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 |
|---|---|---|---|---|---|---|
2021AandA...652A.114P__Nakariakov_&_Verwichte_2005_Instance_1 | Multiple solar missions, such as the Solar Dynamics Observatory (SDO) and the Interface Region Imaging Spectrograph (IRIS), have shown that a diversity of waves occur in the solar atmosphere (Jess et al. 2009; McIntosh et al. 2011; Okamoto & De Pontieu 2011). The various wave types that occur include Alfvén waves (Alfv... | [
"Nakariakov & Verwichte 2005"
] | [
"As they pass by, they modify the transverse magnetic field and velocity components but, do not alter the gas pressure or the mass density",
"at least in the linear limit and in a homogeneous background plasma."
] | [
"Background",
"Background"
] | [
[
699,
726
]
] | [
[
560,
697
],
[
729,
797
]
] |
2021MNRAS.504.5840F__Eriksen_et_al._2007_Instance_2 | The standard cosmological model stands on the shoulders of a fundamental assumption: that the universe is statistically homogeneous and isotropic on the largest scales. This assumption has been thoroughly tested over the last years both with cosmic microwave background (CMB) and Large-scale structure data. In particula... | [
"Eriksen et al. 2007"
] | [
"Power asymmetry from CMB data has also been a matter of intense debate and scrutiny"
] | [
"Background"
] | [
[
1193,
1212
]
] | [
[
1072,
1155
]
] |
2020ApJ...899..147F__Hörst_et_al._2018_Instance_1 | Recent observations of transit spectra of hot Jupiter atmospheres show limited spectral modulation due to H2O that has been largely interpreted as the indicator of the presence of aerosols (Barstow et al. 2016; Iyer et al. 2016; Sing et al. 2016; Pinhas et al. 2019). Whether these aerosols are condensate clouds of phot... | [
"Hörst et al. 2018"
] | [
"Although thermochemical equilibrium models predict the formation of condensate clouds with various composition in these hot atmospheres",
"recent laboratory works highlighted that photochemistry could strongly affect the composition of exoplanet atmospheres and lead to the formation of aerosols in a variety of c... | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
841,
858
]
] | [
[
394,
529
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[
608,
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2020MNRAS.494.5134L__Taylor_1922_Instance_1 | The gas velocity is unknown since no exact analytic solution for turbulence in a disc – and turbulence in general – are known. However, statistical properties of turbulence can be inferred from laboratory, numerical experiment or theory, and turbulent fluctuations can be modelled using stochastic processes, independent... | [
"Taylor 1922"
] | [
"Equation (16) describes turbulent fluctuations from a Lagrangian point of view"
] | [
"Uses"
] | [
[
1297,
1308
]
] | [
[
1217,
1295
]
] |
2019ApJ...871...86K__Friesen_et_al._2014_Instance_1 | On the basis of the 1.3 mm continuum image made from the SMA archival data, Nakamura et al. (2012) found conspicuous substructures inside a prestellar core in the Oph B2 region, which had been previously identified as a single core (B2-N5) in single-dish molecular line (N2H+ (J = 1−0)) observations (Friesen et al. 2010... | [
"Friesen et al. 2014)"
] | [
"Similarly, Kamazaki et al. (2001) found small condensations of 1000 au scale inside the SM1 core in the Oph A region based on 3 mm dust continuum observations with the Nobeyama Millimeter Array (see also",
"The masses of the condensations are around 0.01−0.1 M⊙, comparable to or larger than the local Jeans mass.... | [
"Background",
"Background"
] | [
[
858,
878
]
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[
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[
880,
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2021MNRAS.501.2522J__Mukherjee_&_Paul_2004_Instance_2 | GX 301-2 is an HMXB consisting of a highly magnetized (B ∼ 4 × 1012 G, or even larger Doroshenko et al. 2010) pulsar and a B-type hyper-giant star Wray 977 (Vidal 1973; Kaper et al. 1995; Staubert et al. 2019). According to modelling of high-resolution optical spectra, Wray 977 has a mass of 43 ± 10 $\, \mathrm{M}_{\od... | [
"Mukherjee & Paul 2004"
] | [
"The flares are accompanied by the variability of the equivalent hydrogen column density ($\\rm \\mathit{ N}_{\\rm H}$) and of the fluorescent iron lines, which is believed to be associated with clumpiness of the stellar wind, launched from the donor star"
] | [
"Background"
] | [
[
1772,
1793
]
] | [
[
1519,
1770
]
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2015ApJ...809...44Z__Jang_et_al._2014_Instance_1 | Admittedly, although the prediction success rate of SPM3 is greatly improved compared with the previous SPM2 model, its improvements in the shock TT prediction are limited. Many factors could potentially cause this. On one hand, the sample events used in this study are CMEs from Solar Cycle 23 when SOHO was the only sp... | [
"Jang et al. 2014"
] | [
"Large uncertainties in VCME restrict further improvements to the TT prediction of the shock. Possible solutions to this restriction could include adopting the CME’s radial speed, which is derived from models (such as cone models) based on single spacecraft observations"
] | [
"Compare/Contrast"
] | [
[
790,
806
]
] | [
[
519,
788
]
] |
2019MNRAS.490.5478W__Winter,_Booth_&_Clarke_2018c_Instance_1 | A growing body of work suggests that planet formation is strongly dependent on the birth environment of the host star. Stars preferentially form in groups (Lada & Lada 2003), and in sufficiently dense environments the evolution of a PPD can be significantly influenced by neighbours (de Juan Ovelar et al. 2012). Close s... | [
"Winter, Booth & Clarke 2018c"
] | [
"The influence of tidal truncation is therefore limited to stellar multiples",
"or during the decay of higher order multiplicity"
] | [
"Background",
"Background"
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[
955,
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[
764,
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[
905,
953
]
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2019MNRAS.490.5478W__Winter_et_al._2018b_Instance_3 | A growing body of work suggests that planet formation is strongly dependent on the birth environment of the host star. Stars preferentially form in groups (Lada & Lada 2003), and in sufficiently dense environments the evolution of a PPD can be significantly influenced by neighbours (de Juan Ovelar et al. 2012). Close s... | [
"Winter et al. 2018b"
] | [
"Many stars in the solar neighbourhood are born in regions where UV fields are sufficient to significantly shorten disc lifetimes"
] | [
"Background"
] | [
[
1989,
2008
]
] | [
[
1837,
1965
]
] |
2020MNRAS.494.3413T__Shidatsu_&_Done_2019_Instance_1 | The existence of winds is shown by blueshifted absorption lines from highly ionized ions. These are only seen in soft state but not in hard state (Ponti et al. 2012), anticorrelated with the radio jet which is seen in the hard state but not in the soft. This was thought to be evidence that the wind was magnetically dri... | [
"Shidatsu & Done 2019"
] | [
"However, in Tomaru et al. (2019, hereafter Paper I) we show instead that thermally driven winds can explain this switch (see also"
] | [
"Background"
] | [
[
600,
620
]
] | [
[
439,
568
]
] |
2018MNRAS.475.3419A__Davis_et_al._1999_Instance_2 | If we consider for the bulk density the value 4500 kg m−3, which is one of the highest measured in the asteroid population out of those asteroids with good quality of data (see Carry 2012), it will strengthen the hypothesis that Psyche could be an exposed metal core of a differentiated asteroid (Elkins-Tanton et al. 20... | [
"Davis et al. 1999"
] | [
"However, this may be an unlikely hypothesis, because A-type asteroids that could represent mantle material (almost pure olivine) from differentiated bodies do not exist extensively in the orbital space related to Psyche, but instead are distributed randomly in the Main Belt"
] | [
"Compare/Contrast"
] | [
[
2812,
2829
]
] | [
[
2536,
2810
]
] |
2019AandA...626A..64H__Grinberg_et_al._2017_Instance_1 | Line driven winds are not expected to be smooth flows, but show strong density perturbations or “clumps” (Owocki et al. 1988; Feldmeier et al. 1997; Puls et al. 2006, 2008; Oskinova et al. 2012; Sundqvist & Owocki 2013). In X-ray binaries, thedensity contrast could even be further enhanced by the interaction between th... | [
"Grinberg et al. 2017"
] | [
"When the line of sight to the compact object passes through one of these clumps, X-rays are absorbed by the moderately ionized material in the clump, leading to a so-called dipping event. This is also observed for other sources"
] | [
"Similarities"
] | [
[
888,
908
]
] | [
[
637,
864
]
] |
2021ApJ...906...21J__Fabian_et_al._2009_Instance_1 | Ricci et al. (2017c, hereafter R17c) recently reported on a study of the relationship between obscuration and accretion rate in a large, relatively unbiased, and complete sample of local AGNs. Specifically, they investigated 836 AGNs with a median redshift of 〈z〉 = 0.037 selected by the hard X-ray (14–195 keV) Swift Bu... | [
"Fabian et al. 2009"
] | [
"This strengthened earlier results based on smaller samples (e.g.,"
] | [
"Similarities"
] | [
[
973,
991
]
] | [
[
907,
972
]
] |
2020ApJ...901...41S__Duval_et_al._2014_Instance_1 | Observations have shown that the shape of the Lyα line is diverse. It includes broad damped absorption profiles, P-Cygni profiles, double-peak profiles, pure symmetric emission profiles, and combinations thereof (Kunth et al. 1998; Mas-Hesse et al. 2003; Shapley et al. 2003; Møller et al. 2004; Noll et al. 2004; Tapken... | [
"Duval et al. 2014"
] | [
"Later, numerical algorithms based on Monte Carlo techniques were developed to solve radiative transfer for more general cases. Now theoretical studies mostly rely on them (e.g.,"
] | [
"Background"
] | [
[
1069,
1086
]
] | [
[
640,
817
]
] |
2022ApJ...929...11M__Prasad_et_al._2017_Instance_1 | In this context, it must also be noted here that these conclusions are specific to the geometry of the GCS model, which is an idealized geometrical figure that has its limitations and constraints (see Thernisien et al. 2009). Regarding the evolution of the legs, the identification of the two separate legs of the CMEs r... | [
"Prasad et al. 2017"
] | [
"In this regard, the upcoming ADITYA-L1 mission",
"with the Visible Emission Line Coronagraph",
"will provide much better data and hence will help in arriving at much stronger conclusions on the evolution of CME legs."
] | [
"Future Work",
"Future Work",
"Future Work"
] | [
[
891,
909
]
] | [
[
731,
777
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[
802,
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[
1104,
1224
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2015AandA...584A..75V__Essen_et_al._(2014)_Instance_6 | 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)"
] | [
"We then used the phases determined in",
"during our last observing season as starting values,"
] | [
"Uses",
"Uses"
] | [
[
1684,
1707
]
] | [
[
1646,
1683
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[
1708,
1760
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] |
2016MNRAS.461..248S__Munari_et_al._2013_Instance_1 | In Sifón et al. (2013), we used the σ–M200 scaling relation of Evrard et al. (2008) to estimate dynamical masses. As discussed in Section 1, the scaling relation of Evrard et al. (2008) was calibrated from a suite of N-body simulations using DM particles to estimate velocity dispersions. However, the galaxies, from whi... | [
"Munari et al. 2013"
] | [
"Recent high-resolution hydrodynamical simulations of ‘zoomed’ cosmological haloes have shown that there is a significant difference between the velocity distributions of DM particles and galaxies themselves; whether galaxies (i.e. overdensities of stars in hydrodynamical simulations) or DM subhaloes are used makes... | [
"Compare/Contrast"
] | [
[
953,
971
]
] | [
[
604,
951
]
] |
2018ApJ...855...23I__Yang_et_al._2014_Instance_1 | Cosmic rays (CRs) represent a crucial ingredient in the dynamical and chemical evolution of interstellar clouds. Interaction of CRs with molecular clouds is accompanied by various processes generating observable radiation signatures, such as ionization of molecular hydrogen (see, e.g., Oka et al. 2005; Dalgarno 2006; I... | [
"Yang et al. 2014"
] | [
"Interaction of CRs with molecular clouds is accompanied by various processes generating observable radiation signatures, such as",
"as well as production of neutral pions whose decay generates gamma-rays in the GeV (e.g.,"
] | [
"Background",
"Background"
] | [
[
569,
585
]
] | [
[
113,
241
],
[
479,
568
]
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2015AandA...578L...8B__Berné_et_al._2009_Instance_1 | Gomez’s Hamburger (IRAS 18059-3211; hereafter GoHam) is an A star surrounded by a dusty disk. When first studied by Ruiz et al. (1987), it was classified as an evolved object (post-AGB star) on the basis of its spectral type and the presence of dust. However, all recent studies (Bujarrabal et al. 2008, 2009; Wood et al... | [
"Berné et al. 2009"
] | [
"The distance to GoHam is not known precisely, but a value d = 250 ± 50 pc is required to satisfy all the existing observational constraints",
"We here adopt this value with the uncertainty."
] | [
"Uses",
"Uses"
] | [
[
588,
605
]
] | [
[
429,
568
],
[
632,
678
]
] |
2022AandA...666A..28S__Rutherford_1903_Instance_1 | The velocity distribution of the plasma motion is shown in Fig. 12, where the magnitude is scaled with respect to the Alfvén velocity, vA, which is measured based on the magnetic field strength, B0 = 2 G, and the mass density of the equilibrium current sheet, ρc = 2.81 × 10−15 g cm−3. The Alfvén timescale is measured b... | [
"Rutherford 1903"
] | [
"Figure 13a shows that this evolution exhibits three distinct phases: (i) the early phase (between t = 0 and 250 s), where the velocity growth occurs exponentially (linearly on the logarithmic-linear scale), which is called the linear growth regime; (ii) the middle phase between t = 250 and 665 s, where the growth ... | [
"Uses",
"Uses"
] | [
[
2006,
2021
]
] | [
[
1607,
2004
],
[
2024,
2219
]
] |
2020MNRAS.495..758H__Wang_et_al._2014_Instance_1 | In all our simulations independent of the inflow Mach number, the radial velocity dispersion at the filament boundary amounts to about 0.85 times the total equilibrium velocity dispersion of the non-self-gravitational case for which a functional form can be found in the appendix. Thus, we can calculate the theoretical ... | [
"Wang et al. 2014"
] | [
"This model was successfully applied to explain several observed core distances",
"however it is not able to explain all observations"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
912,
928
]
] | [
[
551,
629
],
[
777,
827
]
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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
]
] |
2021MNRAS.507.1138M__Parfenov_&_Sobolev_2014_Instance_1 | Several mechanisms have been proposed to explain the periodicity of methanol masers. van der Walt, Goedhart & Gaylard (2009) and van der Walt (2011) proposed a colliding wind binary (CWB) system for the periodic methanol masers in G9.62+0.20E and other periodic methanol maser sources with similar light curves. Using a ... | [
"Parfenov & Sobolev 2014"
] | [
"Other mechanisms proposed are",
"spiral shocks associated with very young binary systems orbiting within a circumbinary disc"
] | [
"Background",
"Background"
] | [
[
745,
768
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] | [
[
528,
557
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[
652,
743
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2019AandA...628A.118B__Feruglio_et_al._2017_Instance_2 | Ultra-fast outflows (UFOs) of highly ionised gas observed at sub-parsec scales (Reeves et al. 2003; Tombesi et al. 2012) have been proposed as the likely origin of galaxy-wide outflows, interpreted as the result of the impact of UFOs on the ISM (King & Pounds 2015, and references therein). Furthermore, both models and ... | [
"Feruglio et al. 2017"
] | [
"Recent studies increasing the statistics of sources with detection of molecular outflows have widened the range of measured energetics (e.g."
] | [
"Background"
] | [
[
1731,
1751
]
] | [
[
1540,
1680
]
] |
2020ApJ...903L..22T__Vuitton_et_al._2007_Instance_1 | While the Loison et al. (2015) CH3C3N model corroborates the upper atmospheric abundance of C4H3N inferred by Vuitton et al. (2007) from the T5 INMS measurements (a factor of 2 higher than those derived from T40 in Vuitton et al. 2019), a large disparity between the photochemical models (and within the ensemble of mode... | [
"Vuitton et al. (2007)"
] | [
"While the Loison et al. (2015) CH3C3N model corroborates the upper atmospheric abundance of C4H3N inferred by",
"a large disparity between the photochemical models (and within the ensemble of models produced by Loison et al. 2015) arises in the lower atmosphere due to the poorly constrained C4H3N branching ratio... | [
"Similarities",
"Differences"
] | [
[
110,
131
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[
0,
109
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[
237,
508
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2020ApJ...892..110C__Saladino_et_al._2018_Instance_1 | Asymptotic-giant-branch (AGB) stars have a significantly larger size (∼1 au) than their main-sequence (MS) counterparts. They have pulsating atmospheres (Vlemmings et al. 2017; Khouri et al. 2019) and may exhibit variability with long periods ranging from 200 to 1000 days (Mowlavi et al. 2018; Karambelkar et al. 2019).... | [
"Saladino et al. 2018"
] | [
"In the case that there is an MS star close to an AGB star, a substantial fraction of the mass loss may be accreted onto the MS companion",
"As a result, the metallicity of the companion may change. Such early stage low-mass stars become chemically peculiar, and their future evolution will be strongly affected."
... | [
"Background",
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[
779,
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[
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2021AandA...647A.140C__Gianninas_et_al._2016_Instance_1 | 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"
] | [
"Even more interestingly, the detection of multi-periodic brightness variations in low-mass WDs",
"has brought about new classes of pulsating stars known as ELMVs and pre-ELMVs, respectively (ELM and pre-ELM variables, respectively)."
] | [
"Background",
"Background"
] | [
[
755,
776
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[
510,
604
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[
796,
930
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2020ApJ...892L...3A___2019e_Instance_1 | Because of its large mass, the discovery of GW190425 suggests that gravitational-wave analyses can access densities several times above nuclear saturation (see, e.g., Figure 4 in Douchin & Haensel 2001) and probe possible phase transitions inside the core of a neutron star (NS) (Oertel et al. 2017; Essick et al. 2019; ... | [
"(Abbott et al",
"2019e"
] | [
"Overall, we find that constraints on tides, radius, possible p–g instabilities",
"and the EoS from GW190425 are consistent with those obtained from GW170817"
] | [
"Similarities",
"Similarities"
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[
926,
939
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[
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[
690,
768
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[
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2016ApJ...821..107G__Schwadron_et_al._2011_Instance_3 | We repeated the plasma pressure calculation presented by Schwadron et al. (2011) and Fuselier et al. (2012) for the new ENA energy spectrum. The results for the downwind hemisphere and for the Voyager 1 region are summarized in Table 3. The measured intensity
j
ENA
of neutralized hydrogen at a given energ... | [
"Schwadron et al. 2011"
] | [
"For the density of neutral hydrogen in the inner heliosheath a constant nH = 0.1 cm−3 is assumed"
] | [
"Uses"
] | [
[
1151,
1172
]
] | [
[
1053,
1149
]
] |
2020MNRAS.497.3943M__Eckert_et_al._2012_Instance_1 | The surface brightness profile for the mosaicked image of A2199 was then extracted in concentric annuli centred at the cluster centre (RA, Dec.) = (16:28:38.21, +39:33:02.31). This corresponds to the location of the peak X-ray flux in the cluster. The radial profile of the surface brightness is shown in the upper pane... | [
"Eckert et al. 2012"
] | [
"To convert from surface brightness to density, we use the following widely used approach"
] | [
"Uses"
] | [
[
743,
761
]
] | [
[
653,
741
]
] |
2022MNRAS.514.2407S__Matsunaga_et_al._2011_Instance_1 | The age distribution of the inner Galaxy is less well known. Traditionally, from photometry, the bulge has been viewed as an old structure (e.g. Zoccali et al. 2003) but this was thrown into question by spectroscopic ages of microlensed dwarfs (Bensby et al. 2013), many of which are young. Recent work by Bernard et al.... | [
"Matsunaga et al. 2011"
] | [
"Nogueras-Lara et al. (2020a) have used the luminosity of red clump stars to conclude the majority ($\\sim 95\\, \\mathrm{per\\, cent}$) of the nuclear stellar disc formed more than $8\\, \\mathrm{Gyr}$ ago with some evidence of a more recent ($\\lt 1\\, \\mathrm{Gyr}$ ago) star formation burst",
"This is consist... | [
"Background",
"Similarities",
"Similarities"
] | [
[
1444,
1465
]
] | [
[
1157,
1442
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[
1468,
1555
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[
1580,
1771
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] |
2020MNRAS.494.5576P__Pastorello_et_al._2018_Instance_1 | Another interesting type of transient to compare DES17X1boj and DES16E2bjy with are the SN impostors. As shown in Fig. 3, SN2009ip has a short phase of re-brightening around the same phase as the secondary peak of the DES-SN transients, and its peak brightness (MV = −17.7; see e.g. Fraser et al. 2013) is similar to DES... | [
"Pastorello et al. 2018"
] | [
"Furthermore, our photometric data also constrain the long-term variability of DES17X1boj to a level below what was seen in SN2009ip",
"and SN2016bdu",
"in the years before the brightest event (MV in range −13 to −14)."
] | [
"Compare/Contrast",
"Compare/Contrast",
"Compare/Contrast"
] | [
[
927,
949
]
] | [
[
755,
886
],
[
912,
925
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[
951,
1016
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2016ApJ...833....7Y__Owen_&_Wu_2013_Instance_2 | We use the N-body simulation package—MERCURY (Chambers 1999)—to numerically investigate the effects of photo-evaporation on the dynamical evolution of planet–satellite systems. We choose the Bulirsch–Stoer integration algorithm, which can handle close encounter accurately. It is important in the simulations, as we will... | [
"Owen & Wu 2013"
] | [
"The orbit has a period of ∼10 days (typical value of Kepler planets), and it is sufficiently close to the central star to be subject to significant photo-evaporation effect"
] | [
"Uses"
] | [
[
1966,
1980
]
] | [
[
1792,
1964
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] |
2019MNRAS.485.3715B__Reid_et_al._2014_Instance_1 | The presumed WD cooling age is ≳5 Gyr. If it has a low mass, this age limit can be larger since after the Roche lobe detachment a proto-WD goes through the contraction phase until it reaches its cooling track (Istrate et al. 2014, 2016). The duration of this phase increases as the mass of the proto-WD decreases, and ma... | [
"Reid et al. 2014"
] | [
"Using the J0740 proper motion value from Table 1, the Sun’s Galactocentric velocity and the distance (240 km s−1 and 8.34 kpc, respectively;",
"we calculated these corrections to the pulsar period derivative: $\\dot{P}_{\\rm S}=3.0\\times 10^{-21}$, $\\dot{P}_{\\rm G,\\perp }=-1.6\\times 10^{-22}$, $\\dot{P}_{\\... | [
"Uses",
"Uses"
] | [
[
906,
922
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] | [
[
765,
905
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[
925,
1298
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2021MNRAS.507.2012B__Vogelsberger_et_al._2014a_Instance_1 | Our simulations were run using the AREPO (Springel 2010; Pakmor, Bauer & Springel 2011; Pakmor et al. 2016; Weinberger, Springel & Pakmor 2020) moving-mesh magnetohydrodynamics (MHD) code. The code solves for gravity coupled with MHD. The gravity solver uses the PM-tree method (Barnes & Hut 1986) and the MHD solver use... | [
"Vogelsberger et al. 2014a"
] | [
"AREPO has been used to produce simulations of the Universe at a wide range of scales. At the largest scales, we have uniform volume cosmological simulations such as the Illustris",
"suites. These simulations have box sizes ranging from ∼50 to ∼300 Mpc and baryonic mass resolutions ranging from ∼105 to 107 M⊙."
] | [
"Background",
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[
610,
635
]
] | [
[
411,
589
],
[
853,
981
]
] |
2021MNRAS.504..228S__Lyne_&_Manchester_1988_Instance_1 | In addition, broad-band polarization observations provide essential information about the pulsar radio emission mechanism, beam geometry, and the Galactic magneto-ionic ISM. Pulsars are among the most highly polarized radio sources known (e.g. Lyne & Smith 1968; Gould & Lyne 1998), and the polarization varies with obse... | [
"Lyne & Manchester 1988"
] | [
"In addition, the linear polarization P.A.s across pulse phase can constrain the beam size and inclination angles, with respect to the pulsar’s rotation axis and our line of sight (LoS). For example, the rotating vector model (RVM) predicts a smooth ‘S’-shape, due to the projected vectors of the magnetic field line... | [
"Background"
] | [
[
877,
899
]
] | [
[
497,
848
]
] |
2018MNRAS.476.3631P__Shi_&_Sheth_2018_Instance_1 | The left-hand panel of Fig. 3 shows the scatter plot of b1 and mass, coloured by $1+\delta _{5\,h^{-1}\,{\rm Mpc}}$. There is an obvious correlation visible, with a largely vertical trend in which b1 increases monotonically with $\delta _{5\,h^{-1}\,{\rm Mpc}}$. The symbols with errors show the median bias as a functio... | [
"Shi & Sheth 2018"
] | [
"This trend is consistent with previous results in the literature, which have shown that large-scale bias is more strongly correlated with halo-centric overdensity than it is with halo mass (see e.g."
] | [
"Similarities"
] | [
[
756,
772
]
] | [
[
537,
735
]
] |
2021MNRAS.500.3368S__Dubinski_1998_Instance_1 | Like normal elliptical galaxies, the analysis of the stellar populations in the inner regions of BCGs indicates that the bulk of their stars was formed rapidly in a very intense starburst at redshift z > 2 (Renzini 2006). However, despite sharing similar morphologies with normal massive ellipticals, in addition to red ... | [
"Dubinski 1998"
] | [
"BCGs constitute a special category of objects with peculiar star formation histories (SFHs) seen from both observations",
"and models"
] | [
"Background",
"Background"
] | [
[
702,
715
]
] | [
[
530,
649
],
[
690,
700
]
] |
2017AandA...606A..17M__Conselice_et_al._2003_Instance_1 | Studies of SMGs over the past few tens of years have provided valuable insights into their properties. These include the redshift distribution (e.g. Chapman et al. 2005; Aretxaga et al. 2007; Wardlow et al. 2011; Yun et al. 2012; Smolčić et al. 2012; Simpson et al. 2014, 2017; Zavala et al. 2014; Miettinen et al. 2015a... | [
"Conselice et al. 2003"
] | [
"Studies of SMGs over the past few tens of years have provided valuable insights into their properties. These include",
"merger incidence (e.g."
] | [
"Background",
"Background"
] | [
[
636,
657
]
] | [
[
0,
116
],
[
613,
635
]
] |
2021MNRAS.500.1817L__Abbott_et_al._2020b_Instance_2 | Since the errors of the LIGO-estimated rates are dominated by Poisson statistics (Abbott et al. 2020a,b), we approximate the PDF for the expected number of detections $\mathcal {N}=\mathcal {R}VT$ (from the surveyed space–time volume VT) by $\mathrm{d}P/\mathrm{d}\mathcal {N}\propto \mathcal {N}^{k-1/2}\mathrm{e}^{-\ma... | [
"Abbott et al. 2020b"
] | [
"From the median values of $\\bar{\\mathcal {R}}_{190814}=7\\rm \\, Gpc^{-3}\\, yr^{-1}$",
"$\\bar{\\mathcal {R}}_{\\rm 170817}=760\\rm \\, Gpc^{-3}\\, yr^{-1}$, and $\\bar{\\mathcal {R}}_{\\rm 190425}=460\\rm \\, Gpc^{-3}\\, yr^{-1}$",
"we obtain the effective surveyed space–time volumes $VT=1.2/\\bar{\\mathca... | [
"Uses",
"Uses",
"Uses"
] | [
[
785,
804
]
] | [
[
547,
629
],
[
653,
783
],
[
807,
980
]
] |
2021MNRAS.504.1939G__Zhang_&_Yan_2011_Instance_1 | For the magnetic field configurations considered in this work, the polarization angle can only change exactly by Δϕ = 90○ and a gradual change of the PA is not possible. There are tantalizing hints of a 90○ change in the PA in some of the GRBs, as discussed above, but the results are not yet conclusive. The result pres... | [
"Zhang & Yan 2011"
] | [
"Alternatively, such a change in the PA can be obtained due to magnetic reconnection, e.g. in the ICMART model",
"where the local magnetic field orientation, which is orthogonal to the wave vector of the emitted photon, itself changes by 90○ as the field lines are destroyed and reconnected in the emission region"... | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1158,
1174
]
] | [
[
1047,
1156
],
[
1177,
1376
]
] |
2015MNRAS.446.1799O__Fruscione_et_al._2006_Instance_1 | A262 (RA = 01:52:46.299, Dec. = +36:09:11.80) is a bright, nearby poor cluster at z = 0.0162 (Struble & Rood 1999) with mean ICM temperature ≈2 keV( see e.g. Vikhlinin et al. 2005, 2006; Sato, Matsushita & Gastaldello 2009; Sanders et al. 2010). Due to its low mass and temperature, it may be considered as an intermedia... | [
"Fruscione et al. 2006"
] | [
"We used dmcopy tool in CIAO: Chandra's data analysis system",
"to restrict the energy range to 0.7−7 keV for both imaging and spectral analysis in all of the four data product files: event file, blank-sky observation, RMF and ARF."
] | [
"Uses",
"Uses"
] | [
[
529,
550
]
] | [
[
468,
527
],
[
552,
719
]
] |
2015ApJ...808..157M__Nayfeh_1981_Instance_1 | As we have seen, the asymptotic reduction of the original CR propagation problem, given by Equation (9), to its isotropic part cannot proceed to higher orders of approximation using a simple asymptotic series in Equation (10) and requires a multi-time asymptotic expansion. In the Chapman–Enskog method, the operator
... | [
"Nayfeh 1981"
] | [
"Perhaps more customary today, and equivalently, is to introduce a hierarchy of formally independent time variables (e.g.,",
", so that"
] | [
"Uses",
"Uses"
] | [
[
1296,
1307
]
] | [
[
1174,
1295
],
[
1315,
1324
]
] |
2016ApJ...826..137M__Jewitt_et_al._2013_Instance_1 | We performed a preliminary, zeroth-order analysis of the images by constructing a syndyne–synchrone map for each observing date. From those maps, we inferred that the activation time of the asteroid should be close in time to the discovery date, owing to the absence of dust features that could have shown up at the corr... | [
"Jewitt et al. 2013"
] | [
"In addition, there are no dust condensations along the direction of isolated synchrones, which could have indicated short bursts of activity",
"or several separated short bursts, as in the case of P/2013 P5"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
815,
833
]
] | [
[
550,
690
],
[
751,
813
]
] |
2017MNRAS.472.1152R__Cenko_et_al._2010_Instance_2 | Alternatively, if a magnetar is the central engine powering GRBs, we might expect to see periodic features in the emission. Known magnetars have clear periodic signals in their emission caused by their rotation periods (e.g. Mazets et al. 1979; Kouveliotou et al. 1998). The X-ray pulsations typically contribute to 30 p... | [
"Cenko et al. 2010"
] | [
"The prompt emission of GRB 090709A possibly showed evidence of a periodic signal",
"however this was ruled out with a more careful analysis of the prompt data from BAT, X-ray Telescope (XRT) and X-ray Multi-mirror Mission (XMM) observations of the X-ray afterglow",
"However, in the majority of these studies, t... | [
"Compare/Contrast",
"Compare/Contrast",
"Compare/Contrast"
] | [
[
2232,
2249
]
] | [
[
1884,
1964
],
[
2051,
2230
],
[
2273,
2536
]
] |
2020ApJ...898L..33P__Delrez_et_al._2018_Instance_1 | For the TRAPPIST-1 system, data obtained by HST provide initial constraints on the extent and composition of the planet’s atmospheres, suggesting that the four innermost planets do not have a cloud/haze-free H2-dominated atmosphere (de Wit et al. 2016, 2018). However, follow-up work by Moran et al. (2018) have shown th... | [
"Delrez et al. 2018"
] | [
"Transit observations with Spitzer",
"have found a +208 ± 110 ppm difference between the 3.6 and 4.2 μm bands, suggesting CO2 absorption."
] | [
"Motivation",
"Background"
] | [
[
693,
711
]
] | [
[
658,
691
],
[
713,
812
]
] |
2021ApJ...907...55M__Wang_2016_Instance_1 | Elsässer variables (Elsässer 1950) are usually employed in solar wind studies to separate the outward-propagating waves (denoted by z+) and the reflected or inward propagating waves (denoted by z−). The separation is exact for even fully nonlinear, unidirectionally propagating waves in homogeneous and incompressible pl... | [
"Wang 2016"
] | [
"While kink waves, both propagating and standing, are routinely observed in the corona (e.g.,"
] | [
"Background"
] | [
[
1290,
1299
]
] | [
[
1126,
1218
]
] |
2020AandA...641A.139D__Dvorak_et_al._(2015)_Instance_2 | The use of N-body simulations that include fragmentation allows us to perform a more detailed study of the final composition of the planets formed. In particular, we can study the water loss and/or accretion of the final planets more realistically than in the classic models of accretion. Marcus et al. (2010) presented ... | [
"Dvorak et al. (2015)"
] | [
"The investigations developed by Marcus et al. (2010) and",
"suggest that incorporating a realistic model of volatile transport and removal in an N-body code, may lead to reduced water contents on the resulting terrestrial-like planets, in comparison with those derived from classical models that assume perfect me... | [
"Background",
"Background"
] | [
[
1144,
1164
]
] | [
[
1087,
1143
],
[
1165,
1424
]
] |
2021ApJ...908...95H__Díaz-Sánchez_et_al._2017_Instance_1 | Here we outline our sample of strongly lensed Planck-selected, dusty star-forming galaxies, hereafter “LPs” (Table 1). Our sample of 24 LPs began with a Planck and Herschel cross-match identification of eight objects (8/24) with continuum detections at 857 GHz (Harrington et al. 2016) greater than 100 mJy. The remainin... | [
"Díaz-Sánchez et al. 2017"
] | [
"The use of Planck and WISE data resulted in the discovery of the brightest known, dusty starburst galaxy at z > 1, the “Cosmic Eyebrow”",
"which has also been independently recovered as one of the LPs presented in this survey work."
] | [
"Background",
"Similarities"
] | [
[
1114,
1138
]
] | [
[
977,
1112
],
[
1166,
1258
]
] |
2016AandA...588A..42S__Hopkins_et_al._2010_Instance_1 | Classical bulges (hereafter ClBs) are the central building blocks in many early-type spiral galaxies. Classical bulges might have formed as a result of major mergers during the early phase of cosmic evolution (Kauffmann et al. 1993; Baugh et al. 1996; Hopkins et al. 2009; Naab et al. 2014), or through a number of other... | [
"Hopkins et al. 2010"
] | [
"Classical bulges might have formed as a result of",
"multiple minor mergers"
] | [
"Background",
"Background"
] | [
[
645,
664
]
] | [
[
102,
151
],
[
599,
621
]
] |
2021AandA...648A...5M__Windhorst_et_al._(1990)_Instance_2 | Another important consistency check regards the angular size distribution of the sources. Figure 6 shows the cumulative size distributions of the final catalogs combined together, in four flux density bins (yellow solid lines). Such distributions can be considered reliable only down to a flux-dependent minimum intrinsi... | [
"Windhorst et al. (1990)"
] | [
"It is interesting to note, however, that if we assume a steeper exponent for the distribution function described by Eq. (7) (i.e., q = 0.80), we get a very good match with observations at all fluxes, when assuming a flux-dependent scaling factor (k = k(S); see Eq. (9)) for the",
"median size – flux relation (bla... | [
"Similarities",
"Similarities"
] | [
[
1930,
1953
]
] | [
[
1652,
1929
],
[
1954,
2015
]
] |
2017ApJ...849..123M__Ansdell_et_al._2016_Instance_1 | Until recently, only β Pic and 49 Cet were known as CO-bearing debris disks (Vidal-Madjar et al. 1994; Zuckerman et al. 1995; Roberge et al. 2000). Later, more such objects were discovered, and the first statistical studies could be done (Greaves et al. 2016; Lieman-Sifry et al. 2016; Péricaud et al. 2017). Our present... | [
"Ansdell et al. 2016"
] | [
"Line luminosities of detected CO-bearing disks span almost two orders of magnitude, in which the brightest disks have luminosities that are comparable to those of fainter Herbig Ae and T Tauri disks"
] | [
"Background"
] | [
[
830,
849
]
] | [
[
630,
828
]
] |
2022MNRAS.516.3900A__Calmonte_et_al._2016_Instance_1 | Sudden outbursts of NH3 simultaneously with H2S detected with the ROSINA-DFMS instrument on the Rosetta S/C point to the presence of abundant ammonium hydrosulphide in or on carbonaceous grains from comet 67P/Churyumov-Gerasimenko. There seems to be a clear distinction between the nucleus ice, where H2S and NH3 exist i... | [
"Calmonte et al. 2016"
] | [
"While for operational reasons, S4 could not be measured close to the dust impacts, S4 was clearly identified in periods where the coma was very dusty"
] | [
"Uses"
] | [
[
794,
814
]
] | [
[
643,
792
]
] |
2019MNRAS.482.3288G__Mayer_2013_Instance_1 | The orbital decay of BSBHs may slow down or stall at ∼pc scales (e.g. Begelman et al. 1980; Milosavljević & Merritt 2001; Zier & Biermann 2001; Yu 2002; Vasiliev, Antonini & Merritt 2014; Dvorkin & Barausse 2017; Tamburello et al. 2017), or the barrier may be overcome in gaseous environments (e.g. Gould & Rix 2000; Esc... | [
"Mayer 2013"
] | [
"The accretion of gas and the dynamical evolution of BSBHs are likely to be coupled",
"such that the occurrence rate of BSBHs depends on the initial conditions and gaseous environments at earlier phases (e.g. thermodynamics of the host galaxy interstellar medium;"
] | [
"Background",
"Background"
] | [
[
1516,
1526
]
] | [
[
908,
990
],
[
1262,
1438
]
] |
2015ApJ...806....1M__Ahn_et_al._2012_Instance_1 | For the clustering measurements, we use the sample of galaxies compiled in Data Release 11 (DR11) of the SDSS-III project. The SDSS-III is a spectroscopic investigation of galaxies and quasars selected from the imaging data obtained by the SDSS (York et al. 2000) I/II covering about 11,000 deg2 (Abazajian et al. 2009) ... | [
"Ahn et al. 2012"
] | [
"The",
"BOSS project",
"obtained additional imaging data of about 3000 deg2"
] | [
"Background",
"Background",
"Background"
] | [
[
606,
621
]
] | [
[
554,
557
],
[
592,
604
],
[
643,
694
]
] |
2021AandA...650A.133J__Goss_&_Field_(1968)_Instance_1 | Collisions with charged particles, namely with electrons and heavier ions are not considered in the radiative-transfer calculations presented in this paper, but may play an important role in the excitation of the CH Λ-doublet, particularlyin regions with high electron fractions,
$x_{\textrm{e}} = n_{\textrm{e}}/(n_{\... | [
"Goss & Field (1968)"
] | [
"These authors compute the collisional rate coefficients for collisions with electrons, either using perturbation methods such as those used by"
] | [
"Uses"
] | [
[
1012,
1031
]
] | [
[
869,
1011
]
] |
2022MNRAS.516.5289M__Thompson_et_al._2015_Instance_3 | Given the number densities within the mass-dissociation index plane of Fig. 8, we now ask ourselves whether known dissociated clusters, such as the Bullet cluster, are expected in L210N1024NR? The Bullet Cluster has a mass of $\sim 1.5 \times 10^{15} \, {\rm M}_{\odot }$ (e.g. Clowe et al. 2004; Bradač et al. 2006; Clo... | [
"Thompson et al. 2015"
] | [
"utilizing the same halo finder as"
] | [
"Similarities"
] | [
[
2191,
2211
]
] | [
[
2157,
2190
]
] |
2022MNRAS.516.1539O__Fujita,_Ohira_&_Yamazaki_2013_Instance_1 | In this scenario, the present γ-ray emission from the Fermi bubbles arises predominantly through inverse Compton scattering of an energetic non-thermal cosmic ray (CR) electron population in the remnant structures with ambient radiation supplied by the interstellar radiation field (ISRF) and the cosmological microwave ... | [
"Fujita, Ohira & Yamazaki 2013"
] | [
"In this scenario, the present γ-ray emission from the Fermi bubbles arises predominantly through inverse Compton scattering of an energetic non-thermal cosmic ray (CR) electron population in the remnant structures with ambient radiation supplied by the interstellar radiation field (ISRF) and the cosmological micro... | [
"Background"
] | [
[
666,
695
]
] | [
[
0,
595
]
] |
2017MNRAS.464L..26F__O'Sullivan_et_al._2001_Instance_2 | The diffuse hot gas X-ray luminosities in the 0.3–8 keV band are taken from the work of KF15. They have carefully removed the contribution from discrete sources such as low-mass X-ray binaries (Fabbiano 2006) to the total X-ray luminosity, leaving the diffuse gas contribution LX, Gas. A correction to bolometric would i... | [
"O'Sullivan et al. 2001"
] | [
"Although the contribution from discrete sources in the ROSAT data cannot be subtracted as accurately as it can for Chandra data, their contribution is only about 1 per cent of the diffuse gas luminosity for these high-mass galaxies (see"
] | [
"Uses"
] | [
[
892,
914
]
] | [
[
655,
891
]
] |
2022MNRAS.517.4327M__Indebetouw_et_al._2014_Instance_1 | Supernovae (SNe) play a dual role in the evolution of interstellar dust. On one hand, they are the most important source of dust production in galaxies, but on the other had had also the most important source of grain destruction. Theoretical models show that most of the heavy elements produced can precipitate out of t... | [
"Indebetouw et al. 2014"
] | [
"Infrared and submilimetre observations of",
"SN 1987A",
"confirm the presence of ∼0.1–1.0 M⊙ of dust, indicating that a substantial fraction of refractory elements in their ejecta went to dust grains."
] | [
"Background",
"Background",
"Background"
] | [
[
617,
639
]
] | [
[
466,
507
],
[
585,
593
],
[
771,
914
]
] |
2019MNRAS.482.4290H__Hofmann_2017_Instance_1 | The only non-standard term involves the factor $\frac{\mathrm{d} q}{\mathrm{d} \eta }$. As usual, the perturbation Ψ of the unperturbed phase-space distribution f0 = 1/(exp (ε/T0) − 1) is introduced as
(36)
\begin{eqnarray*}
f = f_0(\epsilon) \left(1 + \Psi \right)\, ,
\end{eqnarray*}
where the co-moving energy ε r... | [
"Hofmann 2017"
] | [
"The use of the geodesic equation for a quasi-particle must be questioned, if this particle associates with pure quantum fluctuations"
] | [
"Compare/Contrast"
] | [
[
1148,
1160
]
] | [
[
1014,
1146
]
] |
2022AandA...663A..50B__Buat_et_al._2005_Instance_1 | In the absence of dust, the spectral emission of a normal star-forming galaxy is dominated by stellar populations of different ages with superimposed nebular emission, mainly in the form of recombination lines as well as continuum. The interaction with dust has a dramatic effect, both dimming and reddening the emission... | [
"Buat et al. 2005"
] | [
"While this approach initially appeared to work remarkably well in the case of starburst galaxies",
"there is now ample evidence that there is no tight universal relation between the UV slope and the attenuation (e.g.,"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
2010,
2026
]
] | [
[
1773,
1869
],
[
1892,
2009
]
] |
2019AandA...622A..62A__Aviles_et_al._(2018)_Instance_2 | On the other hand, PT has experienced many developments in recent years (Matsubara 2008a; Baumann et al. 2012; Carlson et al. 2013), in part because it can be useful to analytically understand different effects in the power spectrum and correlation function for the dark matter clustering. These effects can be confirmed... | [
"Aviles et al. (2018)"
] | [
"The LPT for dark matter fluctuations in MG was developed in Aviles & Cervantes-Cota (2017), and further studies for biased tracers in"
] | [
"Extends"
] | [
[
1331,
1351
]
] | [
[
1197,
1330
]
] |
2016ApJ...833...51Y__Liu_et_al._2012_Instance_1 | The past two decades have seen rapid progress in the field of solar magnetoseismology (SMS; for recent reviews, see e.g., Nakariakov & Verwichte 2005; Banerjee et al. 2007; De Moortel & Nakariakov 2012; Nakariakov et al. 2016; Wang 2016). Among the rich variety of low-frequency waves observed in the Sun’s atmosphere, f... | [
"Liu et al. 2012"
] | [
"Among the rich variety of low-frequency waves observed in the Sun’s atmosphere, flare-related quasi-periodic fast propagating wave trains have received much attention",
"Their quasi-periods usually range from 25 to 400 s. These wave trains were",
"and extensively observed in images acquired with the Atmospheri... | [
"Background",
"Background",
"Background"
] | [
[
687,
702
]
] | [
[
239,
405
],
[
451,
525
],
[
555,
686
]
] |
2018AandA...619A..13V__Saviane_et_al._2012_Instance_5 | 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"
] | [
"In Table 3 we provide the coordinates, radial velocities, and the sum of the equivalent widths for the cluster member stars, both measured (“m”) and corrected (“c”) to the system of"
] | [
"Uses"
] | [
[
2364,
2383
]
] | [
[
2182,
2363
]
] |
2020MNRAS.498..464F__Alam_et_al._2017_Instance_1 | The late-time matter density PDF at a given smoothing scale is mostly sensitive to the skewness of the primordial density field at that scale and to the running of that skewness around the smoothing scale. As such – unless the PDF is measured on a wide range of smoothing scales – it can only poorly distinguish between ... | [
"Alam et al. 2017"
] | [
"In this paper, we consider an analysis of the PDF at redshift z = 1 in a survey volume of V = 100(Gpc h−1)3, which is smaller than the effective volume of upcoming surveys such as Spherex with Veff ≈ 150(Gpc h−1)3 and somewhat larger than existing surveys such as BOSS with Veff ≈ 55(Gpc h−1)3"
] | [
"Compare/Contrast"
] | [
[
802,
818
]
] | [
[
489,
782
]
] |
2019ApJ...871..176X__Eldridge_et_al._2013_Instance_1 | The progenitors of SNe Ib/c have been thought to be Wolf-Rayet (W-R) stars with high initial masses (MZAMS ≳ 25 M⊙; Crowther 2007). Before core collapse, these stars usually have experienced severe mass loss through strong stellar winds or due to interaction with companion stars (van der Hucht 2006; Paxton et al. 2015)... | [
"Eldridge et al. 2013"
] | [
"However, there are increasing studies suggesting that a lower-mass binary scenario is more favorable for most SNe Ib/c, considering the measured low ejecta masses"
] | [
"Background"
] | [
[
774,
794
]
] | [
[
610,
772
]
] |
2022MNRAS.513..232N__Hayden_et_al._2015_Instance_1 | There are a plethora of data available in the form of spectra, astrometric, and photometric information, as well as multiwavelength maps with the advent of large-scale spectroscopic (Apache Point Observatory Galactic Evolution Experiment/APOGEE: Eisenstein et al. 2011, RAdial Velocity Experiment/RAVE: Steinmetz et al. ... | [
"Hayden et al. 2015"
] | [
"At present, data from large-scale spectroscopic surveys",
"have led to the discovery of this trend at different galactocentric radius, R, and average height, |Z|, across the Galaxy shedding light on the disc formation and evolution scenarios."
] | [
"Background",
"Background"
] | [
[
1618,
1636
]
] | [
[
1541,
1596
],
[
1660,
1843
]
] |
2021AandA...651A.111P__Herrera-Camus_et_al._2018_Instance_2 | Irrespective of its origin, the [C II] emission is linked to the presence of stellar far-ultraviolet (FUV) photons (E 13.6 eV). As FUV photons are tied to the presence of massive O and B stars that have short lifetimes, the [C II] 158 μm line is also astar formation rate (SFR) indicator. Indeed, ISO, Herschel and SOFIA... | [
"Herrera-Camus et al. 2018"
] | [
"Some studies have indicated that not only [C II] emission is deficient in some sources, but other FIR cooling lines ([O I], [O III], [N II]), as well (e.g.,"
] | [
"Background"
] | [
[
2035,
2060
]
] | [
[
1851,
2007
]
] |
2020ApJ...903L..12H__Petschek_1964_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... | [
"Petschek 1964"
] | [
"In particular, two major categories of MR have been proposed: the steady state model with a single X line and the outflow approaching the Alfvén speed"
] | [
"Background"
] | [
[
1065,
1078
]
] | [
[
913,
1063
]
] |
2018AandA...616A.173K__Pickett_1991_Instance_1 | The room-temperature millimeter wave rotational spectrum of ethyl isocyanate in Fig. 1 presents an exceptionally high line density. Its analysis was started using predictions from the spectroscopic constants obtained in the previous microwave works (Heineking et al. 1994; Kasten et al. 1983; Sakaizumi et al. 1976) for ... | [
"Pickett 1991"
] | [
"The identification of Ka = 0 and lower-frequency Ka = 1 transitions, originating from J0 J and J1 J energy levels, was relatively straightforward and their assignment and analysis could be easily expanded up to 340 GHz (J˝ = 64) with the help of the Loomis-Wood-type plot technique from the AABS package",
"and SP... | [
"Future Work",
"Future Work"
] | [
[
911,
923
]
] | [
[
554,
857
],
[
879,
909
]
] |
2021MNRAS.500.5009M__Bono_et_al._2003_Instance_2 | RR Lyrae are old low-mass stars that, during the central helium-burning phase, show mainly radial pulsation while crossing the classical instability strip in the colour–magnitude diagram. From the observational point of view, they represent the most numerous class of pulsating stars in the Milky Way and, being associat... | [
"Bono et al. 2003"
] | [
"in the last decades there has been a debate on the coefficient of the metallicity term of the KB and PL relation (see e.g."
] | [
"Motivation"
] | [
[
2658,
2674
]
] | [
[
2535,
2657
]
] |
2022MNRAS.511.2105K__McElroy_et_al._2015_Instance_1 | AGN feedback can exist in several forms such as radiation, thermal, or non-thermal (cosmic rays) pressure-driven winds, jet-mode feedback, and via magnetic forces on accretion disc scales. AGN feedback can explain several observed properties such as the presence of high velocity (>1000 km s−1) multiphase gas outflows i... | [
"McElroy et al. 2015"
] | [
"High velocity outflows from AGN host galaxies have been reported in numerous studies in the literature",
"using optical spectroscopy"
] | [
"Background",
"Background"
] | [
[
759,
778
]
] | [
[
536,
638
],
[
706,
732
]
] |
2015ApJ...808...56M__Beaulieu_et_al._2011_Instance_3 | The field of extrasolar planetary transits is one of the most productive and innovative subject in astrophysics in the last decade. Transit observations can be used to measure the size of planets, their orbital parameters (Seager and Mallén-Ornelas 2003), and stellar properties (Mandel & Agol 2002; Howarth 2011), to st... | [
"Beaulieu et al. 2011"
] | [
"The results obtained with these methods appear to be strongly dependent on a few assumptions, e.g., the degree of the polynomial adopted, the photometric technique, the centroid determination, calibrating instrument systematics over the out-of-transit only or the whole observation (e.g.,"
] | [
"Background"
] | [
[
2482,
2502
]
] | [
[
2193,
2481
]
] |
2017AandA...608A..67B__Luu_(1991)_Instance_1 | The large Jovian irregular satellites have been observed and analyzed using their light curves, colours, and reflectance spectra but the reported measurements are sometimes contradictory. The multicolour observation of some retrograde and prograde Jovian irregular satellites by Tholen & Zellner (1984) suggested C-class... | [
"Luu (1991)"
] | [
"identified C- and D-type asteroid spectral features for both prograde and retrograde families based on spectroscopic observations of JV-JXIII and suggested them to be similar to Jupiter’s Trojan asteroids."
] | [
"Background"
] | [
[
687,
697
]
] | [
[
698,
903
]
] |
2022AandA...661A..10B__Ghirardini_et_al._2021a_Instance_1 | 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)"
] | [
"Following the method presented in"
] | [
"Uses"
] | [
[
241,
266
]
] | [
[
207,
240
]
] |
2018AandA...615L..16F__Hily-Blant_et_al._2013b_Instance_1 | The observational and theoretical studies of nitrogen isotope fractionation in star-forming regions can help to constrain nitrogen chemistry. Nitrogen has two stable isotopes, 14N and 15N. The elemental abundance ratio [14N/15N]elem in the local interstellar medium (ISM) has been estimated to be ~200–300 from the absor... | [
"Hily-Blant et al. 2013b"
] | [
"In L1544, the 14N/15N ratio of several different molecules has been measured:",
"CN/C15N = 500 ± 75"
] | [
"Uses",
"Uses"
] | [
[
955,
978
]
] | [
[
519,
596
],
[
935,
953
]
] |
2022MNRAS.515L..39Z__Koefoed_et_al._2016_Instance_1 | Currently, this 53Mn–53Cr age of 4566.6 ± 0.6 Ma for crystallization for EC 002 represents the oldest record of volcanism in the Solar system. For example, the oldest crust formation of Earth and Moon only dates back to ∼4.3–4.4 Ga (O’Neil & Carlson 2017; Borg et al. 2019), and Mars, Vesta, and the angrite and main-gro... | [
"Koefoed et al. 2016"
] | [
"The crystallization age of EC 002 also predates all those of the other dated achondrites, such as",
"and NWA 7325"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
822,
841
]
] | [
[
553,
650
],
[
808,
820
]
] |
2017MNRAS.464..968S__Tacconi_et_al._2006_Instance_2 | Comparison of apparent effective diameters of these sources to direct size measurements supports a similar conclusion. Simpson et al. (2015) present ALMA observations of 23 SCUBA-2-selected SMGs with a median physical half-light diameter of 2.4 ± 0.2 kpc, while Ikarashi et al. (2015) show ALMA observations of 13 AzTEC-... | [
"Tacconi et al. 2006"
] | [
"However, Simpson et al. (2015) point out that the submillimetre sizes are consistent with resolved 12CO detections, while the sizes derived from 1.4 GHz imaging are about two times larger because of the cosmic ray diffusion, which can explain the results before higher frequency observations at ALMA were possible"
... | [
"Compare/Contrast"
] | [
[
1286,
1305
]
] | [
[
950,
1263
]
] |
2021ApJ...908..164K__Beckwith_et_al._2006_Instance_1 | While these S/Ns may not look promising, there is an interesting question that one can ask: How much LUVOIR-15 m time is needed to detect the present Earth-level concentration of NO2 around a Sun-like star at 10 pc? Figure 6(a) shows the spectrum of the difference in geometric albedo with and without NO2. Also shown as... | [
"Beckwith et al. 2006"
] | [
"For comparison, to obtain the Hubble Ultra Deep Field (UDF) image, ∼400 hr of actual observation time (∼1 yr in real time) was needed"
] | [
"Background"
] | [
[
1000,
1020
]
] | [
[
865,
998
]
] |
2022MNRAS.512.4136C__Pérez-Montero_&_Contini_2009_Instance_1 | If we recall the tight, monotonic dependence of the position of galaxies along the SF sequence in the diagram with metallicity (as outlined in Section 3.1), we can interpret our global results of Figs 4 and 5 as a manifestation of the existence of an O/H versus N/O relation for SDSS star-forming galaxies, whose intrins... | [
"Pérez-Montero & Contini 2009"
] | [
"A tight relationship between O/H and N/O abundances is indeed observed in both H ii regions and local galaxies, especially at M⋆ ≳ 109.5M⊙"
] | [
"Similarities"
] | [
[
643,
671
]
] | [
[
454,
592
]
] |
2020AandA...633A..34C__Martell_&_Shetrone_2013_Instance_1 | Some studies use HIPPARCOS or Gaia data to determine the evolutionary status of field LiRG and show that these objects tend to accumulate close to the RGB bump, the clump, and the early-AGB (e.g. Charbonnel & Balachandran 2000; Kumar et al. 2011; Smiljanic et al. 2018; Deepak 2019), which is in agreement with open clus... | [
"Martell & Shetrone 2013"
] | [
"Other works report, however, that LiRG can be randomly located in the HRD",
"The distinction is crucial to understanding the processes that may provide an explanation for the phenomenon,"
] | [
"Differences",
"Motivation"
] | [
[
526,
549
]
] | [
[
365,
438
],
[
571,
680
]
] |
2018ApJ...868..139W__Schlickeiser_&_Jenko_2010_Instance_1 | By radio continuum surveys of interstellar space and direct in situ measurements in the solar system, it is well established that for many scenarios the background magnetic fields are spatially varying. However, the above research about parallel and perpendicular diffusion only explored the uniform mean magnetic field.... | [
"Schlickeiser & Jenko 2010"
] | [
"One can show that the spatially varying background magnetic fields lead to the adiabatic focusing effect of charged energetic particle transport and introduces correction to the particle diffusion coefficients (see, e.g.,"
] | [
"Background"
] | [
[
974,
999
]
] | [
[
321,
542
]
] |
2018ApJ...854...26L__Tian_2017_Instance_2 | The hot emission line of Fe xxi 1354.09 Å and the cool emission line of Si iv 1402.77 Å have been used in many spectroscopic studies to investigate chromospheric evaporation (e.g., Tian et al. 2014, 2015; Li et al. 2015b, 2017a, 2017b; Brosius et al. 2016; Zhang et al. 2016a, 2016b). It is widely accepted that the forb... | [
"Tian 2017"
] | [
"Using the relatively strong neutral lines (i.e., “O i” 1355.60 Å and “S i” 1401.51 Å), we also perform an absolute wavelength calibration for the spectra at the “O i” and “Si iv” windows, respectively"
] | [
"Uses"
] | [
[
2299,
2308
]
] | [
[
2079,
2279
]
] |
2022MNRAS.512..439C__Lian_et_al._2021_Instance_1 | 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"
] | [
"Newer, alternate cosmological probes could help alleviate this issue. Recent examples of such probes include",
"QSO angular size measurements that reach to z ∼ 2.7"
] | [
"Motivation",
"Background"
] | [
[
909,
925
]
] | [
[
286,
394
],
[
801,
852
]
] |
2017AandA...601A...4A__Cernicharo_et_al._1999_Instance_1 | In addition to thermal excitation through collisions with H2 and He, absorption of infrared photons and pumping to excited vibrational states, followed by radiative decay to rotational levels in the ground-vibrational state, is an important excitation mechanism of molecules in IRC +10216 (Deguchi & Uyemura 1984; Agúnde... | [
"Cernicharo et al. 1999"
] | [
"Here, we have included excitation through infrared pumping for all studied species, mostly through bands lying in the mid-infrared, where the flux in IRC +10216 is large"
] | [
"Uses"
] | [
[
635,
657
]
] | [
[
464,
633
]
] |
2020AandA...640L..11B__Segretain_1996_Instance_1 | Another possibly important cooling delay may arise from the phase separation of 22Ne during crystallization (Isern et al. 1991; Althaus et al. 2010). Our current best understanding is that at the small 22Ne concentrations typical of C/O white dwarfs (∼1% by number), the presence of 22Ne should not affect the phase diag... | [
"Segretain 1996"
] | [
"After a significant fraction of the core has crystallized, the temperature approaches the azeotropic point and the existing calculations indicate that the liquid phase is enriched in 22Ne relative to the solid"
] | [
"Background"
] | [
[
760,
774
]
] | [
[
549,
758
]
] |
2018AandA...616A..99K__Narang_et_al._2016_Instance_1 | 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"
] | [
"The mean speed of network jets is very similar, as reported in previous works (e.g.,"
] | [
"Similarities"
] | [
[
810,
828
]
] | [
[
707,
791
]
] |
2016AandA...589A..73R__Husser_et_al._2013_Instance_1 | Single-burst stellar population (SSP) models mimic uniform stellar populations of fixed age and metallicity, and are an important tool to study unresolved stellar clusters and galaxies. They are created by populating theoretical stellar evolutionary tracks with stars of a stellar library, according to a prescription gi... | [
"Husser et al. 2013"
] | [
"Theoretical stellar libraries like, e.g.",
"or PHOENIX",
"are generally available for both a large range in wavelength and in stellar parameters, whereas empirical libraries are found to be more incomplete in both respects. However, the advantage of the latter ones is that they are not hampered by the still la... | [
"Compare/Contrast",
"Compare/Contrast",
"Compare/Contrast"
] | [
[
864,
882
]
] | [
[
722,
762
],
[
832,
842
],
[
884,
1195
]
] |
2022AandA...659A..41E__Hobbs_et_al._2005_Instance_1 | The age of a neutron star is difficult to measure, as for many other astronomical sources. The most robust way to do it is by identifying the birth supernova of the neutron star. However, this can be done precisely only for a very small number of objects, as 5–10 supernovae have historically been observed in our galaxy... | [
"Hobbs et al. 2005"
] | [
"The transverse velocities of pulsars (based on proper motion and distance estimates) are particularly large, with a mean close to 310 km s−1"
] | [
"Background"
] | [
[
1032,
1049
]
] | [
[
890,
1030
]
] |
2019MNRAS.490.2071Y__Riess_et_al._2018_Instance_2 |
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)"
] | [
"Since for this present UM, the estimation of H0 from CMB alone is compatible with the local estimation of H0 by",
"thus, we can safely add both the data sets to see whether we could have something interesting."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
409,
428
]
] | [
[
297,
408
],
[
430,
524
]
] |
2022AandARv..30....6M__Blanton_et_al._2001_Instance_1 | In a similar fashion to what done by the CARLA survey, the COBRA (Clusters Occupied by Bent Radio AGN) program (Paterno-Mahler et al. 2017) searches for overdense regions around radio-AGN with double-lobed structures which are not aligned with each other, but bent by forming angles 180∘\documentclass[12pt]{minimal}
... | [
"Blanton et al. 2001"
] | [
"The rationale behind this search is that the radio lobes of these AGNs are most likely bent because of the ram pressure that occurs due to the relative motion of the AGN host galaxy and the ICM (e.g.,",
", which makes these sources good tracers for finding galaxy clusters."
] | [
"Motivation",
"Motivation"
] | [
[
802,
821
]
] | [
[
580,
780
],
[
875,
944
]
] |
2017AandA...608A...8L__Momose_et_al._(2014)_Instance_1 | At high redshift, the mapping of the extended Lyα haloes around galaxies (non-AGN) is however a lot more difficult because of sensitivity and resolution limitations. Detections of extended Lyman alpha emission at high redshift have been obtained in the past. While some large Lyα blobs have been observed (e.g. Steidel e... | [
"Momose et al. (2014)",
"Momose et al. (2014)"
] | [
"significantly increased the size of LAEs samples used by stacking ≈2000 and ≈4500 LAEs at redshift z ≃ 3 and 2.2 ≤ z ≤ 6.6, respectively.",
"found typical Lyα halo exponential scale lengths of 5–10 physical kpc."
] | [
"Background",
"Background"
] | [
[
998,
1018
],
[
1157,
1177
]
] | [
[
1019,
1156
],
[
1178,
1248
]
] |
2021MNRAS.507..904N__Castor,_Abbott_&_Klein_1975_Instance_1 | In equations (2) and (3), $\boldsymbol{f}_{\rm rad}=(f_{{\rm rad},\, r},\, f_{{\rm rad},\theta })$ is the radiation force described as
(6)$$\begin{eqnarray*}
\boldsymbol{f}_{\rm rad}=\frac{\sigma _{\rm e} \boldsymbol{F}_{\rm D}}{c}+\frac{\sigma _{\rm e} \boldsymbol{F}_{\rm line}}{c}M,
\end{eqnarray*}$$where σe is the... | [
"Castor, Abbott & Klein 1975"
] | [
"The line force is exerted mainly by the radiation flux in the UV band (200–3200 Å), because the metal lines are densely distributed (e.g."
] | [
"Background"
] | [
[
940,
967
]
] | [
[
801,
939
]
] |
2020ApJ...901...10D__Raddi_et_al._2015_Instance_1 | In order to calculate oxygen fugacities, we follow the methods described by Doyle et al. (2019). From the element abundance ratios, we assign oxygen to Mg, Si, Ca, and Al in the necessary proportions to obtain the relative abundances of the charge-balanced rock-forming oxide components MgO, SiO2, CaO, and Al2O3. The re... | [
"Raddi et al. 2015"
] | [
"Other studies have used similar methods for budgeting oxygen"
] | [
"Background"
] | [
[
732,
749
]
] | [
[
613,
673
]
] |
2022AandA...666A.153D__Dartois_2005_Instance_1 | In the first stages of star formation, protostars are still embedded in their parental cloud, where an active gas-grain chemistry is at work. Using either (i) background stars for dense clouds or (ii) a nascent protostellar object once it is able to emit sufficient light flux in the vibrational infrared wavelength rang... | [
"Dartois 2005"
] | [
"A harvest of astronomical observations from ground-based telescopes (e.g. UKIRT, IRTF, CFHT, and VLT) or satellites (e.g. IRAS, ISO, Akari, and Spitzer) of such lines of sight has led, since the late seventies, to the deciphering of the chemical compositions, column densities, and variations associated with these ... | [
"Background"
] | [
[
995,
1007
]
] | [
[
616,
948
]
] |
2021ApJ...919...33C__Staubert_et_al._2019_Instance_1 | The variability of the cyclotron line centroid energy in the spectra of XRPs is considered to be related to the geometry of accretion flow in close proximity to the surface of an NS. The geometry of the emitting region is related to the mass accretion rate. At low mass accretion rates, the radiation pressure is small, ... | [
"Staubert et al. 2019"
] | [
"The dynamics of the cyclotron line was shown to be dependent on the luminosity state of XRPs (see",
"for review)."
] | [
"Background",
"Background"
] | [
[
991,
1011
]
] | [
[
893,
990
],
[
1012,
1024
]
] |
2022MNRAS.512.1499R__LeVeque_1992_Instance_1 | Let ui be the evolved quantity at the coordinate position xi. Then, THC_M1 approximates the derivative of the flux f(u) at the location xi as
(31)$$\begin{eqnarray}
\partial _x f (u) \simeq \frac{F_{i - 1 / 2} - F_{i + 1 / 2}}{\Delta x},
\end{eqnarray}$$where Fi − 1/2 and Fi + 1/2 are numerical fluxes defined at $x_i... | [
"LeVeque 1992"
] | [
"The term φi + 1/2 is the so-called flux limiter"
] | [
"Uses"
] | [
[
796,
808
]
] | [
[
747,
794
]
] |
2020MNRAS.494.2948P__Lyne_et_al._1990_Instance_1 | Spider pulsar systems are characterized by having a low-mass companion star in a compact orbit with an energetic millisecond pulsar (MSP) resulting in heavy irradiation of the companion by the pulsar’s wind. The spider pulsar population has been observed to have a clearly bimodal distribution of companion star masses (... | [
"Lyne et al. 1990"
] | [
"A large proportion of the spiders, whether BWs or RBs, have been observed to exhibit (quasi-)periodic eclipses of the pulsars’ radio emission (e.g.",
"that are generally attributed to excess material in the orbits",
"interfering with the propagation of the radio emission.",
"Studies of such eclipses are key ... | [
"Background",
"Background",
"Background",
"Motivation"
] | [
[
690,
706
]
] | [
[
506,
653
],
[
708,
770
],
[
947,
1002
],
[
1003,
1317
]
] |
2016ApJ...833...76B__Klimchuk_et_al._2008_Instance_2 | A significant limitation of the model is that it ignores the well-established hydrodynamic evolution of the loop during the cooling process, involving the substantial transfer of mass between the chromosphere and the corona. For large downward heat fluxes, the transition region is unable to radiate the supplied energy,... | [
"Klimchuk et al. 2008"
] | [
"This basic idea has allowed the development of global “Enthalpy-Based Thermal Evolution of Loops” (EBTEL) models that describe the evolution of the average temperature and density in the coronal part of the loops;",
"these models are generally in good agreement with one-dimensional hydrodynamic simulations"
] | [
"Background",
"Similarities"
] | [
[
1343,
1363
]
] | [
[
1037,
1250
],
[
1251,
1341
]
] |
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