puglisi et al. 2019"
] | [
"We do detect starburst-like behaviors in galaxies on the main sequence",
"likely linked to the existence of transitional objects",
"to limit the references to recent works based on submillimeter observations"
] | [
"Compare/Contrast",
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1086,
1105
]
] | [
[
869,
939
],
[
961,
1015
],
[
1120,
1195
]
] |
2018AandA...615A..61C__Gladders_et_al._2013_Instance_1 | To tackle this problem, one must study the recent star formation history (SFH) of galaxies. This information is embeddedin their spectral energy distribution (SED). However, recovering it through SED modeling is complex and subject to many uncertainties and degeneracies. Although an average SFH of galaxies can be deriv... | [
"Gladders et al. 2013"
] | [
"However, implementation of these models is complex and a large library is needed to model all galaxies properties. Instead, numerous studies have used simple analytical forms to model galaxies SFH (e.g.,"
] | [
"Background"
] | [
[
892,
912
]
] | [
[
625,
828
]
] |
2022ApJ...938...92B__Zikanov_&_Thess_1998_Instance_1 | Flows with
Rem≪1
and
N∼(1)
have the distinct property that the induced magnetic field is quickly diffused away, yet the Lorentz force is not negligible. This limit is referred to as the quasi-static approximation to MHD (which we call “QMHD” henceforth; Moffatt 1967; Sommeria & Moreau 1982; Davidson 1995; ... | [
"Zikanov & Thess 1998"
] | [
"This limit is referred to as the quasi-static approximation to MHD",
"although recent numerical studies on its turbulent properties and anisotropy have been done as well"
] | [
"Background",
"Background"
] | [
[
703,
723
]
] | [
[
166,
232
],
[
602,
701
]
] |
2016MNRAS.461.2328M__Smith_et_al._2005_Instance_1 | This work, which focuses on mass reconstruction from gravitational lensing, is only the first in a series, which will exploit our mesh-free numerical techniques. Two regimes are typically distinguished in lensing mass reconstruction. Strong lensing is usually confined to the inner-most core of the gravitational lens an... | [
"Smith et al. 2005"
] | [
"Reconstruction techniques are divided into two classes, although this distinction is by no means unique or even consistent in some cases. Parametric techniques (e.g.",
"assume a parametric form of the underlying mass density distribution for the lens and typically make the assumption that light traces mass in th... | [
"Background",
"Background"
] | [
[
846,
863
]
] | [
[
637,
802
],
[
1053,
1237
]
] |
2020ApJ...903L..12H__Zhong_et_al._2020_Instance_1 | Magnetic reconnection (MR) may occur in various space and astrophysical plasma environments, among which the planetary magnetopause boundaries separating the solar wind and magnetospheric origins of plasmas and magnetic field are some of the most likely sites for the occurrence of MR. Due to the easy access to the in s... | [
"Zhong et al. 2020"
] | [
"In particular, the Magnetospheric Multiscale (MMS) mission has contributed greatly to the kinetic physics of magnetopause reconnection"
] | [
"Background"
] | [
[
675,
692
]
] | [
[
498,
632
]
] |
2015MNRAS.450.3458C__Cichowolski_et_al._2001_Instance_7 | The kinetic energy stored in the CO shell can be estimated as $E_{\rm kin} = 0.5\, M_{\rm shell}\, V^2_{\rm exp}$, where Vexp is the expansion velocity of the shell and Mshell is the total (molecular, atomic, and ionized) shell mass. Adopting an expansion velocity equal to half the velocity interval where the structure... | [
"Cichowolski et al. 2001"
] | [
"see fig. 1 of"
] | [
"Background"
] | [
[
2785,
2808
]
] | [
[
2771,
2784
]
] |
2022MNRAS.509.1504M__Komissarov_2006_Instance_1 | Energy flows induced into magnetically dominated relativistic magnetospheres of compact objects are commonly modelled by numerical simulations in the force-free electrodynamics (FFE) limit. Fueled by the track record of observations in the era of multimessenger astrophysics, current targets for such simulations include... | [
"Komissarov 2006"
] | [
"With the remarkable progress in scientific computing, their rotating magnetosphere has captured designers of numerical methods that integrate FFE and magnetohydrodynamics (MHD) with ever-improving accuracy (e.g."
] | [
"Background"
] | [
[
1055,
1070
]
] | [
[
843,
1054
]
] |
2018MNRAS.480.1081K__Hunter_et_al._2008_Instance_1 | Work in recent years has shown that rotation is a key ingredient in shaping the evolution of massive stars with very low metallicities (Z SMC metallicity down to Population III stars; see Meynet & Maeder 2017, and references therein). Fast rotators (with initial vrot ≳300 km s−1) are expected to lead to chemically hom... | [
"Hunter et al. 2008"
] | [
"Presently, although we still know little about rotation velocities of massive stars and their variation with environment, observations seem to favor fast rotators at low Z (e.g."
] | [
"Background"
] | [
[
785,
803
]
] | [
[
585,
762
]
] |
2019MNRAS.488.1066C__Link_et_al._1992_Instance_1 | A pulsar rotates at an angular velocity Ω with inertial moment I and magnetic moment $\boldsymbol {\mathcal {M}}$. It is described by the canonical rotation-down equation in the magnetic dipole model:
(4)
\begin{eqnarray*}
\dot{\Omega } = - K \Omega ^3,
\end{eqnarray*}
where $K = \frac{\mu _0 | \boldsymbol{\mathcal... | [
"Link et al. 1992"
] | [
"The possible change of macroscopic magnetic moment of pulsars at the moment of a glitch occurring was discussed by Link and Epstein"
] | [
"Background"
] | [
[
655,
671
]
] | [
[
522,
653
]
] |
2016MNRAS.459.1422E__Ebrahimi_&_Bhattacharjee_2014_Instance_1 | We begin with our results from global DNS MHD simulations of the MRI in cylindrical (r, ϕ, z) geometry using the DEBS (Schnack et al. 1987; Ebrahimi et al. 2009) initial-value code to solve the non-linear, viscous and resistive MHD equations
(1)
\begin{eqnarray}
\frac{\mathrm{\partial} \boldsymbol A }{ \mathrm{\parti... | [
"Ebrahimi & Bhattacharjee 2014"
] | [
"We use the same normalization",
"where time, radius and velocity are normalized to the outer radius a, the resistive diffusion time τR = a2/μ0η, and the Alfvén velocity $V_{\\rm A} = B_0/\\sqrt{\\mu _0 \\rho _0}$, respectively."
] | [
"Uses",
"Uses"
] | [
[
1436,
1465
]
] | [
[
1362,
1391
],
[
1468,
1658
]
] |
2021MNRAS.500.1772N__Siegel_&_Ciolfi_2015_Instance_1 | While these early studies demonstrated the viability of neutron star mergers as a major r-process site, they identified only one ejection channel: ‘dynamical ejecta’ that are tidally flung out by gravitational torques. Since they are never substantially heated, these ejecta carry their original β −equilibrium electron ... | [
"Siegel & Ciolfi 2015"
] | [
"As of today, many more mass ejection channels have been discussed:",
"as MHD-driven winds"
] | [
"Background",
"Background"
] | [
[
1243,
1263
]
] | [
[
869,
935
],
[
1222,
1241
]
] |
2016AandA...586A..80O__Fornasier_et_al._2015_Instance_3 | Figure 1 shows that in the regions where activity was detected visually, i.e., Hapi, Seth, and Ma’at pits have lower (8–13%/100 nm) spectral slopes than the rest of the comet surface (13–22%/100 nm). In addition to those places, Seth alcoves, the wall of the large Anuket alcove, around the circular features, both clust... | [
"Fornasier et al. 2015"
] | [
"Unfortunately, the previous work does not cover all the phase angles of the images we investigated, but the spectral slope variation between 35–54° (Fig. 3 of",
"is small so that we can make this comparison. However, if we follow the linear trend of the phase reddening, for the image taken in 70.45° phase angle ... | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
2053,
2074
]
] | [
[
1893,
2051
],
[
2076,
2328
]
] |
2020MNRAS.492.3241V__Frebel_et_al._2006_Instance_1 | Progress in this field will require large statistical samples of metal-poor stars in a variety of environments within the Local Group. Unfortunately, metal-poor stars are exceedingly rare and difficult to find, being overwhelmed by the more numerous metal-rich populations in the Galaxy. Examination of the Besançon mode... | [
"Frebel et al. 2006"
] | [
"Most of the known metal-poor stars have been found in dedicated surveys, such as objective prism surveys (the HK survey and Hamburg-ESO survey"
] | [
"Background"
] | [
[
967,
985
]
] | [
[
736,
878
]
] |
2018ApJ...860...88B__Paradijs_1978_Instance_1 | Thermonuclear (type-I) X-ray bursts are intermittently observed from many neutron star low-mass X-ray binaries (LMXBs; Strohmayer & Bildsten (2006) and references therein). Such a burst originates from an unstable thermonuclear burning of the accreted matter accumulated on the neutron star surface (Joss 1977; Lamb & La... | [
"van Paradijs 1978"
] | [
"These motivated an effort to measure the neutron star radius using the burst continuum spectrum, where the normalization of the burst blackbody is expected to be proportional to the square of the stellar radius (e.g.,"
] | [
"Background"
] | [
[
1088,
1105
]
] | [
[
870,
1087
]
] |
2019AandA...632A.104G__Hirabayashi_et_al._2016_Instance_1 | Finally, our observations are consistent with the bilobate shape of the nucleus of comet 8P/Tuttle. As noted in Sect. 1, this shape is likely common among comets because it was found for four out of the six comets for which we have spatially resolved images. This is also the case of the trans-Neptunian object 2014 MU69... | [
"Hirabayashi et al. 2016"
] | [
"A contact binary could result from",
"(ii) the disruption of a monolithic object due to excessive spin-up resulting from non-gravitational forces or YORP5 effect followed by a reaccretion"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
811,
834
]
] | [
[
490,
524
],
[
633,
782
]
] |
2018ApJ...867..120H__Takahashi_et_al._1990_Instance_1 | Although the magnetic (i.e., one-photon) pair production is also taken into account, most electron–positron pairs are found to be produced via photon–photon (i.e., two-photon) collisions, which take place via two paths. One path is through the collisions of two MeV photons, both of which were emitted from the equatoria... | [
"Takahashi et al. 1990"
] | [
"If the pairs are produced via TeV–eV collisions (i.e., via the second path) outside the gap outer boundary, they have outward ultrarelativistic momenta to easily “climb up the hill” of the potential k0",
"see also Figure 2 of HP16) and propagate to large distances without turning back."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
956,
977
]
] | [
[
753,
954
],
[
979,
1060
]
] |
2021AandA...655A..12T__Tang_et_al._2017b_Instance_3 | Using the RADEX3 non local thermodynamic equilibrium (LTE) modeling program (van der Tak et al. 2007) with collisional rate coefficients from Wiesenfeld & Faure (2013), we modeled the relation between the gas kinetic temperature and the measured average of para-H2CO 0.5 × [(322–221 + 321–220)/303–202] ratios, adopting ... | [
"Tang et al. 2017b"
] | [
"Considering that the relation between the gas temperature and the para-H2CO line ratio may vary at different spatial densities (see Fig. 2 in",
"we modeled it at spatial densities 104, 105, and 106 cm−3 in Fig. 5."
] | [
"Uses",
"Uses"
] | [
[
1097,
1114
]
] | [
[
955,
1096
],
[
1117,
1185
]
] |
2020MNRAS.492.5675C__Pérez-Montero_et_al._2019_Instance_2 | In regarding AGNs, the Te method tends to underestimate the oxygen abundance by an average value of about 0.6 dex in comparison to estimations based on strong-line methods and it produces subsolar O/H values for most of these objects (Dors et al. 2015; Dors, Freitas-Lemes & Âmores 2020). An alternative method to derive... | [
"Pérez-Montero et al. 2019"
] | [
"Moreover, the Te problem can also be originated due to the use of an unappropriate calculation of the ionization correction factor (ICF) for oxygen in AGNs"
] | [
"Compare/Contrast"
] | [
[
2078,
2103
]
] | [
[
1921,
2076
]
] |
2021MNRAS.500.3957E__Springel_&_Hernquist_2003_Instance_1 | The results presented in this paper are based on data from IllustrisTNG,1the next-generation suite of state-of-the-art magnetohydrodynamical cosmological simulations of galaxy formation (Marinacci et al. 2018; Naiman et al. 2018; Nelson et al. 2018; Pillepich et al. 2018b; Springel et al. 2018). Building on the success... | [
"Springel & Hernquist 2003"
] | [
"The models for galaxy formation include physical processes such as gas heating by a spatially uniform and time-dependent UV background, primordial and metal-line gas cooling, a subgrid model for star formation, and the unresolved structure of the interstellar medium"
] | [
"Uses"
] | [
[
915,
940
]
] | [
[
647,
913
]
] |
2017AandA...607A.126Y__Gunawardhana_et_al._2011_Instance_1 | Observed high mass end power-law index of the galaxy-wide IMF resulting from the calculated IGIMF, \hbox{$\alpha_3^{\mathrm{gal}}$}α3gal (i.e., αgal in Eq. (15) for m> 1 M⊙), for a constant SFR over δt = 10 Myr in dependence of the galaxy-wide SFR. In Fig. 5, \hbox{$\alpha_3^{\mathrm{gal}}$}α3gal values diverge for dif... | [
"Gunawardhana et al. 2011"
] | [
"The blue squares are data from the GAMA galaxy survey"
] | [
"Uses"
] | [
[
758,
782
]
] | [
[
703,
756
]
] |
2015AandA...576L..16P__Li_et_al._(2013)_Instance_1 | To constrain the size of outflows that we could have missed, we performed simple simulations. We placed artificial, unipolar secondary sources next to a primary point source model representing Sgr A* and compared the closure phases obtained from the resulting artificial visibility data with the observations. We conside... | [
"Li et al. (2013)"
] | [
"We probed four orientations for the simulated outflows",
"the jet direction claimed by"
] | [
"Uses",
"Uses"
] | [
[
598,
614
]
] | [
[
444,
498
],
[
569,
597
]
] |
2020MNRAS.491.5881Y__McConnell_et_al._2011_Instance_1 | There is good observational and theoretical evidence that supermassive black holes (SMBHs) exist in nearly every galaxy in universe. Understanding the properties of these SMBHs will clarify their roles in galaxy formation and evolution across the cosmology history (e.g. Kormendy & Ho 2013). There are mainly two paramet... | [
"McConnell et al. 2011"
] | [
"For a few very nearby (100 Mpc) quiescent galaxies, including our Galaxy, SMBH masses can be measured through the stellar or gaseous dynamics method (e.g."
] | [
"Background"
] | [
[
569,
590
]
] | [
[
392,
546
]
] |
2016ApJ...831...37K__Dadina_2008_Instance_1 | Based on previous works (Kawamuro et al. 2013; Tazaki et al. 2013), we start with a base-line model,
in the XSPEC terminology. This model includes absorbed primary X-ray emission (i.e., a cut-off power law), a scattered component, and a reflection continuum from distant cold matter accompanied by a narrow iron-Kα ... | [
"Dadina 2008"
] | [
"Because it is difficult to determine the cut-off energy from our data, we fix it at 300 keV, which is a typical value measured in nearby AGNs"
] | [
"Uses"
] | [
[
684,
695
]
] | [
[
541,
682
]
] |
2019ApJ...875...61M__Marco_2006_Instance_1 | A substantial fraction of metal-poor stars that have recently evolved off the MS, e.g., giants and planetary nebulae (PNe), have been influenced by binary interactions. The IMF is significantly weighted toward low-mass stars (Bastian et al. 2010; Kroupa et al. 2013), and the MW star formation rate was ≈3 times larger ≈... | [
"Moe & De Marco 2006"
] | [
"For example, the enhanced close binary fraction of metal-poor solar-type stars substantially strengthens the conclusion that the shaping of PN morphologies is the result of binary interactions"
] | [
"Similarities"
] | [
[
981,
1000
]
] | [
[
787,
979
]
] |
2020MNRAS.492.2510L__Galsgaard_et_al._2007_Instance_1 | We suggest that the jet–facula collision does not cause a change in the field-line connectivity and only leads to the redistribution of jet material. There are two main reasons supporting this viewpoint. The first is the 3D magnetic configuration at the collision region. The penumbra and facula are both located at nega... | [
"Galsgaard et al. 2007"
] | [
"When the magnetic field lines are parallel it is not easy to have reconnection"
] | [
"Uses"
] | [
[
535,
556
]
] | [
[
432,
510
]
] |
2022ApJ...933..243F__Woosley_&_Bloom_2006b_Instance_2 | Gamma-ray bursts (GRBs) are among the most powerful gamma-ray sources in the universe. They could be generated from the merger of binary compact objects (BCOs; Duncan & Thompson 1992; Usov 1992; Thompson 1994; Metzger et al. 2011) or the death of massive stars (Woosley 1993; Paczyński 1998; Woosley & Bloom 2006a). The ... | [
"Woosley & Bloom 2006b"
] | [
"Hereafter, we adopt natural units c = ℏ = 1. have been reported (see, e.g.,"
] | [
"Uses"
] | [
[
1357,
1378
]
] | [
[
1240,
1315
]
] |
2016ApJ...831..200W__Lorén-Aguilar_&_Bate_2015_Instance_1 | HD 97048 is yet another disk for which the dust emission at (sub-)mm wavelengths shows evidence of axisymmetric ring-like structures, here on spatial scales of around tens of au (Walsh et al. 2014; ALMA Partnership et al. 2015; Andrews et al. 2016; Nomura et al. 2016; Zhang et al. 2016). We predict that this substructu... | [
"Lorén-Aguilar & Bate 2015"
] | [
"There remains much debate in the literature on the origin of such axisymmetric substructure in protoplanetary disks including",
"and toroidal dust traps created by hydrodynamic or magnetohydrodynamic effects (see, e.g.,"
] | [
"Motivation",
"Motivation"
] | [
[
944,
969
]
] | [
[
426,
551
],
[
831,
921
]
] |
2022AandA...665L...1F__Peck_et_al._2001_Instance_1 | In our model, we compute the tidal response of the oceans and the solid-Earth to luni-solar semi-diurnal forcing, both combined with mimetic continental drift driven by plate tectonics. We focus on the dependence of dissipation on the Earth’s spin rate. We combine two analytical approaches that describe long-wavelength... | [
"Peck et al. 2001"
] | [
"The existence of an early ocean is supported by",
"and from records of the oxygen isotope composition of seawater"
] | [
"Background",
"Background"
] | [
[
836,
852
]
] | [
[
539,
586
],
[
772,
834
]
] |
2015AandA...574A..62S__Burkepile_et_al._(2004)_Instance_1 | Quiescent prominences are objects formed by relatively cool plasma in the hot corona. Their cool material occurs mostly in the dipped magnetic field lines. In quiescent prominences, which can persist from several hours to several days, magnetic dips form quasi-vertical structures called threads. Quiescent prominences a... | [
"Burkepile et al. (2004)"
] | [
"However,",
"also saw highly structured material most probably originating from a prominence in 63% of CMEs associated with eruptive prominences at the limb observed in visible light using the broadband filter (λλ 5000−5350 Å).",
"Although such observations are called as white light in literature, it would be b... | [
"Background",
"Background",
"Compare/Contrast"
] | [
[
1035,
1058
]
] | [
[
1026,
1034
],
[
1059,
1273
],
[
1274,
1644
]
] |
2016MNRAS.463..696L__Randich_et_al._2006_Instance_1 | Another possible explanation for the peculiar solar composition is that some of the dust in the pre-solar nebula was radiatively cleansed by luminous hot stars in the solar neighbourhood before the formation of the Sun and its planets. This dust-cleansing scenario is supported by the finding that the open cluster M67 s... | [
"Randich et al. 2006"
] | [
"This cluster has about solar metallicity ([Fe/H] in the range −0.04 to +0.03, e.g."
] | [
"Motivation"
] | [
[
1029,
1048
]
] | [
[
883,
965
]
] |
2016MNRAS.455..449H__Oman_et_al._2015_Instance_1 | With only six free parameters, the standard Λ cold dark matter (ΛCDM) cosmological model fits no less than 2500 multipoles in the cosmic microwave background (CMB) angular power spectrum (Planck Collaboration XVI 2014), the Hubble diagram of Type Ia supernovae, the large-scale structure matter power spectrum, and even ... | [
"Oman et al. 2015"
] | [
"Nevertheless, it still faces numerous challenges on galaxy scales. Among these, the most important ones are",
"or the unexpected diversity of rotation curve shapes at a given mass scale"
] | [
"Background",
"Background"
] | [
[
996,
1012
]
] | [
[
526,
633
],
[
920,
994
]
] |
2018ApJ...864...49P__Tacconi_et_al._2013_Instance_1 | Figure 9 summarizes our constraints on the molecular gas mass fraction in the analyzed samples of galaxies. In order to convert CO luminosity to molecular gas mass, we consider two different assumptions for αCO. First, we assume a constant value of αCO = 3.6 M⊙ (K km s−1 pc2)−1 adopted by some previous studies (e.g., D... | [
"Tacconi et al. 2013"
] | [
"While the PHIBSS project estimated molecular gas masses by measuring the CO(3–2) line emission",
"Scoville et al. (2016, 2017) used the flux on the Rayleigh–Jeans tail of the dust continuum emission to estimate the total gas masses."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
879,
898
]
] | [
[
783,
877
],
[
921,
1055
]
] |
2021ApJ...910...86R__Stark_et_al._2017_Instance_1 | One of the major endeavors of modern observational cosmology is to paint a coherent picture of the history of the universe. To this end, the final frontier remains the identification and characterization of the first sources that appeared in the universe, those which played a significant role in reionizing the intergal... | [
"Stark et al. 2017"
] | [
"Complementing these observations, the spectroscopic confirmation",
"of over a dozen sources has seen impressive advances with ground-based spectroscopy (e.g., probing the rest-frame UV and FIR with Keck/MOSFIRE, VLT/X-Shooter, and ALMA), particularly for the brightest and rarest objects."
] | [
"Background",
"Background"
] | [
[
1131,
1148
]
] | [
[
948,
1012
],
[
1264,
1484
]
] |
2018MNRAS.481.3573L__Robotham_et_al._2017_Instance_1 | Another important test for galaxy formation models, is whether they place the right amount of stellar mass into discs and bulges. Moffett et al. (2016) measured the SMF separating galaxies into different morphological types and also into discs/bulges. With this, they derived the fractional contribution from bulges/disc... | [
"Robotham et al. 2017"
] | [
"This is quite a difficult measurement to do in observations as light profile fitting is required, which can be robustly done in very disc- and bulge-dominated galaxies, but when both components contribute similarly, the measurement is less robust"
] | [
"Motivation"
] | [
[
621,
641
]
] | [
[
373,
619
]
] |
2019MNRAS.490.2071Y__Riess_et_al._2018_Instance_1 |
Set II: we now focus on the observational constraints on the model parameters after the inclusion of the local measurement of H0 by Riess et al. (2018) with the previous data sets (CMB, Pantheon, and CC) in order to see how the parameters could be improved with the inclusion of this data point. Since for this present ... | [
"Riess et al. (2018)"
] | [
"Set II: we now focus on the observational constraints on the model parameters after the inclusion of the local measurement of H0 by",
"with the previous data sets (CMB, Pantheon, and CC) in order to see how the parameters could be improved with the inclusion of this data point."
] | [
"Uses",
"Uses"
] | [
[
133,
152
]
] | [
[
1,
132
],
[
153,
296
]
] |
2021ApJ...907...47L__Lee_et_al._2019_Instance_1 | In Figure 8, we also find small differences in the [Na, Al, O/Fe] abundance ratios between the stars in the bright and faint RC groups, although it is not as clear as in the case of [Na, Al, O/H] abundances. In particular, unlike Figure 7, stars in the bRC group are more enhanced in [Na/Fe] but appear to be more deplet... | [
"Lee et al. 2019"
] | [
"When the relative fraction of RC stars is taken into account (27%; see Section 4), the difference in [Na/Fe] between the genuine RC stars would correspond to Δ[Na/Fe] ∼ 0.20 dex, which is comparable to that expected from our chemical evolution model for the bulge stars (Δ[Na/Fe] = 0.2 ∼ 0.3 dex;"
] | [
"Similarities"
] | [
[
889,
904
]
] | [
[
576,
872
]
] |
2018AandA...616A..11G__Westerhout_1957_Instance_1 | Gaia DR2 contains unprecedented information about the Galaxy, which should allow us to infer its current structure, its equilibrium state, its evolution, modes of mass growth over time, dark matter distribution (and perhaps nature), to cite a few of the questions of modern Galactic astrophysics. As an example, it has b... | [
"Westerhout 1957"
] | [
"As an example, it has been known for several decades that the Galactic disc contains large-scale non-axisymmetric features, including",
"a warp"
] | [
"Background",
"Background"
] | [
[
822,
837
]
] | [
[
297,
430
],
[
791,
797
]
] |
2020ApJ...891...59R__Feruglio_et_al._2015_Instance_1 | In order to understand the origin of the termination of the powerful jet in Mrk 231, consider the very low accretion rates in these FRI NLRGs, three to four orders of magnitude less than a quasar (Chiaberge et al. 1999, 2002; Hardcastle et al. 2009). However, there are the occasional FRI broad-line galaxies such as the... | [
"Feruglio et al. 2015"
] | [
"In low radio states, it has also displayed evidence of a high-ionization X-ray-absorbing wind"
] | [
"Background"
] | [
[
780,
800
]
] | [
[
685,
778
]
] |
2021AandA...647A..35B__Laffon_et_al._(2010)_Instance_1 | When we now compare the photodesorption yields at 541 eV between fluences 5 × 1015 photon cm−2 and at 3 × 1017 photon cm−2 in Fig. 2, the CO2 photodesorption first increases from 2.6 × 10−2 molecule/photon to 7.3 × 10−2 molecule/photon. We also observed this phenomenon for CO photodesorption yield (the data are not sh... | [
"Laffon et al. (2010)"
] | [
"estimated with NEXAFS spectroscopy (at the C K-edge) that X-ray irradiation at 150 eV of pure methanol ice at 20 K leads to a survival rate of 50% for methanol after an absorbed dose of 1.1 MGy."
] | [
"Uses"
] | [
[
865,
885
]
] | [
[
886,
1080
]
] |
2016MNRAS.461.1745E__Goerdt_et_al._2010_Instance_1 | Given that the CDM paradigm only begins to face significant problems at precisely such scales when complex baryonic physics begins to play an important role, it is natural to inquire whether it is the central culprit behind erroneous theoretical predictions. It was for example realized early on that energy from superno... | [
"Goerdt et al. 2010"
] | [
"However, the complexity of such simulations obscures the physical mechanisms through which these processes affect the dark matter distribution. These mechanisms normally invoke ‘heating’ of the cold central density cusp through an irreversible process, such as dynamical friction from infalling clumps"
] | [
"Background"
] | [
[
1245,
1263
]
] | [
[
833,
1134
]
] |
2019ApJ...876L..28D__Lamb_et_al._2018_Instance_2 | In Figures 1 and 2 we show that the X-ray (1.7 keV5
5
This value corresponds to the geometric mean of the XRT energy band, at which the error of the estimated flux can be reasonably suppressed.
), optical (R-band), and radio (6 GHz) fluxes varied with the time of observation applied to the proper corrections if observ... | [
"Lamb et al. 2018"
] | [
"In the jet model, such a p can also reasonably account for the very late flux decline of"
] | [
"Uses"
] | [
[
1312,
1328
]
] | [
[
1215,
1303
]
] |
2017MNRAS.464.3385W__Tsiganis_et_al._2005_Instance_1 | Oort Cloud. The conclusions that can be reached from this figure about the formation of the Oort Cloud are well known. For example, T93 showed that the parameter space in which an Oort Cloud forms is quite restricted, and that those Oort Clouds that do form have a narrow range of semimajor axes ∼10 000 au. While this p... | [
"Tsiganis et al. 2005"
] | [
"While this parameter space is inhabited by Uranus and Neptune in the Solar system, which should thus readily supply objects to the Oort Cloud (even accounting for the possibility that these planets may have started closer to the Sun;",
"it could be that Oort Clouds are relatively rare."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
542,
562
]
] | [
[
308,
541
],
[
565,
614
]
] |
2022ApJ...926..206Z__Schwab_et_al._2016_Instance_1 | The first possible scenario is that all FRBs are generated from magnetars, the population of non-repeating FRBs are from magnetars born in the delay formation channels (Margalit et al. 2019) such as neutron star−neutron star mergers associated with short gamma-ray bursts (Rosswog et al. 2003; Price & Rosswog 2006; Giac... | [
"Schwab et al. 2016"
] | [
"The first possible scenario is that all FRBs are generated from magnetars, the population of non-repeating FRBs are from magnetars born in the delay formation channels",
"or white dwarf−white dwarf mergers"
] | [
"Background",
"Background"
] | [
[
527,
545
]
] | [
[
0,
167
],
[
474,
508
]
] |
2018AandA...613A..35K__Leloudas_et_al._2011_Instance_1 | As shown in Fig. 3, the differences in metallicity between different SN subclasses are not significant. This is in contradiction with what is expected from single-star evolution theory, where metallicity-driven winds are crucial: type Ic SNe, which are the most highly stripped, would show the highest metallicity, follo... | [
"Leloudas et al. 2011"
] | [
"This result strengthens the notion that metallicity may not play an important role in deciding theresulting SN type, in agreement with other works based on SN environments"
] | [
"Similarities"
] | [
[
745,
765
]
] | [
[
544,
715
]
] |
2022MNRAS.517.5744G__Caro_et_al._2016_Instance_3 | The CO photodesorption yield reaches its highest value when this ice is deposited at low temperatures (down to 7 K, the lowest temperature studied experimentally) and decreases gradually at higher deposition temperatures (Öberg et al. 2007; Öberg et al. 2009; Muñoz Caro et al. 2010, 2016; Sie et al. 2022). The explanat... | [
"Muñoz Caro et al. 2016"
] | [
"Absorption band shifts of CO ice in the UV and IR ranges only occurred at deposition temperatures above 20 K",
"suggesting that CO ice grown at lower temperatures is amorphous below 20 K in our experiments, and therefore, the decreasing photodesorption yield is not related to a transition from amorphous to cryst... | [
"Background",
"Compare/Contrast"
] | [
[
912,
934
]
] | [
[
783,
891
],
[
937,
1286
]
] |
2022AandA...658A..35K__Boquien_et_al._2019_Instance_1 | It is important in our analysis to only keep sources for which the SFR and stellar mass estimates are reliable. To this end, we first excluded sources whose fit had reduced χ2,
χ
red
2
>5
$ \chi ^2_{\rm red}>5 $
. This criterion is based on visual inspection of the SED fits and has been adopted in previous s... | [
"Boquien et al. 2019"
] | [
"One is evaluated from the best-fit model, and one weights all models allowed by the parametric grid, with the best-fit model having the heaviest weight"
] | [
"Uses"
] | [
[
1030,
1049
]
] | [
[
877,
1028
]
] |
2015AandA...584A.103S__Baym_et_al._1971b_Instance_1 | Also plotted in Fig. 2 is the pressure in the outer crust from some popular EoSs that model the complete structure of the NS. The figure is drawn up to nb = 3 × 10-4 fm-3, thus comprising the change from the outer crust to the inner crust in order to allow comparison of the EoSs also in this region (notice, however, ... | [
"Baym et al. 1971b"
] | [
"In the seminal work of BPS",
"the nuclear masses for the outer crust were provided by an early semi-empirical mass table.",
"The corresponding EoS is seen to display a similar pattern with the BCPM, FRDM, and BSk21 results in Fig. 2."
] | [
"Background",
"Background",
"Similarities"
] | [
[
1073,
1090
]
] | [
[
1045,
1071
],
[
1092,
1183
],
[
1184,
1292
]
] |
2019ApJ...881...38E__Pinto_et_al._2016_Instance_1 | We fitted the XMM-Newton spectra of ULX-1 and ULX-2 from observation 0794581201 with an absorbed power-law model, using two tbabs absorption components, one frozen to the Galactic value of NH = 1.84 × 1021 cm−2 and the other allowed to vary. In the case of ULX-1, a power-law model was not sufficient to produce a good f... | [
"Pinto et al. 2016"
] | [
"These soft residuals are known to be a common feature in the spectra of ULXs and bright X-ray binaries",
"and found in other ULXs to be a combination of emission and absorption features related to powerful outflowing winds (including in NGC 6946 ULX-3;"
] | [
"Similarities",
"Similarities"
] | [
[
729,
746
]
] | [
[
405,
507
],
[
582,
728
]
] |
2019MNRAS.487.5666S__Wolfe_et_al._1986_Instance_1 | The observations of the characteristic double-horned line profiles (Stewart et al. 2014) are all restricted to very low redshifts (z 0.5). Our understanding of the kinematics of H i at high redshifts (z > 0.5) majorly depends on the study of the QSO absorption spectra where the absorption features are mainly dominated... | [
"Wolfe et al. 1986"
] | [
"Modelling of DLAs observations suggests that DLAs resemble rotating disc galaxies with circular velocities typically of the order of $100\\!-\\!200\\, {\\rm km\\, s}^{-1}$"
] | [
"Background"
] | [
[
681,
698
]
] | [
[
513,
679
]
] |
2020AandA...639A..46B__Štverák_et_al._(2009)_Instance_2 | The linear relationship that we observe between breakpoint energy and core temperature is in line with previous measurements (e.g. McComas et al. 1992; Štverák et al. 2009), for both the halo and strahl. According to Scudder & Olbert (1979), a linear trend in the halo relation also follows under the assumption that bin... | [
"Štverák et al. (2009)"
] | [
"Findings by",
", on the other hand, show that the (nh + ns)/nc ratio remains roughly constant with heliocentric distance in the slow wind, suggesting a lack of interchange between the thermal and suprathermal populations."
] | [
"Differences",
"Differences"
] | [
[
783,
804
]
] | [
[
771,
782
],
[
804,
1010
]
] |
2017ApJ...834..178Y__Tachihara_et_al._2007_Instance_2 | In order to investigate the gas kinematics at an early evolutionary stage and the formation of Keplerian disks, we conduct ALMA observations toward three candidate young protostars, Lupus 3 MMS, IRAS 15398−3559, and IRAS 16253−2429. They are selected from our SMA sample (Yen et al. 2015a). These three protostars all ha... | [
"Tachihara et al. 2007"
] | [
"These three protostars are all embedded in dense cores with masses ≳0.5 M⊙",
"Therefore, they are excellent targets by which to study the gas motions on a 100 au scale at an early evolutionary stage."
] | [
"Motivation",
"Motivation"
] | [
[
1930,
1951
]
] | [
[
1838,
1912
],
[
1973,
2094
]
] |
2017AandA...601A.130R__Hernández_et_al._2013_Instance_1 | Various strategies have been devised to identify modes. One can, for instance, search for frequency patterns appropriate for rapid rotation. The background for this search is the discovery of asymptotically uniform frequency spacings in the numerically computed spectra of uniformly rotating polytropic models (Lignières... | [
"García Hernández et al. 2013"
] | [
"In observed spectra, recurrent frequency spacings that may correspond to the large separation or half its value have been found in some stars"
] | [
"Background"
] | [
[
733,
761
]
] | [
[
560,
701
]
] |
2018MNRAS.473.3810Y__Mitrushchenkov_et_al._2017_Instance_2 | The lack of data on inelastic processes due to collisions with neutral hydrogen atoms has been a major limitation on modelling of F-, G- and K-star spectra in statistical equilibrium, and thus to reliably proceeding beyond the assumption of local thermodynamic equilibrium (LTE) in analysis of stellar spectra and the de... | [
"Mitrushchenkov et al. 2017"
] | [
"Comparisons of the two methods show quite good agreement and reasonable agreement with the full quantum calculations is found, particularly for the most important processes with the largest rates"
] | [
"Similarities"
] | [
[
1873,
1899
]
] | [
[
1619,
1814
]
] |
2018ApJ...863..162M__Liu_et_al._2013_Instance_2 | NLFFF extrapolation provides the reconstructed coronal magnetic field for AR 11158 from 2011 February 13 − 2011 February 15 (Figures 1(d)–(f)). The field lines (yellow lines) within the core of the AR have arcade-like structure with a relatively strong twist mainly near the PIL. These figures show that the magnetic fie... | [
"Liu et al. 2013"
] | [
"However, our result is consistent with other NLFFF results"
] | [
"Similarities"
] | [
[
1352,
1367
]
] | [
[
1257,
1315
]
] |
2015AandA...582A..42K__Cardelli_et_al._(1989)_Instance_1 | Spectral energy distributions in accordance with the physical parameters of the best-fit spectra were generated with FASTWIND, to provide the flux density per surface unit through our studied bands. The composite flux measured at Earth from a binary at a distance d, at a wavelength λ, reddened to extinction A(λ), is gi... | [
"Cardelli et al. (1989)"
] | [
"The composite SED was reddened according to the new family of optical and near-infrared extinction laws for O-type stars provided by Maíz Apellániz et al. (2014), which constitute an improvement of the widely used extinction laws by"
] | [
"Uses"
] | [
[
829,
851
]
] | [
[
596,
828
]
] |
2022AandA...661A.129S__Rodríguez-Almeida_et_al._2021_Instance_3 | Radio astronomy is recognized as one of the most effective techniques to search for interstellar molecules. By comparing the spectra of candidate molecules in the laboratory with the spectra observed in astronomical surveys, we can determine whether these molecules exist in interstellar space. Therefore, it is necessar... | [
"Rodríguez-Almeida et al. 2021"
] | [
"For instance, thioformic acid (HC(O)SH) was very recently detected in G+0.693–0.027. Its trans-isomer has an abundance of ~1 × 10–10"
] | [
"Background"
] | [
[
1516,
1545
]
] | [
[
1382,
1514
]
] |
2015MNRAS.454.1468K__Winckel_2003_Instance_2 | Owing to their dusty circumstellar environments, a large mid-infrared (mid-IR) excess is a characteristic feature of post-AGB stars and a detection of cold circumstellar material using mid-IR photometry can be used to identify these objects. The first extensive search for these objects was initiated in the mid-80's usi... | [
"Van Winckel 2003"
] | [
"Studies showed that the majority of the optically visible Galactic post-AGB stars could be classified based on their spectral energy distributions (SEDs) into two groups: shell-sources and disc-sources"
] | [
"Background"
] | [
[
922,
938
]
] | [
[
719,
920
]
] |
2019MNRAS.487...24G__Rogers_2015_Instance_2 | NASA’s Kepler mission has unveiled a wealth of new planetary systems (e.g. Borucki et al. 2010). These systems offer new insights into the process of planet formation and evolution. One of Kepler’s key findings is that the most common planets in our Galaxy, observed to date, are between 1 and 4 R⊕, i.e. larger than Ear... | [
"Rogers 2015"
] | [
"Studies suggest that this valley likely marks the transition from the smaller rocky planets: ‘super-Earths’, to planets with significant H/He envelopes typically containing a few per cent of the planet’s total mass: ‘sub-Neptunes’ (e.g."
] | [
"Background"
] | [
[
1574,
1585
]
] | [
[
1293,
1529
]
] |
2022ApJ...936..102A__Williams_et_al._2006_Instance_1 | Following the original BGK kinetic-theoretical scheme (Bernstein et al. 1957), we transform the above equations to the energy frame, defined as
5
w=12v2+ϕ.
In the energy frame, the ion distribution transforms into
6
fi(w)=Γ(κi)πκi−3/2Γ(κi−1/2)1+2wκi−3/2−κi,
where
7
f(x,v)dv=f(w)dw/2w−ϕ.
Here, the total ener... | [
"Williams et al. 2006"
] | [
"Spacecraft observations show that wave potential structures of Gaussian form are common in space and astrophysical plasmas",
"We assume this potential well to have Gaussian form"
] | [
"Uses",
"Uses"
] | [
[
997,
1017
]
] | [
[
850,
972
],
[
1106,
1157
]
] |
2016ApJ...821...74J__Díaz_et_al._2016_Instance_1 | Recent theoretical work has suggested that the presence, or lack thereof, of long-period giant planets could affect the formation of such systems. Batygin & Laughlin (2015) argued that the migration of Jupiter within our own solar system might have disrupted a massive primordial inner protoplanetary disk that could hav... | [
"Díaz et al. 2016"
] | [
"Super-Earths can be found with either high-precision RV observations or space-based transit searches. Such high-precision RV surveys include those being undertaken currently with HARPS (e.g.,"
] | [
"Background"
] | [
[
1085,
1101
]
] | [
[
893,
1084
]
] |
2021ApJ...921..179L__Hayes_et_al._2019_Instance_1 | Quasi-periodic pulsations (QPPs) often refer to the quasi-periodic intensity variations during solar/stellar flares (see Zimovets et al. 2021, for a recent review). In many observations, the flare QPPs were found to show a nonstationary property in the time series integrated over the whole Sun/star or over the oscillat... | [
"Hayes et al. 2019"
] | [
"The signature of flare QPPs can be detected in flare light curves across a broad band of the electromagnetic spectrum, i.e., radio/microwave emissions"
] | [
"Background"
] | [
[
749,
766
]
] | [
[
472,
622
]
] |
2019AandA...632A.104G__Hirabayashi_et_al._2016_Instance_2 | Finally, our observations are consistent with the bilobate shape of the nucleus of comet 8P/Tuttle. As noted in Sect. 1, this shape is likely common among comets because it was found for four out of the six comets for which we have spatially resolved images. This is also the case of the trans-Neptunian object 2014 MU69... | [
"Hirabayashi et al. (2016)"
] | [
"For cometary nuclei, the primary cause for spin-up is torques caused by outgassing, therefore it is possible that 8P/Tuttle formed as a monolithic body and became a contact binary after its injection into the inner Solar System as a result of excessive spin-up resulting from non-gravitational forces. This scenario... | [
"Compare/Contrast"
] | [
[
1892,
1917
]
] | [
[
1519,
1891
]
] |
2020AandA...641A.155V__Gómez-Guijarro_et_al._2019_Instance_2 | The scenario presented above has been formulated in various flavors to individually explain several of the properties reported here. The main addition of this work, namely the excitation of CO in distant main-sequence and starburst galaxies, fits in the general picture that we sketched. The ensemble of properties and c... | [
"Gómez-Guijarro et al. 2019"
] | [
"Such transition might well imply an imminent increase of the SFR, driving the object in the realm of starbursts",
"or its cessation, bringing the system back onto or even below the main sequence",
"with the CO properties potentially able to distinguish between these two scenarios."
] | [
"Compare/Contrast",
"Compare/Contrast",
"Future Work"
] | [
[
1419,
1445
]
] | [
[
1198,
1309
],
[
1338,
1417
],
[
1469,
1552
]
] |
2018ApJ...866L...1S__Pecharromán_et_al._1999_Instance_3 | It was found that the complex dielectric function from Pecharromán et al. (1999) for the sample obtained by heating bayerite at 1273 K, assuming a spheroid with depolarization parameters of (0.35, 0.003), produced an opacity with 11, 20, 28, and 32 μm features, so this component was included in the models. However, wit... | [
"Pecharromán et al. 1999"
] | [
"The complex dielectric functions of the samples obtained by heating bayerite and boehmite to various temperatures",
"were derived by modeling the reflectance spectra of pellets obtained by pressing powders of these materials under great pressure"
] | [
"Uses",
"Uses"
] | [
[
891,
914
]
] | [
[
776,
889
],
[
916,
1044
]
] |
2017MNRAS.471.4256V__King_et_al._2000_Instance_1 | Our ideas about which systems may survive spiral-in and produce WR X-ray binaries were triggered by the realization that the peculiar X-ray binary SS433 has avoided going into CE evolution, and that the donor star in this system is transferring mass to the compact star by stable Roche lobe overflow (RLOF; King & Begelm... | [
"King et al. 2000"
] | [
"The avoidance of its going into CE evolution is – as we will argue – a consequence of the donor star having a radiative envelope"
] | [
"Uses"
] | [
[
1012,
1028
]
] | [
[
882,
1010
]
] |
2016AandA...586A..92P__Maciesiak_et_al._2012_Instance_1 | We calculated the dependence of the width of the profiles on the pulse period, considering the different frequencies separately. We note that the pulse width is not a direct reflection of the beam size or diameter (i.e. 2ρ, where ρ is beam radius). For a visual representation of the geometry see for instance Maciesiak ... | [
"Maciesiak et al. 2012"
] | [
"In such a case, when the emission beam is confined by dipolar open field lines, we would expect a P− 1 / 2 dependence, which has indeed been observed when correcting for geometrical effects by transforming the pulse width into a beam radius measurement (see"
] | [
"Compare/Contrast"
] | [
[
811,
832
]
] | [
[
519,
776
]
] |
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