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 |
|---|---|---|---|---|---|---|
2020ApJ...900..143S__Potgieter_et_al._2014_Instance_1 | It is well known that there exists an anticorrelation between the cyclic variations of GCR intensity and SSN (Forbush 1954), and the time lag in this relationship has also been reported by Forbush (1958). The time lag in solar modulation of GCRs should be closely related to the transport of solar wind plasma with its e... | [
"Potgieter et al. 2014"
] | [
"This effect has been considered in numerical models of GCR modulation to study the long-term modulation mechanism (e.g.,"
] | [
"Background"
] | [
[
556,
577
]
] | [
[
363,
483
]
] |
2018AandA...619A..59S__Sander_et_al._2015_Instance_1 | Information about fundamental parameters of stars – like their mass, luminosity, surface temperature and chemical composition – comes primarily from matching observations to synthetic spectra computed using models of stellar atmospheres. For massive stars with hot surfaces, scattering and absorption in spectral lines f... | [
"Sander et al. 2015"
] | [
"Over the past decades, much effort has been devoted toward constructing such global NLTE, steady-state model atmospheres of hot stars with winds; several numerical computer codes meanwhile exist on the market, for example",
"POWR"
] | [
"Background",
"Background"
] | [
[
1988,
2006
]
] | [
[
1706,
1927
],
[
1960,
1964
]
] |
2022MNRAS.516..167B__Steinborn_et_al._2015_Instance_1 | Otherwise (i.e. if there is insufficient mass left in the sub-grid gas reservoir), the mass deficit $m_\mathrm{BH} + \Delta m - m_\mathrm{BH}^\mathrm{dynamical}$ (the last term denotes the dynamical mass of the SMBH) is drawn from the surrounding gas particles. In eagle, this was done by stochastically swallowing indiv... | [
"Steinborn et al. 2015"
] | [
"This is not an ideal approach: the momentum imparted on the SMBH from the swallowed gas particle may artificially dislodge it from its position, particularly without instantaneous repositioning (as also discussed by"
] | [
"Compare/Contrast"
] | [
[
558,
579
]
] | [
[
342,
557
]
] |
2017ApJ...834...20A__Temi_et_al._2007a_Instance_1 | Lenticular galaxies seems to have a wider range of properties compared to ellipticals that resemble more the old definition of ETGs. However, even in ellipticals, large differences prevail. Recent observations of elliptical galaxies with Spitzer and Herschel (Temi et al. 2005, 2007a, 2007b, 2009; Smith et al. 2012; Agi... | [
"Temi et al.",
"2007a"
] | [
"However, even in ellipticals, large differences prevail. Recent observations of elliptical galaxies with Spitzer and Herschel",
"have revealed that the far-infrared (FIR) luminosity LFIR from these galaxies can vary by ∼100 among galaxies with similar optical luminosity."
] | [
"Background",
"Background"
] | [
[
260,
271
],
[
278,
283
]
] | [
[
133,
258
],
[
357,
499
]
] |
2020ApJ...905..111Z__Jirička_et_al._2001_Instance_2 | Surveys of radio bursts in decimetric wavelengths is presented in papers by Isliker & Benz (1994) and Jirička et al. (2001), within 1–3 GHz and 0.8–2.0 GHz frequency ranges, respectively. Some of these bursts are still not well understood. This is a case of the slowly positively drifting bursts (SPDBs). They appear in ... | [
"Jirička et al. 2001"
] | [
"Some of these bursts are still not well understood. This is a case of the slowly positively drifting bursts (SPDBs). They appear in groups or as single bursts, with a duration of an individual burst from 1 to several seconds and their frequency drift is lower than about 100 MHz s−1"
] | [
"Background"
] | [
[
472,
491
]
] | [
[
188,
470
]
] |
2022MNRAS.513.4556Z__Swartz,_Wheeler_&_Harkness_1991_Instance_1 | Type II supernovae (SNe II) are believed to originate from the core collapse of massive stars with initial masses larger than 8 M⊙ (Heger et al. 2003). They are characterized by prominent P-Cygni profiles of Balmer series in their spectra (Filippenko 1997). Photometrically, they are classified as SNe IIP if their light... | [
"Swartz, Wheeler & Harkness 1991"
] | [
"Such a distribution is believed to be related to the mass of the hydrogen envelope maintained by the progenitor stars, as evidenced by the results that SNe having larger envelope masses produce light curves with shallower plateau slopes and longer plateau durations"
] | [
"Motivation"
] | [
[
1029,
1060
]
] | [
[
742,
1007
]
] |
2021ApJ...911...75M__Yamauchi_et_al._2004_Instance_1 | With the advent of the Parker Solar Probe (PSP) we are able to directly measure properties of the solar wind closer to the Sun than ever before (Fox et al. 2016). One of the early highlight discoveries of PSP is the omnipresence of strong local deflections of the magnetic field in the solar wind, mostly referred to as ... | [
"Yamauchi et al. 2004"
] | [
"Several explanations about their origin have been put forth. Among these theories, interchange reconnection is the most focused upon",
"In this scenario, switchbacks are generated in the solar corona, and form at the reconnection sites between open and closed magnetic fluxes."
] | [
"Background",
"Background"
] | [
[
1689,
1709
]
] | [
[
1555,
1687
],
[
1743,
1883
]
] |
2021ApJ...917...59C__Schiller_et_al._2020_Instance_1 | With regard to Ni isotopes in the metal phase of iron meteorites, multiple studies have analyzed samples belonging to the same iron groups (e.g., IIAB, IIIAB, IVA, IVB) using broadly similar techniques (i.e., wet chemical separation of Ni followed by mass spectrometry). The initial studies reported no nucleosynthetic a... | [
"Schiller et al. 2020"
] | [
"However, more recent studies",
"have revealed small non-mass-dependent variations in Fe isotopes."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
987,
1007
]
] | [
[
931,
959
],
[
1009,
1074
]
] |
2017ApJ...837...89W__Henry_et_al._2013_Instance_1 | For over a decade, a tight correlation between metallicity and galaxy stellar mass (
), i.e., the mass–metallicity relation (MZR), has been quantitatively established, from the vast database of local galaxies observed by the Sloan Digital Sky Survey (SDSS; Tremonti et al. 2004; Zahid et al. 2012; Andrews & Martini... | [
"Henry et al. 2013"
] | [
"This relation has been further extended to high redshifts, using deep near-infrared (IR) spectroscopy facilitated by large ground-based and space-based telescopes"
] | [
"Background"
] | [
[
550,
567
]
] | [
[
328,
490
]
] |
2016ApJ...817..152X__Brien_et_al._2006_Instance_1 | Afterglows of gamma-ray bursts (GRBs) are generally believed to be produced by a relativistic jet interacting with the surrounding medium (e.g., Mészáros & Rees 1997; Sari et al. 1998; Kumar & Zhang 2015). Very early multi-wavelength afterglows are critical to reveal the properties of the radiating fireball and its env... | [
"O’Brien et al. 2006"
] | [
"The early X-ray afterglows are usually dominated by erratic X-ray flares and the tail emission of prompt gamma-rays are due to the arrival time delay of photons in the high latitude of the radiating fireball"
] | [
"Background"
] | [
[
812,
831
]
] | [
[
584,
791
]
] |
2022ApJ...926..151Z__Saxena_et_al._2020_Instance_1 | Unlike the CMB, the 21 cm signal is highly non-Gaussian, because patchy, bubble-like structures of ionized hydrogen (H ii) regions are produced surrounding the ionizing sources. Thus, there is potentially a wealth of information in the 21 cm signal that is not contained in the 21 cm power spectrum, a two-point statisti... | [
"Saxena et al. 2020"
] | [
"Toward this goal, conventionally, new summary statistics that can only be measured with imaging have been proposed. These include",
"bispectrum"
] | [
"Background",
"Background"
] | [
[
885,
903
]
] | [
[
559,
688
],
[
772,
782
]
] |
2020MNRAS.499.1788W__Wolfire_et_al._2003_Instance_1 | Owing to their brightness at rest-frame FIR wavelengths, the ionized and neutral species of Carbon, Nitrogen, and Oxygen are powerful diagnostic lines for tracing the ISM of nearby and distant galaxies. When combined with photodissociation region (PDR) models (Tielens & Hollenbach 1985), measurement of the emission fro... | [
"Wolfire et al. 2003"
] | [
"The [C ii]158 μm line is typically the brightest in star-forming galaxies, arising from ionized, and even neutral gas where it is the main coolant"
] | [
"Background"
] | [
[
873,
892
]
] | [
[
725,
871
]
] |
2021MNRAS.508.2823C__Baumgardt,_Makino_&_Ebisuzaki_2004_Instance_1 | Globular clusters are of particular dynamical interest because of the phenomena of core collapse and binary burning. Stellar interactions in dense globular clusters tend to drive the central core towards a collapse to a state of extremely small radius and high density. Primordial binary populations may delay the onset ... | [
"Baumgardt, Makino & Ebisuzaki 2004"
] | [
"In addition, an intermediate-mass black hole (IMBH) in a cluster core will act as a strong central energy source able to delay, or even prevent, core collapse (e.g."
] | [
"Background"
] | [
[
925,
959
]
] | [
[
760,
924
]
] |
2022MNRAS.512.3137Z__Katz_et_al._1999_Instance_3 | However, it is not straightforward to explain H2 formation in astronomical sources even when the catalytic roles of dust grains are introduced into models. Interstellar species are believed to be formed on cold grain surfaces via the so called Langmuir–Hinshelwood mechanism (Watson & Salpeter 1972; Pickles & Williams 1... | [
"Katz et al. 1999"
] | [
"Moreover, it was found that the highest dust temperature at which H2 can be formed efficiently is less than 17 K"
] | [
"Background"
] | [
[
1807,
1823
]
] | [
[
1693,
1805
]
] |
2016ApJ...817...12P__Chamandy_et_al._2014_Instance_2 | Large-scale magnetic fields with strength of the order of 1–10 μG have been observed in disk galaxies (e.g., Beck et al. 1996; Fletcher 2010; Beck 2012; Beck & Wielebinski 2013; Van Eck et al. 2015). The origin of these fields can be explained through mean-field dynamo theory (Ruzmaikin et al. 1988; Beck et al. 1996; B... | [
"Chamandy et al. 2014"
] | [
"and through diffusive flux"
] | [
"Background"
] | [
[
1504,
1524
]
] | [
[
1404,
1430
]
] |
2017AandA...605A.102C__Konstantinova-Antova_et_al._2013_Instance_1 | Magnetic fields are actively searched for at the surface of all kinds of stars throughout the Hertzsprung-Russell diagram (HRD), as they probably impact stellar evolution from birth to death in various ways (see e.g., Donati & Landstreet 2009 for a general review; and Wade et al. 2016; Alecian et al. 2013; Vidotto et a... | [
"Konstantinova-Antova et al. 2013"
] | [
"Recently, magnetic fields have been unambiguously detected via Zeeman signatures in a large sample of single G-K giants observed with the spectropolatimeters TBL/Narval and CFHT/ESPaDOnS"
] | [
"Background"
] | [
[
627,
659
]
] | [
[
439,
625
]
] |
2019MNRAS.488.5748W__Mao_&_Schneider_1998_Instance_1 | The search for observational evidence of dark matter substructure in galaxies is on-going, as traditional methods for in-directly detecting dark matter sub-haloes (e.g. modelling tidal streams and gravitational lensing) have yet to agree on either the Milky Way’s or an external galaxies’ current substructure compositio... | [
"Mao & Schneider 1998"
] | [
"Gravitational lensing allows for constraints to be placed on the dark matter substructure content of external galaxies, as orbiting sub-haloes will result in anomalies in strong gravitational lenses"
] | [
"Motivation"
] | [
[
523,
543
]
] | [
[
323,
521
]
] |
2021MNRAS.506.1978L__Krivov_et_al._2018_Instance_1 | This dynamical limit on planetesimal sizes could suggest that these may exist in the belt a factor of 103 larger than the ${\sim }1\,$km sized lower limit predicted by collisional replenishment. However, if the assumed α = 3.5 Dohnanyi (1969) size distribution continued up to planetesimals of this size, then the disc m... | [
"Krivov et al. 2018"
] | [
"Whilst this higher total disc mass is still consistent with the dust mass measurements of protoplanetary discs",
"high debris disc masses, i.e. those in the range of $100\\!-\\!1000\\, M_{\\oplus }$, become problematic since these would require a very high efficiency of primordial dust being incorporated into th... | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1196,
1214
]
] | [
[
727,
837
],
[
922,
1195
]
] |
2015AandA...576A...5C__Jørgensen_et_al._2012_Instance_1 | The relative abundances of the three species are derived from the column densities in Table 2 and are compared with other star-forming regions and comets in Table 3. The (CH2OH)2/CH2OHCHO abundance ratio of ~0.3–0.5 previously derived in IRAS 16293 by Jørgensen et al. (2012) was revised. Indeed, the assignment in Jørge... | [
"Jørgensen et al. (2012)"
] | [
"The (CH2OH)2/CH2OHCHO abundance ratio of ~0.3–0.5 previously derived in IRAS 16293 by",
"was revised."
] | [
"Differences",
"Differences"
] | [
[
252,
275
]
] | [
[
166,
251
],
[
276,
288
]
] |
2015ApJ...799...99K__Coelho_&_Gadotti_2011_Instance_2 | The nonaxisymmetric potential of a bar induces large-scale streaming motions in stars and gas into the central part of the galaxy (e.g., Athanassoula 1992a, 1992b; Sellwood & Wilkinson 1993). Being dissipative, the gas loses angular momentum and energy and flows inward toward the galactic center (Knapen et al. 1995; R... | [
"Coelho & Gadotti 2011"
] | [
"Some studies find weak statistical links among AGN activity and the presence of bars (e.g.,"
] | [
"Background"
] | [
[
1590,
1611
]
] | [
[
1414,
1505
]
] |
2018MNRAS.479.4073L__Chatterjee_et_al._2008_Instance_1 | As can be seen from Fig. 1, in both the optical and the NIR band, several predominant flares appearing in the whole period considered are usually surrounded by other smaller subflares. In addition, it seems that the NIR light curves follow a similar flaring activity, lasting for several days or weeks, to the optical ba... | [
"Chatterjee et al. 2008"
] | [
"An exponential rise/decay model can appropriately fit the blazar light curve, which generally consists of superpositions of a steady background flux density and a number of flare components caused by events in the jet or the accretion disc/corona region (e.g."
] | [
"Uses"
] | [
[
774,
796
]
] | [
[
492,
751
]
] |
2022MNRAS.511.4946N__Vivek,_Srianand_&_Gupta_2016_Instance_1 | Outflows from the central regions of active galactic nuclei (AGNs) are thought to be the main agents that regulate the evolution of both the central supermassive black holes as well as the host galaxies (Silk & Rees 1998; Di Matteo, Springel & Hernquist 2005). The presence of high-velocity outflows from AGNs can be est... | [
"Vivek, Srianand & Gupta 2016"
] | [
"BALQSOs are classified into three sub-classes based on the ionization state of the absorbing gas: (a) high-ionization BALQSOs (HiBALs) consist of absorption from high-ionization lines such as C iv, Si iv, and N v"
] | [
"Background"
] | [
[
755,
783
]
] | [
[
499,
711
]
] |
2021MNRAS.503.1319G__Bolton_et_al._2008_Instance_1 | In this paper, following the method proposed by Ofek et al. (2003), we use the differential optical depth to lensing with respect to the lens redshift zl as the probability density. For a statistical sample that contains Nl strong lensing systems, the log-likelihood of observing the lens at redshift zl is given by
(9)$... | [
"Bolton et al. 2008"
] | [
"The sample used in this paper is primarily drawn from Sloan Lens ACS Survey (SLACS)",
"The combined sample includes 91 lenses from SLACS"
] | [
"Uses",
"Uses"
] | [
[
1081,
1099
]
] | [
[
820,
903
],
[
1030,
1079
]
] |
2018AandA...611A..74R__Grady_et_al._2013_Instance_3 | In this context, MWC 758 (HD 36112) offers a unique environment to probe the existence of planetary companions and to explore the connection between disk structures and planet formation. MWC 758 is a young stellar object (3.5 ± 2 Myr, Meeus et al. 2012) at a distance of 151
$^{+9}_{-8}$
151
−9
+8
4
pc (Ga... | [
"Grady et al. (2013)"
] | [
"Using Ks-band (2.15 μm) direct imaging andH-band (1.65 μm) polarimetric imaging with the High-Contrast Instrument with Adaptive Optics (HiCIAO) at the Subaru Telescope,",
"detected two spiral arms and polarized light down to 0.′′ 1 (15 au) from the star."
] | [
"Background",
"Background"
] | [
[
1583,
1602
]
] | [
[
1414,
1582
],
[
1603,
1685
]
] |
2021AandA...650A.205V__Fontaine_et_al._2012_Instance_1 | The formation of the approximately 40% of sdB stars that appear to be single has been a mystery for decades. In the absence of a companion, it is hard to explain how the star can expel most of its envelope on the RGB and still achieve core-He burning ignition. Recently, Pelisoli et al. (2020) suggested that all sdB sta... | [
"Fontaine et al. 2012"
] | [
"Second, the mass distributions of single and binary sdB stars are indistinguishable (",
", Table 3 in particular)."
] | [
"Motivation",
"Motivation"
] | [
[
762,
782
]
] | [
[
677,
762
],
[
782,
807
]
] |
2016AandA...595A.106C__Korista_&_Goad_2000_Instance_1 | The present HST-COS data were taken 20 days after the last XMM-Newton pointing (Kaastra et al. 2011) as the closing measurements of the campaign, which lasted in total about 100 days. Spectral coverage simultaneous to HST-COS was provided instead by both Chandra-LETGS (Ebrero et al. 2011) and Swift-XRT (Mehdipour et al... | [
"Korista & Goad 2000"
] | [
"The choice of SED is very important in the BLR modeling, as different lines respond to the continuum variations on different time scales"
] | [
"Motivation"
] | [
[
573,
592
]
] | [
[
435,
571
]
] |
2022AandA...666L...5G__Esquej_et_al._2014_Instance_1 | More recently, García-Bernete et al. (2022) found that the PAH molecules responsible for the 11.3 μm PAH emission band are more resilient in the hard environments often present in AGN. In particular, the authors found larger 11.3/7.7 μm and 11.3/6.2 μm PAH ratios in AGN-dominated systems compared to SF galaxies, indica... | [
"Esquej et al. 2014"
] | [
"Previous sub-arcsecond angular resolution N-band (∼8–13 μm) ground-based spectroscopic studies investigated the 11.3 μm PAH feature in the nuclear and circumnuclear regions of AGN (e.g.,",
"However, these works were unable to provide definitive details regarding the effect of the AGN on the PAH molecules due to ... | [
"Background",
"Motivation"
] | [
[
880,
898
]
] | [
[
592,
778
],
[
980,
1147
]
] |
2022AandA...661A..10B__Ghirardini_et_al._2021a_Instance_2 | It is also possible that these clusters have a smaller extent and can just be missed by our extent selection as our detection algorithm sets the extent to zero if it is smaller than 6 (Brunner et al. 2022). Following the method presented in Ghirardini et al. (2021a), we estimated several dynamical properties of the clu... | [
"Ghirardini et al. (2021a)"
] | [
"we estimated several dynamical properties of the clusters in the point source sample and compared them with the extent-selected sample presented in"
] | [
"Uses"
] | [
[
416,
441
]
] | [
[
268,
415
]
] |
2016MNRAS.463.2348S__Narlikar_&_Padmanabhan_1991_Instance_1 | We appear to live in a flat, homogeneous and isotropic expanding Universe (at scales >100 Mpc) well described by the Friedmann–Lemaître–Robertson–Walker (FLRW) metric where the scalefactor, a(t), describes the time dependence of the Universe geometry: a(t) ∝ t1/2 for radiation domination, a(t) ∝ t2/3 for matter dominat... | [
"Narlikar & Padmanabhan 1991"
] | [
"Between the end of inflation at t = te ∼ 10−33 s; (e.g.",
"and t = teq = 2.37 × 1012 s, the Universe was radiation-dominated since at the latter instant a radiation-matter equality is reached (Table 1)."
] | [
"Background",
"Background"
] | [
[
1146,
1173
]
] | [
[
1090,
1145
],
[
1175,
1318
]
] |
2021MNRAS.505..435S__Goodman_2009_Instance_1 | Detections of ionic, atomic, and molecular species in exoplanetary atmospheres serve as a unique and strong diagnostic of those chemical and dynamical processes driving their formation and evolution. Their detection and abundance measurements could act as indicators of planetary formation scenarios and reveal connectio... | [
"Goodman 2009"
] | [
"Furthermore, discoveries of atmospheric chemical species allow us to better understand various thermodynamical processes and chemistry, winds in the upper atmosphere"
] | [
"Background"
] | [
[
619,
631
]
] | [
[
452,
617
]
] |
2018AandA...616A.139G__Rao_et_al._(2009)_Instance_1 | Observations of the polarized dust emission of nine low-mass protostars at 0.87 mm were obtained using the SMA (Projects 2013A-S034 and 2013B-S027, PI: A. Maury) in the compact and subcompact configuration. To increase our statistics, we also included SMA observations from three additional sources from Perseus (NGC 133... | [
"Rao et al. (2009)"
] | [
"The observations of NGC 1333 IRAS4A and IRAS16293 are presented in Girart et al. (2006) and",
"respectively."
] | [
"Background",
"Background"
] | [
[
575,
592
]
] | [
[
483,
574
],
[
594,
607
]
] |
2020MNRAS.494.2465B__Lee,_Sode-Yome_&_Park_1991_Instance_1 | Here we demonstrate that, over a fixed time interval, the planar three-body problem can be solved by means of a multilayered deep artificial neural network (ANN; e.g. see LeCun, Bengio & Hinto 2015). These networks are designed for high-quality pattern recognition by mirroring the function of our brains (McCulloch & Pi... | [
"Lee, Sode-Yome & Park 1991"
] | [
"Together, these properties lead to the result that an ANN can be trained to provide accurate and practical solutions to Newton’s laws of motion, resulting in major improvements in computational economy",
"relative to modern technologies."
] | [
"Motivation",
"Motivation"
] | [
[
1108,
1134
]
] | [
[
905,
1106
],
[
1136,
1168
]
] |
2022ApJ...926..208Y__Zheng_&_Hu_2018_Instance_1 | Magnetic flux ropes are frequently observed magnetic structures with helical magnetic field lines and a strong core field. In spacecraft observations, flux ropes are often identified from bipolar variations in one magnetic field component and the enhancement of magnetic strength at the center. There are various observa... | [
"Zheng & Hu 2018"
] | [
"There are various observations of flux ropes in the",
"and solar wind (e.g.,"
] | [
"Background",
"Background"
] | [
[
643,
658
]
] | [
[
295,
346
],
[
621,
642
]
] |
2022ApJ...934..145I__from_1995_Instance_1 | The projected position angle (PA) of the jet gradually rotates counterclockwise with increasing distance from the jet base. In the 2.3 GHz VLBA image the PA is 50° ± 5° east of north at about 20 mas from the core and the jet bends toward the north–south direction closer to the core, consistently with the jet orientatio... | [
"Kellermann et al. 1998"
] | [
"At 8.7 GHz we find a PA of 25° ± 5° at about 5 mas from the core, consistent with the archival VLBA monitoring results at 15 GHz, showing a persistent jet orientation at a PA of about 30° in the epochs from 1995 to 2013 at angular scales ∼5 mas"
] | [
"Compare/Contrast"
] | [
[
651,
673
]
] | [
[
405,
649
]
] |
2021AandA...656A..16C__Bruno_&_Carbone_2013_Instance_2 | Investigations of the turbulent nature of solar wind fluctuations have been ongoing for more than half a century (see, e.g., Bruno & Carbone 2016). Advances have been made consistently thanks to the increasingly accurate measurements of several dedicated space mission as well as to the enormous improvement of numerical... | [
"Bruno & Carbone 2013"
] | [
"Magnetic field fluctuations have been characterized with great detail at magnetohydrodynamic and kinetic scales, for example, through spectral and high-order moments analysis"
] | [
"Background"
] | [
[
1078,
1098
]
] | [
[
884,
1058
]
] |
2021AandA...654A.124W__Gao_et_al._2015_Instance_1 | In view of the ultrahigh mass of the merger product of around 2.5 M⊙, it is undoubtedly necessary and important to further test the existence of post-merger NSs (Gao et al. 2016; Li et al. 2016, 2017; Ai et al. 2018; Zhu et al. 2018; Sarin et al. 2020; Beniamini & Lu 2021), which can provide a robust constraint on the ... | [
"Gao et al. 2015"
] | [
"Besides the GRB 170817A/AT 2017gfo event, searches for possible kilonova emission have already been carried out in the afterglows of many SGRBs since 2013"
] | [
"Background"
] | [
[
688,
703
]
] | [
[
439,
593
]
] |
2020ApJ...894..107I__Kastner_et_al._1994_Instance_1 | AFGL 2136 IRS 1 (also referred to as CRL 2136, G17.64+0.16, and IRAS 18196−1331) is a luminous (1.0 × 105 L; Lumsden et al. 2013), high-mass (45 ± 10 M; Maud et al. 2019) protostar that is believed to be in the latter stages of its evolution due to a variety of observed characteristics (Boonman & van Dishoeck 2003; Mau... | [
"Kastner et al. 1994"
] | [
"The large scale outflow is observed in CO emission at millimeter wavelengths, with both the red and blue lobes being about 100″ in extent"
] | [
"Background"
] | [
[
874,
893
]
] | [
[
735,
872
]
] |
2021AandA...650L...4B__DeForest_et_al._2016_Instance_1 | As Parker Solar Probe (PSP) descends deeper into the solar corona on its succeeding orbits, its measurements reveal features of the heliospheric plasma that will significantly increase our fundamental understanding of the workings of the solar corona, the origins of the solar wind, and the behavior of heliospheric ener... | [
"DeForest et al. 2016"
] | [
"In this very region, the analysis of heliospheric imaging (HI;",
"has described a transition from striated images that appear to be highly collimated due to a structured magnetic field and lower plasma beta to higher altitude images that appeared to be more disordered and isotropic, a condition described as “flo... | [
"Background",
"Background"
] | [
[
801,
821
]
] | [
[
738,
800
],
[
823,
1081
]
] |
2018AandA...609A..28B__Hansen_&_Milosavljević_2003_Instance_1 | A number of works have tried to explain this conundrum with different ideas, which follow one of three possibilities. When Genzel et al. (1996) first discovered missing RGB stars, they proposed that this might be due to stellar collisions depleting giant stars in the innermost parts through the high stellar densities t... | [
"Hansen & Milosavljević 2003"
] | [
"Such a massive secondary black hole would require the Milky Way to have experienced a major merger relatively recently, which is excluded by observations (see"
] | [
"Background"
] | [
[
1306,
1333
]
] | [
[
1147,
1305
]
] |
2021MNRAS.504..444C__Steiner_&_McClintock_2012_Instance_1 | After a first part of ballistic, high-speed motion, the deceleration of RK1 was rather abrupt, which is something not observed in the majority of discrete ejecta from BH XRBs (e.g Mirabel & Rodríguez 1994; Fender et al. 1999; Miller-Jones et al. 2012). This scenario is consistent with a jet that travels first at consta... | [
"Steiner & McClintock 2012"
] | [
"Those cavities have been suggested to exist at ∼pc scales at least for XTE J1550–564 and H1743–322"
] | [
"Uses"
] | [
[
815,
840
]
] | [
[
697,
795
]
] |
2018ApJ...852L...1Z__Metzger_2017_Instance_1 | The short gamma-ray burst (GRB) 170817A was observed by the Fermi- Gamma-ray Burst Monitor (GBM; Goldstein et al. 2017). The fact that it was not detected by the Insight Hard X-ray Modulation Telescope (Li et al. 2017) suggests that the burst had a very weak fluence and a soft spectrum. The burst was highly noticeable ... | [
"Metzger 2017"
] | [
"Compared with other short GRBs, the luminosity of GRB 170817A was extremely weak, thus suggesting that the jet was off-axis to the line of sight"
] | [
"Compare/Contrast"
] | [
[
908,
920
]
] | [
[
627,
771
]
] |
2017ApJ...845...86E__Soler_&_Terradas_2015_Instance_3 | Among the suggestedmechanisms responsible for the strong damping of the coronal loop oscillations (e.g., Ruderman & Roberts 2002; Ofman 2005, 2009; Morton & Erdélyi 2009) resonant absorption of the MHD waves, which was established first by Ionson (1978), is a strong candidate. Several works developed this theory (e.g.,... | [
"Soler & Terradas 2015"
] | [
"There are a variety of theoretical works related to the damping of the coronal loop oscillations based on the theory of resonant absorption of MHD waves (e.g.,"
] | [
"Background"
] | [
[
1923,
1944
]
] | [
[
1576,
1735
]
] |
2018ApJ...855...48Q__Falgarone_&_Passot_2003_Instance_1 | The dust condensations could not arise from a thermal Jeans fragmentation process. If that is the case, with a density of 104–105 cm−3 for the surrounding medium, one may expect the mass of the condensations on the order of 20–50 M⊙ (the Jeans mass at 105–104 cm−3) and the nearest separations between the condensations ... | [
"Falgarone & Passot 2003"
] | [
"Alternatively, small dense structures can be temporary density fluctuations frequently created and destroyed by supersonic turbulence (e.g.,"
] | [
"Background"
] | [
[
598,
621
]
] | [
[
427,
567
]
] |
2021AandA...652A.124N__Wiśniewska_et_al._(2016)_Instance_1 | Figure 9 presents Fourier power spectrum for wave period P versus height. The initial pulse has a Gaussian spectrum of wave number k which results in a spectrum of period P. The steepening of the magnetoacoustic waves results from the growing wave amplitude with height. Hence, waves with shorter wavelengths and wave pe... | [
"Wiśniewska et al. (2016)"
] | [
"We note that some of our data fits the observational findings of",
"represented by diamonds over-plotted on the power spectra",
"The agreement of the theory with the observational data indicates that the results can be used to determine the background structure of the solar atmosphere and confirms that wave ge... | [
"Similarities",
"Uses",
"Compare/Contrast"
] | [
[
925,
949
]
] | [
[
860,
924
],
[
951,
1008
],
[
1054,
1338
]
] |
2017MNRAS.465..492M__Taverna_et_al._2015_Instance_1 | Given the quite strong surface magnetic field of the M7, thermal radiation is expected to be polarized, either if emission is from a bare surface or from an atmosphere (see Turolla et al. 2004; Potekhin 2014). The polarization properties are quite different in the two cases, although there are still uncertainties, espe... | [
"Taverna et al. 2015"
] | [
"In the absence of QED vacuum polarization effects, this would produce a drastic depolarization of the radiation collected at infinity",
"see also"
] | [
"Background",
"Background"
] | [
[
966,
985
]
] | [
[
795,
928
],
[
957,
965
]
] |
2019AandA...622A.146M__Arribas_et_al._(2014)_Instance_2 | Previous works (e.g. Holt et al. 2011; Arribas et al. 2014; Villar Martín et al. 2014, 2015) have found very high reddening and densities associated with ionised outflows in local objects (e.g. Hα/Hβ ∼ 4.91 and ne ≳ 1000 cm−3, Villar Martín et al. 2014). Concerning the reddening, although we find that the outflowing ga... | [
"Arribas et al. (2014)"
] | [
"This could stem from the fact that the galaxies studied by Holt et al. (2011),",
"are local luminous or ultra-luminous infrared galaxies (U/LIRGs), and those of Villar Martín et al. (2014, 2015) are highly obscured Seyfert 2, thus sampling sources that are more gas and dust rich compared to our sample."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
744,
765
]
] | [
[
665,
743
],
[
766,
987
]
] |
2020AandA...641A.155V__Gómez-Guijarro_et_al._2019_Instance_1 | 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"
] | [
"We do detect starburst-like behaviors in galaxies on the main sequence",
"likely linked to the existence of transitional objects"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1058,
1084
]
] | [
[
869,
939
],
[
961,
1015
]
] |
2022MNRAS.512.2854P__Pétri,_Heyvaerts_&_Bonazzola_2002_Instance_1 | The aforementioned fluid description offers a good starting point to understand the global electric circuit made of charge and current densities. However, it neglects some fundamental kinetic aspects required to self-consistently include single particle acceleration as well as radiation feedback. As kinetic simulations... | [
"Pétri, Heyvaerts & Bonazzola 2002"
] | [
"Eventually Philippov & Spitkovsky (2014) computed the first two-dimensional axisymmetric pulsar magnetosphere for an aligned rotator by permanently injecting particle supposed to be released from the surface, avoiding to end to an electrosphere configuration"
] | [
"Background"
] | [
[
1347,
1380
]
] | [
[
1087,
1345
]
] |
2021AandA...646L...9M__Quan_&_Herbst_(2007)_Instance_1 | The chemistry of C4H3N isomers in cold molecular clouds was discussed by Balucani et al. (2000), and more specifically by Balucani et al. (2002), based on crossed molecular beam experiments and ab initio calculations. In these studies, it was pointed out that reactions of the CN radical with methyl acetylene and allene... | [
"Quan & Herbst (2007)"
] | [
"This chemical scheme was implemented in a chemical model by",
"to explain the abundance of cyanoallene in TMC-1."
] | [
"Background",
"Background"
] | [
[
661,
681
]
] | [
[
601,
660
],
[
682,
731
]
] |
2022MNRAS.509..619I__Różańska_et_al._2011_Instance_1 | A number of sources of systematic error disproportionately affect the soft X-rays. One important example is absorption by partially ionized material around the AGN. Although the response of the absorbing gas to changes in the irradiating flux from the AGN does contribute its own time lag, this should only influence the... | [
"Różańska et al. 2011"
] | [
"The soft X-ray region of the reflection spectrum is also the most sensitive to modelling assumptions such as vertical disc structure"
] | [
"Compare/Contrast"
] | [
[
962,
982
]
] | [
[
770,
902
]
] |
2019MNRAS.489.2792Z__Zahid_et_al._2014_Instance_1 | The compact blobs instead likely have a different origin. The fact that compact blobs are unresolved even at the HST resolution, that they are found at ∼1 kpc distance from the galaxy barycentre, that they have relatively small stellar masses (≲15 per cent of the underlying disc), but are actively forming stars suggest... | [
"Zahid et al. 2014"
] | [
"The in situ formation of the compact blobs is further supported by their metallicity. In fact, while the disc properties are consistent with the stellar mass–metallicity relation of z ∼ 2 star-forming galaxies (e.g.",
"compact blobs instead show metallicities inconsistent with the mass–metallicity relation (Fig.... | [
"Similarities",
"Differences"
] | [
[
721,
738
]
] | [
[
483,
698
],
[
741,
859
]
] |
2018AandA...616A..99K__Narang_et_al._2016_Instance_2 | The high-resolution imaging observations of TR from IRIS reveal the ubiquitous presence of network jets. We have used three different IRIS observations of the quiet sun, which are located near the disk center. On the basis of careful inspection, 51 network jets are identified from three QS observations and used for fur... | [
"Narang et al. 2016"
] | [
"However, the mean length for QS network jets is smaller (3.53 Mm;"
] | [
"Compare/Contrast"
] | [
[
1539,
1557
]
] | [
[
1473,
1538
]
] |
2016ApJ...819...23S__Kendall_et_al._1992_Instance_1 | Single-photon VUV excitation from the N2(X1
) ground state can only populate the ungerade states. Many of these ungerade states can be coupled by spin–orbit or vibronic interactions. Hence, only the ungerade states of N2 are calculated and presented. Because of the potential diffuse nature of the excited states, t... | [
"Kendall et al. 1992"
] | [
"Because of the potential diffuse nature of the excited states, their wavefunctions were calculated using a large basis set composed by the aug-cc-pVQZ quality, which is augmented by 3s and 2p diffuse Gaussian-type orbitals (GTOs;"
] | [
"Uses"
] | [
[
500,
519
]
] | [
[
256,
485
]
] |
2018AandA...619A..13V__Saviane_et_al._2012_Instance_3 | The EWs were measured with the methods described in Vásquez et al. (2015). As in Paper I, we used the sum of the EWs of the two strongest CaT lines (λ8542, λ8662) as a metallicity estimator, following the Ca II triplet method of Armandroff & Da Costa (1991). Different functions have been tested in the literature to mea... | [
"Saviane et al. (2012)"
] | [
"Figure 5 shows the comparison between our EWs measurements and the line strengths measured by",
"(in both cases the sum of the two strongest lines) for the five calibration clusters.",
"The observed scatter is consistent with the internal errors of the EW measurements,"
] | [
"Compare/Contrast",
"Compare/Contrast",
"Similarities"
] | [
[
1530,
1551
]
] | [
[
1436,
1529
],
[
1552,
1637
],
[
1638,
1721
]
] |
2020MNRAS.496.3448D__Joy,_Sahni_&_Starobinsky_2008_Instance_1 | The aforementioned form of power-law primordial power spectrum is a prediction of inflation where the scalar field (inflaton) slowly rolls down to the bottom of the flat inflationary potential. With the constraints on the tilt and an upper bound on the amplitude of tensor perturbation with respect to scalar perturbatio... | [
"Joy, Sahni & Starobinsky 2008"
] | [
"Note that any changes in the nearly flat potential will eventually lead to certain features in the spectrum. Local glitches in the potential including rapid change of its amplitude, or the break in its first or second derivatives",
"all lead to local and non-local oscillations in the spectrum."
] | [
"Motivation",
"Motivation"
] | [
[
824,
853
]
] | [
[
506,
735
],
[
1524,
1585
]
] |
2021ApJ...908...95H__Goto_et_al._2011_Instance_1 | Star-forming galaxies at redshifts z ∼ 1–3 probe the cosmic epoch when most of the stellar mass assembly in the universe took place (Madau & Dickinson 2014, and references therein). A better understanding of star formation (SF) during this epoch is therefore imperative to understand SF across cosmic time. Locally, less... | [
"Goto et al. 2011"
] | [
"Locally, less than 5% of the galaxy population has a star formation rate (SFR) that is significantly higher than the empirical main sequence for star-forming galaxies, i.e., the tight correlation (∼0.3 dex) between the SFR and stellar mass, M⋆"
] | [
"Background"
] | [
[
621,
637
]
] | [
[
307,
550
]
] |
2015MNRAS.450...53H__Muñoz_et_al._2014_Instance_2 | Using moving meshes helps reduce the angular momentum errors from advection in grid codes. We have run >200 iterations of this test problem using the public version of fvmhd3d, systematically varying choices like the mesh regularization scheme, mesh ‘drifting’ (whether to use a strictly Lagrangian drift, or locally smo... | [
"Muñoz et al. 2014"
] | [
"In a shearing disc, if the cells adapt in a truly Lagrangian manner, then they are inevitably deformed into a highly sheared/irregular shape"
] | [
"Compare/Contrast"
] | [
[
1198,
1215
]
] | [
[
1056,
1196
]
] |
2015MNRAS.450..630S__Moore_et_al._1996_Instance_1 | While there are increasing efforts to try to explain the SFR dependence on the environment, by conducting surveys at high redshift (e.g. Hayashi et al. 2010; Matsuda et al. 2011; Sobral et al. 2011; Muzzin et al. 2012; Koyama et al. 2013; Darvish et al. 2014; Tal et al. 2014), so far such studies have not been able to ... | [
"Moore et al. 1996"
] | [
"Several strong processes have been proposed and observed, such as harassment (e.g."
] | [
"Background"
] | [
[
561,
578
]
] | [
[
478,
560
]
] |
2018AandA...618A..67C__Moriguchi_et_al._(2002)_Instance_2 | The close proximity in the sky of M 16 and M 17, two of the nearest giant HII regions of our galactic neighborhood lying at a similar distance from the Sun, naturally leads to the question of whether they are physically related, and whether they may share a common origin (Moriguchi et al. 2002; Oliveira 2008; Nishimura... | [
"Moriguchi et al. (2002)",
"Moriguchi et al. (2002)"
] | [
"Both giant HII regions are projected on the contour of a giant bubble-shaped structure, outlined in the distribution of HI and CO emission as first noted by",
"noted the presence of O and early B stars in the area and proposed that they were part of a massive star population responsible for having caused the bub... | [
"Background",
"Compare/Contrast"
] | [
[
492,
515
],
[
1670,
1693
]
] | [
[
335,
491
],
[
1694,
2049
]
] |
2017AandA...606A..17M__Kennicutt_(1998)_Instance_2 | The SFR reported in Table C.1 refers to a stellar mass range from Mlow = 0.1M⊙ to Mup = 100M⊙, is averaged over the past Δt = 100 Myr, and was calculated using the standard SFR(LIR) relationship from Kennicutt (1998; here scaled to a Chabrier 2003, IMF) (1)\begin{equation} \label{eq:sfr} \textit{SFR}=10^{-10}\times L_{... | [
"Kennicutt (1998)"
] | [
"If the cirrus ISM component heated by the more general galactic UV radiation field contributes to LIR, then the",
"relationship overestimates the SFR."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1112,
1128
]
] | [
[
1000,
1111
],
[
1129,
1164
]
] |
2018MNRAS.480.4931V__Dokkum_2001_Instance_1 | We made use of the SALT product data generated by the in-house pipeline called PySALT (Crawford et al. 2010), which mosaics the individual CCD data to a single FITS file, corrects for cross-talk effects, and performs bias and gain corrections. We then carried out further reduction steps using our own custom tools, writ... | [
"van Dokkum 2001"
] | [
"We then remove the cosmic rays using the LACosmic algorithm"
] | [
"Uses"
] | [
[
1530,
1545
]
] | [
[
1469,
1528
]
] |
2021MNRAS.500.2336Y__Lin_et_al._2020_Instance_1 | Various surveys of SNRs in our Galaxy and nearby galaxies have been carried out at radio, X-ray, Infrared (IR), and optical wavelengths. The first extragalactic SNR candidates were identified in the LMC by Mathewson & Healey (1964) and later confirmed with a combination of radio and optical techniques by Westerlund & M... | [
"Lin et al. 2020"
] | [
"However, sensitivity and resolution limitations severely reduce the effectiveness of the past and present generations of radio and X-ray searches for SNRs in galaxies beyond the Small and Large Magellanic Clouds (MCs)"
] | [
"Background"
] | [
[
900,
915
]
] | [
[
502,
719
]
] |
2018ApJ...856..136P__Burkhart_et_al._2010_Instance_2 | Depending on the specific driver, the characteristics of turbulence will then be imprinted within the ISM mainly as three-dimensional density and velocity fluctuations, and these fluctuations have been traditionally studied via correlation functions such as the spatial power spectrum (SPS) (e.g., Crovisier & Dickey 198... | [
"Burkhart et al. 2010"
] | [
"These slopes essentially provide information on the relative amount of structure as a function of spatial scale and can be compared with theoretical models of turbulence (mainly numerical simulations) to characterize turbulence cascade (e.g.,"
] | [
"Background"
] | [
[
1089,
1109
]
] | [
[
846,
1088
]
] |
2018AandA...617A..86L__Tian_2017_Instance_2 | The IRIS spectra measure the flare in a “sit-and-stare” mode with a roll angle of 45∘. The spectral scale is ∼25.6 mÅ per pixel in the far-ultraviolet (FUV) wavelengths. The IRIS slit crosses the flaring loop and one ribbon (Fig. 1). Two red bars enclose the flaring loop region used to study the quasi-periodic oscillat... | [
"Tian 2017"
] | [
"Two orange peaks represent the cool lines of O I 1354.60 Å and C I 1354.84 Å",
"which are far away from the flaring line of Fe XXI 1354.08 Å."
] | [
"Uses",
"Uses"
] | [
[
1978,
1987
]
] | [
[
1900,
1976
],
[
1990,
2051
]
] |
2016MNRAS.461.1719C__Harris_et_al._2012_Instance_1 | HATLAS12-00 had already been identified as a candidate gravitationally lensed galaxy as a result of its high submm flux (i.e. F500 > 100 mJy), red Herschel colours and the lack of a bright optical or radio counterpart (see e.g. Negrello et al. 2010 for a discussion of the selection of lens candidates in H-ATLAS and oth... | [
"Harris et al. 2012"
] | [
"A CO spectroscopic redshift of 3.26 was first suggested by Z-spec",
"observations, then subsequently confirmed by observations",
"and the Zpectrometer instrument",
"on the Greenbank Telescope"
] | [
"Similarities",
"Similarities",
"Similarities",
"Similarities"
] | [
[
696,
714
]
] | [
[
409,
474
],
[
498,
555
],
[
615,
646
],
[
668,
694
]
] |
2022MNRAS.513.3458B__Robertson_et_al._2019_Instance_1 | Among the most viable mechanisms of cusp-core transformation that require changes to the assumed cosmogony is one that was proposed specifically as a possible solution to the cusp-core problem. It proposes that the DM is in fact not collisionless but self-interacting (SIDM; Spergel & Steinhardt 2000; Yoshida et al. 200... | [
"Robertson et al. 2019"
] | [
"The most stringent and precise constraints on the self-interaction cross-section have been put on the scales of galaxy clusters (e.g.",
"where observations require that $\\sigma _T/m_chi \\lesssim 1\\, {\\rm cm^2g^{-1}}$."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1630,
1651
]
] | [
[
1466,
1599
],
[
1704,
1784
]
] |
2022AandA...666A.107S__BeyondPlanck_2022_Instance_1 | While new data will refine our understanding of the interplanetary medium, it is necessary for future models to be consistent with both new and archival data. It is precisely this need that motivates the COSMOGLOBE project1, which aims to create a framework that will allow for the refinement of astrophysical models joi... | [
"BeyondPlanck 2022"
] | [
"This form of joint analysis is already being explored within the framework of WMAP",
"and LiteBIRD",
"in combination with Planck Low Frequency Instrument data"
] | [
"Background",
"Background",
"Background"
] | [
[
577,
594
]
] | [
[
375,
457
],
[
478,
490
],
[
519,
575
]
] |
2017AandA...599A..97H__Carretta_et_al._2009b_Instance_1 | Amongst the oldest stellar systems known to exist in the Milky Way (MW) are metal-poor globular clusters (GCs). These accumulations of stars do not seem to have undergone substantial star formation for extended periods. Given the limited quality of the available data, for a long time color-magnitude diagrams (CMDs) of ... | [
"Carretta et al. 2009b"
] | [
"Moreover, in recent years evidence has grown supporting the statement that GCs are generally composed of two or three chemically distinct populations. These subpopulations are separated by a few tens to hundreds of Myr in age and show vastly varying abundances of light elements such as C, N, O, Na, Mg, and Al (see... | [
"Background"
] | [
[
1319,
1340
]
] | [
[
996,
1318
]
] |
2021MNRAS.500.2336Y___2018_Instance_1 | Various surveys of SNRs in our Galaxy and nearby galaxies have been carried out at radio, X-ray, Infrared (IR), and optical wavelengths. The first extragalactic SNR candidates were identified in the LMC by Mathewson & Healey (1964) and later confirmed with a combination of radio and optical techniques by Westerlund & M... | [
"Vučetić et al.",
"2018"
] | [
"Optical extragalactic searches for SNRs are mainly done by using an emission line ratio criterion of the form [S ii]/H α > 0.4–0.5"
] | [
"Background"
] | [
[
1324,
1338
],
[
1349,
1353
]
] | [
[
1041,
1171
]
] |
2020ApJ...891...10L__Song_et_al._2009_Instance_1 | We need to build data sets to train and evaluate the model. Then the data sets are prepared in the following way: (1) if the AR does not flare within 24 hr after the observation time, the No-flare (weaker than C1.0) label is assigned to the magnetogram sample in the same AR. (2) If the C/M/X-level flare occurs within 2... | [
"Song et al. 2009"
] | [
"We adopt a four-level AR classification scheme based on the maximum GOES-level flare an AR ever yields"
] | [
"Uses"
] | [
[
976,
992
]
] | [
[
872,
974
]
] |
2021MNRAS.506.1962S__Nordlander_&_Lind_2017_Instance_1 | Among the odd Z elements, we derived the abundances of Na, Al, K, and Sc using the high-resolution spectra and the details of the lines are given in Table A1. The Na D lines were not used as the lines are too strong for deriving the abundances. So, we depended on the weaker lines 5682 Å and 5688 Å to derive the Na abun... | [
"Nordlander & Lind 2017"
] | [
"Al i lines at 6696 and 6698 are used for deriving the Al abundance and these lines have negligible contributions from NLTE effects"
] | [
"Uses"
] | [
[
631,
653
]
] | [
[
473,
603
]
] |
2015AandA...584A..75V__Essen_et_al._(2014)_Instance_4 | The data presented here comprise quasi-simultaneous observations during secondary eclipse of WASP-33 b around the V and Y bands. The predicted planet-star flux ratio in the V-band is 0.2 ppt, four times lower than the accuracy of our measurements. Therefore, we can neglect the planet imprint and use this band to measur... | [
"von Essen et al. (2014)"
] | [
"As pointed out in",
"we found clear evidences of pulsation phase variability with a maximum change of 2 × 10-3 c/d. In other words, as an example after one year time a phase-constant model would appear to have the correct shape with respect to the pulsation pattern of the star, but shifted several minutes in tim... | [
"Similarities",
"Similarities"
] | [
[
1114,
1137
]
] | [
[
1096,
1113
],
[
1139,
1433
]
] |
2016MNRAS.460.3472E__Ercolano_et_al._2008a_Instance_1 | We use the set of wind solutions (density and velocity distribution of gas in the wind) for primordial discs (i.e. gas-rich, optically thick discs, which do not have an evacuated inner cavity) calculated by Owen et al. (2010, 2011) and EO10 for a 0.7 M⊙ star and X-ray luminosities (0.1 ≤ hν ≤ 10 keV) of LX = 2 × 1028, ... | [
"Ercolano et al. 2008a"
] | [
"The dust radiative transfer and photosionisation code mocassin",
"was used produce the temperature parametrization. The atomic data base of the mocassin code included opacity data from Verner et al. (1993) and Verner & Yakovlev (1995), energy levels, collision strengths and transition probabilities from Version ... | [
"Uses",
"Uses"
] | [
[
783,
804
]
] | [
[
665,
727
],
[
854,
1262
]
] |
2019MNRAS.487.1626Q__Merloni,_Fabian_&_Ross_2000_Instance_1 | Low-mass X-ray binaries (LMXBs) which either contain a black hole (BH) or a neutron star (NS), accreting matter from its low-mass companion star (≲1M⊙) are ideal natural laboratories for studying the physics of accretion and jet around a BH or an NS (e.g. Migliari & Fender 2006). According to the timing and spectral fe... | [
"Merloni, Fabian & Ross 2000"
] | [
"For BH-LMXBs",
"and the X-ray spectrum can be well described by a multicolour blackbody spectrum (e.g."
] | [
"Background",
"Background"
] | [
[
809,
836
]
] | [
[
482,
494
],
[
678,
764
]
] |
2019AandA...625A.121M__Beaugé_&_Nesvorný_2012_Instance_1 | The final location of close-in giant planets in our models reflects the strength of the tides that we include in our modeling, which play a very important role in the decay of planetary orbits. These are dynamical tides (e.g., Lai 1997; Ivanov & Papaloizou 2004, 2007, 2011) and in our simulations we used a formulation ... | [
"Beaugé & Nesvorný 2012"
] | [
"Equilibrium tides become then effective (e.g.,",
"and references therein) and the tidal evolution may occur on a longer timescale."
] | [
"Uses",
"Uses"
] | [
[
626,
648
]
] | [
[
579,
625
],
[
649,
729
]
] |
2021MNRAS.508.4332M__Sickafoose_et_al._2001_Instance_1 | As a first step, we need to specify the photoelectron sheath features. In this course, we first evaluate the steady state potential over the lunar surface (equation 4), and then after, we use this as a boundary condition to solve the Poisson equation (equation 2) and estimate the photoelectron sheath profile. In calcul... | [
"Sickafoose et al. 2001"
] | [
"For instance, for the Lyman α radiation χνr = 0.042 for optimum efficiency χo = 0.1"
] | [
"Uses"
] | [
[
1046,
1068
]
] | [
[
961,
1044
]
] |
2019ApJ...883..130L__Hansen_2009_Instance_1 | (3) What is the likelihood of obtaining Mercury and Mars analogs in systems with Venus–Earth pair analogs? Recent terrestrial planet formation studies managed to statistically produce low-mass Mars analogs. In particular, there are currently five main competing models. (1) Grand Tack: the protoplanetary disk is truncat... | [
"Hansen 2009"
] | [
"In particular, there are currently five main competing models.",
"(2) Empty Asteroid Belt: embryos and planetesimals in the protoplanetary disk formed concentrated within a narrow belt at ∼0.7–1 au"
] | [
"Background",
"Background"
] | [
[
772,
783
]
] | [
[
207,
269
],
[
639,
770
]
] |
2017AandA...605A.121M__Thompson_et_al._2017_Instance_1 | The effects of the wet air, the variable water vapour cells, are the main cause of the refraction at submillimetre/millimetre wavelengths. The dipole moment of water makes water vapour, the wet component in the troposphere, a strong absorber at submillimetre/millimetre wavelengths and significantly increases the refrac... | [
"Thompson et al. 2017"
] | [
"In what is called the “frozen-screen” hypothesis",
"these pockets, or turbulent eddies, are assumed to be fixed in the atmospheric layer that advects over an interferometric array"
] | [
"Background",
"Background"
] | [
[
649,
669
]
] | [
[
456,
504
],
[
520,
647
]
] |
2021AandA...653A.154T__VI_2020_Instance_1 | The global volume-weighted neutral fraction of hydrogen QH I in the high-resolution volume is presented as the thick blue line in Fig. 10. The reionization process starts when the first stars are born, and by z50 ≃ 7.63, half of the volume is reionized. We identify the redshifts at which 1%, 10%, 50%, 90% and 99% of th... | [
"Planck Collaboration VI 2020"
] | [
"The dark and light shaded areas in Fig. 10 correspond to the 1σ and 2σ constraints on the redshift of reionization from the cosmic microwave background measurements of the Planck mission",
"with a reionization midpoint zre = 7.67 ± 0.73."
] | [
"Uses",
"Uses"
] | [
[
752,
780
]
] | [
[
564,
750
],
[
783,
830
]
] |
2022AandA...666L...5G__Esparza-Arredondo_et_al._2018_Instance_1 | More recently, García-Bernete et al. (2022) found that the PAH molecules responsible for the 11.3 μm PAH emission band are more resilient in the hard environments often present in AGN. In particular, the authors found larger 11.3/7.7 μm and 11.3/6.2 μm PAH ratios in AGN-dominated systems compared to SF galaxies, indica... | [
"Esparza-Arredondo et al. 2018"
] | [
"Previous sub-arcsecond angular resolution N-band (∼8–13 μm) ground-based spectroscopic studies investigated the 11.3 μm PAH feature in the nuclear and circumnuclear regions of AGN",
"However, these works were unable to provide definitive details regarding the effect of the AGN on the PAH molecules due to limited... | [
"Background",
"Motivation"
] | [
[
948,
977
]
] | [
[
592,
771
],
[
980,
1147
]
] |
2021AandA...654A..80S__Urrutia_et_al._2019_Instance_1 | In this study we are focusing on rest-frame UV emission red-wards of the strongest UV emission line, Lyα, partially motivated by the challenges of observing this line at high redshift (z ≳ 6) where the significantly neutral CGM and IGM absorbs the Lyα photons escaping the galaxy along the line of sight (e.g., Dijkstra ... | [
"Urrutia et al. 2019"
] | [
"In particular, the asymmetric Lyα line profile has enabled redshift confirmations of large samples of sources at both 2 z 6 (e.g.,"
] | [
"Background"
] | [
[
706,
725
]
] | [
[
491,
623
]
] |
2022ApJ...938..124Z__Tu_&_Marsch_1995_Instance_1 | In the context of solar wind turbulence, one crucial question concerns turbulence evolution and heating (Parashar et al. 2015; Chen 2016; Viall & Borovsky 2020). Numerous correlations exist between solar wind parameters and magnetic fluctuations, which can provide important indications and constraints on the physics of... | [
"Tu & Marsch 1995"
] | [
"The faster solar wind tends to be more imbalanced with greater wave energy flux antisunward than sunward"
] | [
"Background"
] | [
[
618,
634
]
] | [
[
512,
616
]
] |
2022ApJ...940....5D__Bálazs_et_al._2003_Instance_1 | Figure 1 shows the best fits of a multiple-Gaussian model to the T
90 distributions of distinct Swift/BAT GRB samples. Interestingly, we find from Figures 1(a)–(d) that the lognormal T
90 durations of all Swift GRBs except those with good spectra in sample V are triply distributed. It is confirmed in Figure 1(e) that t... | [
"Bálazs et al. 2003"
] | [
"In addition, another classification scheme uses a scatter plot of flux and duration fitted with two-dimensional Gaussian functions"
] | [
"Compare/Contrast"
] | [
[
873,
891
]
] | [
[
741,
871
]
] |
2020MNRAS.495.4508E__Heinke_et_al._2014_Instance_3 | Several qLMXBs have been identified in GCs and in the Galactic field (for some examples, see table 4 in Guillot et al. 2009 and references therein). While LMXBs in the field were detected following the onset of a bright accretion outburst, most qLMXBs in GCs, including all those with the highest flux at Earth, have not... | [
"Heinke et al. 2014"
] | [
"Since NS He-atmosphere models have harder spectra than H-atmosphere models, using the incorrect composition for the observed thermal emission can result in biases of the inferred radii"
] | [
"Uses"
] | [
[
1994,
2012
]
] | [
[
1785,
1969
]
] |
2022ApJ...924...56S__Schreiber_et_al._2015_Instance_1 | The second ingredient is the probability distribution of stellar mass at given SFR and redshift:
5
dpdlogM⋆(M⋆∣ψ,z)∝M⋆M⋆M⋆,MS(ψ,z)M⋆,MSexp−logM⋆−logM⋆,MSψ,z22σlogM⋆2M⋆≥M⋆,MS(ψ,z),
where M
⋆,MS(ψ, z) is the observed redshift-dependent galaxy main sequence with log-normal scatter
σlogM⋆≈0.2
dex (we adopt the de... | [
"Schreiber et al. 2015"
] | [
"The main sequence is a relationship between SFR and stellar mass followed by the majority of star-forming galaxies, apart from some outliers located above the average SFR at given stellar mass"
] | [
"Background"
] | [
[
712,
733
]
] | [
[
401,
593
]
] |
2018ApJ...853..148C__Shibuya_et_al._2014_Instance_2 | LAE galaxies are defined by a high equivalent width (EW > 20 Å) Lyα line and are believed to be composed of extremely large regions of active star formation. Many efforts have been made to detect and characterize LAE galaxies (e.g., Conselice et al. 2003; Conselice 2004; Ravindranath et al. 2006; Shimasaku et al. 2006;... | [
"Shibuya et al. 2014"
] | [
"As a result, direct imaging studies cannot decisively determine whether the clumps are different in nature from star-forming regions in our local universe or if the larger apparent size is merely an artifact of insufficient resolution"
] | [
"Background"
] | [
[
2420,
2439
]
] | [
[
2184,
2418
]
] |
2020ApJ...895L...8R__Kapferer_et_al._2009_Instance_1 | As clusters of galaxies assemble, they dynamically transform the physical properties of in-falling cluster members. Galaxies falling into a cluster experience ram pressure from dense intracluster medium (ICM) gas that can potentially unbind their individual gas reservoirs (Gunn et al. 1972). This process referred to as... | [
"Kapferer et al. 2009"
] | [
"Prior to complete gas removal, moderate values of ram pressure have also been shown to increase the star formation rate in galaxies both observed",
"and simulated"
] | [
"Background",
"Background"
] | [
[
1117,
1137
]
] | [
[
867,
1012
],
[
1078,
1091
]
] |
2016MNRAS.461.3982B__Walsh_&_Richardson_2008_Instance_1 | Many studies have been done to understand the dynamics and origin of such systems since the discovery of the first binary asteroid system, Dactyl orbiting around (243) Ida in 1993 (Chapman et al. 1995). Based on the structure of ‘rubble pile’ asteroids (a collection of gravitationally bound boulders with a distribution... | [
"Walsh & Richardson 2008"
] | [
"However, close encounters with the planets proved not to be enough for creation of the current population of binary systems"
] | [
"Background"
] | [
[
609,
632
]
] | [
[
464,
587
]
] |
2020MNRAS.496.5528M__Greif_et_al._2012_Instance_1 |
Theoretically predicted magnetic field in the formation of the first stars. The evolution of a dynamo in a collapsing minihalo depends on a large number of parameters: the initial density, nH,0, the turbulent velocity, vt (which we parametrize in terms of the virial velocity, vt = ϕtvvir), the temperature, T, the mass... | [
"Greif et al. 2012"
] | [
"Choosing values of these parameters that are consistent with simulations (e.g. those of"
] | [
"Uses"
] | [
[
730,
747
]
] | [
[
642,
729
]
] |
2021ApJ...913L..14H__Priest_&_Schrijver_2000_Instance_1 | Thanks to the observations with high time resolution and high optical sensitivity from state-of-the-art facilities, various dynamic phenomena, and processes (e.g., magnetic reconnections, jet flows, and oscillatory waves) have been observed to be omnipresent in the multi-layers of solar atmosphere (Shibata et al. 2007;... | [
"Priest & Schrijver 2000"
] | [
"Magnetic reconnection rapidly converts magnetic energy to particle energy, causing emission flare in multiple wave bands and even triggering coronal mass ejections"
] | [
"Background"
] | [
[
801,
824
]
] | [
[
636,
799
]
] |
2018AandA...616A..99K__Narang_et_al._2016_Instance_3 | The high-resolution imaging observations of TR from IRIS reveal the ubiquitous presence of network jets. We have used three different IRIS observations of the quiet sun, which are located near the disk center. On the basis of careful inspection, 51 network jets are identified from three QS observations and used for fur... | [
"Narang et al. (2016)"
] | [
"So, the mean length for QS network jets from the present work is in good agreement with"
] | [
"Similarities"
] | [
[
1648,
1668
]
] | [
[
1560,
1647
]
] |
2022AandA...666A..51M__Djurašević_1993_Instance_1 | RX Cas is part of a group of interacting binaries showing light curves similar to β Lyrae and showing a long photometric cycle of unknown origin (Mennickent 2017). Few of these interacting binaries have been studied in terms of their physical changes during the long cycle. Here we provide a brief comparison with some o... | [
"Djurašević 1993"
] | [
"We note that a hotter disk during maximum was predicted by a simpler study in the past"
] | [
"Similarities"
] | [
[
769,
784
]
] | [
[
681,
767
]
] |
2018MNRAS.476.2591V__Nikolic,_Cullen_&_Alexander_2004_Instance_1 | Galaxy interactions represent a fundamental component of our current view of hierarchical galaxy evolution. Studies based on both observations and simulations have shown that galaxy collisions and mergers can dramatically affect the galaxies undergoing the interaction, by, e.g. triggering nuclear activity (e.g. Kennicu... | [
"Nikolic, Cullen & Alexander 2004"
] | [
"The most evident effect driven by galaxy encounters is probably the triggering of new episodes of star formation, which can occur both in the pre-merger regime between first pericentre and coalescence (e.g."
] | [
"Background"
] | [
[
957,
989
]
] | [
[
750,
956
]
] |
2022MNRAS.516.3532M__Johnson_et_al._2017_Instance_1 | The size–SFR relation has been already well-defined in the local Universe investigating H ii regions in nearby spiral and irregular galaxies by Kennicutt (1988). On the other hand, outliers are mainly hosted by interacting systems as shown in the case of the Antennae galaxy (Bastian et al. 2006), and have been thorough... | [
"Johnson et al. 2017",
"Johnson et al. 2017"
] | [
"In Fig. 10, we show the relation between the size and star formation rate of clumps, including samples across different redshifts",
"Our sample",
"despite being at z ∼ 2–6, have sizes comparable to local H ii regions and GCs",
"but they have SFRs ∼300 times higher."
] | [
"Uses",
"Similarities",
"Similarities",
"Differences"
] | [
[
625,
644
],
[
992,
1011
]
] | [
[
418,
547
],
[
789,
799
],
[
849,
926
],
[
1014,
1051
]
] |
2019AandA...627A.172R__Rozitis_&_Green_(2013)_Instance_3 | For comparisons with the light curve YORP constraints, the YORP effect acting on Cuyo could be predicted by computing the total recoil forces and torques from reflected and thermally emitted photons from the asteroid surface using the ATPM. These calculations were made for both a smooth and rough surface, and were aver... | [
"Rozitis & Green (2013)"
] | [
"However, a study of non-convex shape models for fast two to four hour rotators in",
"indicated that such asteroids have rather minimal levels of global-scale concavities, and the ~ 2.7 h rotation period of Cuyo implies that its shape could be similar."
] | [
"Similarities",
"Similarities"
] | [
[
1004,
1026
]
] | [
[
922,
1003
],
[
1027,
1193
]
] |
2017AandA...604A..53C__Bolatto_et_al._(2013)_Instance_1 | The reasons for such a tight – and linear – correlation between \hbox{$L^{\prime}_{\rm CO(1{-}0)}$}LCO(1−0)′ and M∗ (or LK) observed consistently across different galaxy samples except in early type galaxies have been little explored in the literature. The interpretation favoured by Leroy et al. (2005) is that CO emiss... | [
"Bolatto et al. (2013)"
] | [
"An alternative explanation that we propose here goes back to the nature of the optically thick 12CO emission and to the approximately linear relation between 12CO luminosity and virial mass found for GMCs (see e.g.",
"for a more recent compilation"
] | [
"Uses",
"Uses"
] | [
[
766,
787
]
] | [
[
500,
714
],
[
788,
817
]
] |
2020AandA...638A..44B__Jiménez-Serra_et_al._2010_Instance_1 | Combining these different velocity signatures, the data show strong signatures of two gas components at different velocities (around 6 km s−1 apart) that converge to a common intermediate velocity at the location of the infrared dark cloud and active star-formingregion, similar to filament formation via gravitationally... | [
"Jiménez-Serra et al. 2010"
] | [
"Similar signatures were also reported in observations (e.g.,"
] | [
"Similarities"
] | [
[
928,
953
]
] | [
[
867,
927
]
] |
2021MNRAS.508..637S__Johnston_et_al._2019_Instance_1 | We also present the correlation functions of centrals and satellites in Fig. 17. This is a worthwhile exercise for a variety of reasons, not least that there is information on the small-scale IA signal missed in the large-scale fits. While we cannot, at the present time, fit the IA signal on scales ∼1 h−1 Mpc, the qual... | [
"Johnston et al. 2019"
] | [
"For reference, the dark red crosses also show the equivalent satellite/central red galaxy wg + correlations from KiDS×GAMA here (c.f.",
"fig. 7, red points/band).",
"On large scales at least, our illustristng red sample is consistent with their measurements.",
"There are a few interesting features here to no... | [
"Uses",
"Uses",
"Similarities",
"Compare/Contrast",
"Similarities",
"Differences",
"Compare/Contrast"
] | [
[
1129,
1149
]
] | [
[
995,
1128
],
[
1150,
1175
],
[
1176,
1268
],
[
1269,
1328
],
[
1411,
1459
],
[
1460,
1595
],
[
1596,
1784
]
] |
2021MNRAS.508..637S__Chang_et_al._2019_Instance_1 | It is now well established that the weak lensing of distant galaxies by foreground mass provides a relatively clear window on to the large-scale structure of the Universe. This is true whether that foreground mass is in the form of discrete matter concentrations, as traced by galaxies (i.e. galaxy–galaxy lensing; Mande... | [
"Chang et al. 2019"
] | [
"It is now well established that the weak lensing of distant galaxies by foreground mass provides a relatively clear window on to the large-scale structure of the Universe. This is true whether that foreground mass is in the form",
"or the continuous large-scale matter distribution (cosmic shear;"
] | [
"Background",
"Background"
] | [
[
673,
690
]
] | [
[
0,
228
],
[
528,
592
]
] |
2019MNRAS.488.5029H__Stacey_et_al._2010_Instance_2 | For the first time, we detected [C ii] 158-μm emission from a GRB host galaxy at z > 2. This is the second detection of [C ii] 158-μm emission among known GRB host galaxies, following GRB 980425 (Michałowski et al. 2016). The [C ii] 158-μm fine structure line is the dominant cooling line of the cool interstellar medium... | [
"Stacey et al. 2010"
] | [
"The [C ii] deficit persists when including high-z galaxies (e.g."
] | [
"Motivation"
] | [
[
1105,
1123
]
] | [
[
1040,
1104
]
] |
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