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 |
|---|---|---|---|---|---|---|
2016ApJ...828...41S__Chatterjee_et_al._2004_Instance_1 | Figure 1 shows the main features of the butterfly diagram: (1) the onset of the cycle at mid-latitudes; (2) the sunspot drift toward the equator and its slowdown represented by a change in the slope of the butterfly wing (Maunder 1904; Li et al. 2001); (3) the tail-like attachment over the minimum phase that is more pr... | [
"Chatterjee et al. 2004"
] | [
"FTD models driven only by the Babcock–Leighton mechanism",
"currently have the best agreement with observations",
"because the length of the simulated overlap is short and it occurs only during the minimum at low latitudes."
] | [
"Similarities",
"Similarities",
"Similarities"
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2018AandA...619A.105T__Matt_et_al._2015_Instance_1 | We have presented MoCA, a Monte Carlo code for Comptonisation in Astrophysics which includes polarisation. To our knowledge MoCA is the first code operating with single photons and including all special relativity and quantum effects. The main disadvantage of this approach is the long computing time, which implies the ... | [
"Matt et al. 2015"
] | [
"In some sources it has been found that coronae can have extremely high energy cut-off (e.g. NGC 5506,",
"and therefore thermal energy, which is inferred by measuring the curvature of NuSTAR spectra at high energy and in this context K–N effects cannot be neglected."
] | [
"Background",
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] | [
[
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]
] | [
[
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[
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2020ApJ...899..147F__Venot_et_al._2015_Instance_2 | The C/O ratio varies across exoplanets’ host star populations (Delgado Mena et al. 2010; Brewer & Fischer 2016; Brewer et al. 2017), and this variation is likely to be reflected in the composition of exoplanet atmospheres, assuming that they are formed with the same materials as their stars. Moreover, various processes... | [
"Venot et al. 2015"
] | [
"This work focused on the chemistry in atmospheres with T > 1000 K and a C/O ratio of 1 (representing C enhancement compared to the solar value of 0.54), because chemical models predict that the abundances of hydrocarbon and nitrile species increase by several orders of magnitude in these atmospheres compared to at... | [
"Motivation",
"Motivation"
] | [
[
1624,
1641
]
] | [
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2021MNRAS.500.1772N__Fernandez_et_al._2015_Instance_1 | While these early studies demonstrated the viability of neutron star mergers as a major r-process site, they identified only one ejection channel: ‘dynamical ejecta’ that are tidally flung out by gravitational torques. Since they are never substantially heated, these ejecta carry their original β −equilibrium electron ... | [
"Fernandez et al. 2015"
] | [
"As of today, many more mass ejection channels have been discussed: matter that becomes unbound on secular time-scales (∼1 s) from the post-merger accretion torus"
] | [
"Background"
] | [
[
1107,
1128
]
] | [
[
869,
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]
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2022MNRAS.515.1795B__Yang_et_al._2021_Instance_2 | The most widely adopted parametrization of the observed Universe is based on the so-called Λ cold dark matter (ΛCDM) model (Peebles 1984), relying on the existence of cold dark matter and dark energy (Λ) associated with a cosmological constant (Carroll 2001) in a spatially flat geometry. Predictions from this model hav... | [
"Yang et al. 2021"
] | [
"and do not fully rule out a spatially non-flat Universe"
] | [
"Compare/Contrast"
] | [
[
1392,
1408
]
] | [
[
1258,
1313
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] |
2021ApJ...920..145H__Damone_et_al._2018_Instance_2 | Over the past decade, many attempts to address this issue have been carried out, such as from the perspective of conventional nuclear physics and even exotic physics beyond the standard BBN framework (Angulo et al. 2005; Cyburt et al. 2008, 2016; Boyd et al. 2010; Pospelov & Pradler 2010; Fields 2011; Kirsebom & Davids... | [
"Damone et al. 2018"
] | [
"Meanwhile, enormous efforts have been made to refine the reaction rates of key BBN reactions in the past 20 yr",
"but the probability of solving or alleviating the 7Li problem by improving our knowledge of relevant nuclear reaction rates still cannot be eliminated."
] | [
"Background",
"Motivation"
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[
2016,
2034
]
] | [
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2017MNRAS.469S.238L__Massironi_et_al._2015_Instance_1 | ESA's Rosetta spacecraft orbited closely around comet 67P/Churyumov–Gerasimenko (hereafter 67P) during its 2 yr mission. From 2014 August to 2016 September, the camera system Optical, Spectroscopic, and Infrared Remote Imaging System (OSIRIS; Keller et al. 2007) onboard Rosetta observed the comet nucleus down to few ce... | [
"Massironi et al. 2015"
] | [
"The comet's surface revealed a wide diversity in morphology such as layering"
] | [
"Background"
] | [
[
755,
776
]
] | [
[
677,
753
]
] |
2018AandA...616A..34H__Mohamed_&_Podsiadlowski_(2012)_Instance_2 | The CO emission, tracking the bulk of the gas, reveals an almost face-on one-armed spiral, of which almost two full windings can be traced. What could be the origin of this spiral structure? As the majority of AGB stars are in binary systems, and perhaps all host planets, interaction between the outflow and a sufficien... | [
"Mohamed & Podsiadlowski (2012)"
] | [
"The morphology resulting from this particular type of wind–binary interaction is shown in Fig. 3 in"
] | [
"Background"
] | [
[
1510,
1540
]
] | [
[
1410,
1509
]
] |
2020ApJ...898....4C__Shipp_et_al._2018_Instance_1 | Detecting the halo response to the LMC-induced DM wake would be an exciting advancement in testing our assumptions about the properties of DM, as well as providing key constraints on the potential of the MW and the mass and orbital history of the LMC. However, the GC19 simulations give predictions for the response in t... | [
"Shipp et al. 2018"
] | [
"In reality, the MW stellar halo contains a wealth of substructure that is not yet phase mixed, in the form of stellar streams (e.g.,"
] | [
"Background"
] | [
[
584,
601
]
] | [
[
366,
498
]
] |
2019ApJ...883...53T__Armano_et_al._2016_Instance_1 | LISA Pathfinder (LPF; Antonucci et al. 2011), a European Space Agency (ESA) mission that operated near the first Sun–Earth Lagrange point (L1) from 2016 January through 2017 July, is in an ideal orbit to make such measurements. However, LPF flew no instrumentation dedicated to micrometeoroid or dust detection. LPF’s pr... | [
"Armano et al. 2016"
] | [
"The key achievement of LPF was placing two gold-platinum cubes known as “test masses” into a freefall so pure that it was characterized by accelerations at the femto-g level (e.g.,",
"the level required to detect the minute disturbances caused by passing gravitational waves."
] | [
"Background",
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[
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2020MNRAS.498.6013A__Magaña_et_al._2015_Instance_1 | On the other hand, observational data are used to test these models. Among the most frequently used are the cosmic microwave background radiation (CMB; Planck Collaboration XIII 2016; Aghanim et al. 2018), baryonic acoustic oscillations (BAO; Eisenstein et al. 2005; Blake et al. 2012; Alam et al. 2017; Bautista et al. ... | [
"Magaña et al. 2015"
] | [
"Grillo, Lombardi & Bertin (2008) introduced a methodology to estimate cosmological parameters using strong-lensing systems (SLS; see also"
] | [
"Background"
] | [
[
1107,
1125
]
] | [
[
950,
1087
]
] |
2018ApJ...856...51R__Reale_2014_Instance_2 | Close to the end of their formation, stars are surrounded by a gas and dust disk, from which planets form. Magnetic fields are known to play a key role in the star-disk system (Johns-Krull 2014). It is believed that the inner regions of the disk are significantly ionized by the stellar radiation and that accreting mate... | [
"Reale 2014"
] | [
"However, if a single stellar loop were flaring, the cooling time of the confined plasma would be proportional to the loop length"
] | [
"Uses"
] | [
[
2197,
2207
]
] | [
[
2048,
2176
]
] |
2018ApJ...856..144M__McIntosh_et_al._2011_Instance_1 | The solar corona is still enigmatic from a scientific point of view, with important unsolved questions about its nature, such as solar wind acceleration and coronal heating (McComas et al. 2007; Parnell & De Moortel 2012). Although finding solutions to these questions is important on its own, it is also expected to hav... | [
"McIntosh et al. 2011"
] | [
"However, the discovery of ubiquitous propagating transverse oscillations with CoMP",
"and SDO",
"led to the possibility of continuous diagnostics in time, i.e., dynamic coronal seismology."
] | [
"Background",
"Background",
"Background"
] | [
[
1935,
1955
]
] | [
[
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[
1926,
1933
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[
2177,
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2018MNRAS.478.2541F__Bertin_&_Arnouts_1996_Instance_1 | The distance between the peak of the main source and the transient source (blue POSS I) is ≈6 pixels or ≈6 arcsec (≈0.3 kpc) towards the North, at an angle of ≈− 10° (Fig. 2; left-hand column; rows 4–5). From the PSF characteristics of the blue POSS I and blue subtracted POSS images (Section 2.1.1), the transient sourc... | [
"Bertin & Arnouts 1996"
] | [
"Because of the faintness of the transient and its proximity to the larger, brighter main source, an automated detection algorithm such as SExtractor",
"implemented in GAIA36 2016A, was unsuccessful in deblending the two sources."
] | [
"Uses",
"Compare/Contrast"
] | [
[
510,
531
]
] | [
[
360,
508
],
[
534,
610
]
] |
2020MNRAS.498.4906B__Stinson_et_al._2013_Instance_1 | Throughout their short lifetimes, high-mass stars (>8 M⊙) inject large amounts of energy and momentum into their host environments through a variety of feedback processes (e.g. Krumholz et al. 2014). The most potentially disruptive of these feedback mechanisms occurs when the stars eventually die, exploding as supernov... | [
"Stinson et al. 2013"
] | [
"For example, SNe that explode within dense molecular clouds may be limited to disrupting their natal gas clouds, whilst SNe that explode into lower density environments can drive hot expanding bubbles to much larger distances (tens to hundreds of pc) and influence galactic scale processes (e.g."
] | [
"Background"
] | [
[
1287,
1306
]
] | [
[
903,
1198
]
] |
2016AandA...592A..74S__Roming_et_al._2005_Instance_1 | We observed our full sample of all 24 candidate highly variable AGN with Swift (Gehrels et al. 2004) for ~2 ks each, between 2010 and 2014 as part of a fill-in programme. All XRT (Burrows et al. 2005) observations were made in photon counting mode with exposure times ranging from 1.6–3.7 ks. The Swift-XRT data were obt... | [
"Roming et al. 2005"
] | [
"Simultaneous observations were made with",
"the Swift UV/Optical Telescope (UVOT;",
"with the u filter applied."
] | [
"Uses",
"Uses",
"Uses"
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[
643,
661
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[
508,
548
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605,
642
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[
663,
689
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2019AandA...625A..12G__Wunderlich_et_al._2019_Instance_1 | To calculate the boundaries of the HZ of a stagnant-lid Earth around M, K, G, and F dwarfs, we applied a 1D, cloud-free, radiative-convective climate model, which has been described in detail by von Paris et al. (2010) and von Paris et al. (2015), and is based on Kasting et al. (1984) and Segura et al. (2003). The radi... | [
"Wunderlich et al. 2019"
] | [
"Especially for late M dwarfs the cut-off at 4.545 μm leads to non-negligible loss in incoming radiation of up to ≈5% (see also",
"Hence, HZ boundaries obtained with the models lie closer to the star than would be expected when accounting for this missing portion of irradiation."
] | [
"Uses",
"Uses"
] | [
[
878,
900
]
] | [
[
751,
877
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[
903,
1051
]
] |
2016ApJ...833..216G___2010_Instance_1 | SEP events with gigaelectronvolt particles are generally rare. Typically about a dozen events occur during each solar cycle, although only two GLEs were reported in cycle 24, probably due to the change in the state of the heliosphere (Gopalswamy et al. 2013a, 2014a; Thakur et al. 2014). It appears that the 2012 July 23... | [
"Gopalswamy et al. 2010"
] | [
"Particles up to gigaelectronvolt energies are accelerated by strong shocks driven by CMEs of very high speeds (∼2000 km s−1) and intense, soft X-ray flares (see"
] | [
"Background"
] | [
[
878,
900
]
] | [
[
717,
877
]
] |
2017MNRAS.470..755H__Toomre_&_Toomre_1972_Instance_1 | Supermassive black holes (SMBHs) are believed to exist in the centres of all massive galaxies (Kormendy & Richstone 1995). A small proportion of these are growing, with gas accretion rates ranging from ∼10−4 to 10 M⊙ yr−1 and a proportionately wide range of bolometric luminosities (∼1042–1047 erg s−1). These are active... | [
"Toomre & Toomre 1972"
] | [
"Theoretical work suggests major mergers can provide the torque to displace such an overwhelming fraction of the angular momentum of the gas, allowing for the highest accretion rates on to the central black hole whilst transforming the galaxy morphology"
] | [
"Background"
] | [
[
902,
922
]
] | [
[
648,
900
]
] |
2021ApJ...909..173B__Bandiera_&_Petruk_2016_Instance_1 | Taking advantage of modern computer architecture, numerical simulations have become a powerful tool for investigating SNR dynamical evolution by means of testing various scenarios with specific purposes (Ferrand 2020). As relevant observational evidence is steadily growing, particular attention has been devoted to tack... | [
"Bandiera & Petruk 2016"
] | [
"As relevant observational evidence is steadily growing, particular attention has been devoted to tackling with SNR temporal evolution in an inhomogeneous medium, aiming at deciphering the observed asymmetries of emission morphology or clarifying the effects on the synthetic radio polarization maps exerted by vario... | [
"Motivation"
] | [
[
656,
678
]
] | [
[
219,
593
]
] |
2020AandA...639A.116Y__Wenger_et_al._2000_Instance_1 | The main RSG sample contains 1405 candidates from the SMC source catalog. However, targets with Rank 4 and 5 are selected only in one CMD by either the MIST models or the theoretical J − KS color cuts, and many of them reach down close to the tip of the red giant branch (TRGB) and AGB population (see also Figs. 13 and ... | [
"Wenger et al. 2000"
] | [
"In order to make the sample as complete as possible, we retrieved and added all known spectroscopic RSGs in both optical and mid-infrared (MIR) bands from Simbad"
] | [
"Uses"
] | [
[
950,
968
]
] | [
[
787,
948
]
] |
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
]
] |
2015ApJ...809..117Y__Hayasaki_et_al._2008_Instance_1 | Considering a BBH system resulting from a gas rich merger, the BBH is probably surrounded by a circumbinary disk, and each of the two SMBHs is associated with a mini-disk (see Figure 1). In between the circumbinary disk and the inner mini-disks, a gap (or hole) is opened by the secondary SMBH, which is probably the mos... | [
"Hayasaki et al. 2008"
] | [
"This type of geometric configurations for the BBH–disk accretion systems has been revealed by many numerical simulations and analysis"
] | [
"Background"
] | [
[
703,
723
]
] | [
[
523,
656
]
] |
2021AandA...655A..12T__Tang_et_al._2017b_Instance_4 | Using the RADEX3 non local thermodynamic equilibrium (LTE) modeling program (van der Tak et al. 2007) with collisional rate coefficients from Wiesenfeld & Faure (2013), we modeled the relation between the gas kinetic temperature and the measured average of para-H2CO 0.5 × [(322–221 + 321–220)/303–202] ratios, adopting ... | [
"Tang et al. 2017",
"b"
] | [
"Local thermodynamic equilibrium (LTE) is a good approximation for the H2CO level populations under optically thin and high-density conditions"
] | [
"Uses"
] | [
[
1497,
1513
],
[
1515,
1516
]
] | [
[
1331,
1472
]
] |
2018AandA...610A..38F__Bisterzo_et_al._2017_Instance_3 | Similarly to the [α/Fe] ratio, the ratio of the slow (s-) neutron capture process elements to iron can be regarded as a cosmic clock. Ba, Sr, La, and Y are mainly s-process elements produced on long timescales by low mass AGB stars (Matteucci 2012). Since a low mass star must evolve to the AGB phase before the s-proces... | [
"Bisterzo et al. 2017"
] | [
"For comparison, we show in Fig. 13 the predictions of the most recent one",
"where the updated nuclear reaction network was used."
] | [
"Compare/Contrast",
"Background"
] | [
[
2199,
2219
]
] | [
[
2124,
2197
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[
2221,
2273
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2019MNRAS.485L..78V__Chatterjee_et_al._2017_Instance_1 | The properties of the persistent radio source associated with FRB 121102 may be constrained independently of the Faraday-rotating medium. We assume equipartition between the relativistic gas and magnetic field as is common in synchrotron sources3 (Readhead 1994). The source becomes self-absorbed at $1.5$ GHz for radius... | [
"Chatterjee et al. 2017"
] | [
"This is consistent with the ${\\approx } 30\\, {{\\rm per\\, cent}}$ amplitude modulations observed in the source at 3 GHz",
"being caused by refractive interstellar scintillation in the Milky Way interstellar medium"
] | [
"Similarities",
"Similarities"
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[
690,
712
]
] | [
[
570,
688
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[
714,
804
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2020AandA...643A...5D__Saintonge_et_al._2011_Instance_1 | There is significant scatter (larger than 1 dex) among the tdepl measurements in all redshift bins, even though we only consider MS galaxies with ΔMS = ±0.3 dex around the MS parametrization of Speagle et al. (2014). This scatter at a fixed redshift is believed to be a product of the multi-functional dependence of tdep... | [
"Saintonge et al. 2011"
] | [
"The previously reported anti-correlation between tdepl and sSFR",
"is also further supported by our galaxies at z = 4.4 − 5.9 (Fig. 6, middle panel)."
] | [
"Similarities",
"Similarities"
] | [
[
1034,
1055
]
] | [
[
969,
1032
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[
1089,
1171
]
] |
2016MNRAS.461..344P__Bernardi_2009_Instance_2 | The fact that all massive ETGs fall into a single FP, coupled with the segregation of the highest ranked objects from lesser galaxies, entails that any non-edge-on projection of this flat surface must also lead to segregated 2D scaling laws. To investigate this issue we now use M⋆ to represent scale, shifting to the (l... | [
"Bernardi 2009"
] | [
"Our numerical experiments, however, do not seem to support claims of the steepening of the R ∝ Mα relation for CGs towards values α ≳ 1"
] | [
"Differences"
] | [
[
1510,
1523
]
] | [
[
1354,
1489
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] |
2017AandA...599A...4K__hand,_Hotta_et_al._(2016)_Instance_1 | Our results appear to stand apart from similar studies in full spherical shells (e.g., Nelson et al. 2013; Hotta et al. 2016) in that the differential rotation is strongly quenched as a function of the magnetic Reynolds number. However, in Nelson et al. (2013) the values of Rm′ (=2πReM) correspond to a range of 8...32 ... | [
"Hotta et al. 2016"
] | [
"Our results appear to stand apart from similar studies in full spherical shells (e.g.,",
"in that the differential rotation is strongly quenched as a function of the magnetic Reynolds number."
] | [
"Differences",
"Differences"
] | [
[
107,
124
]
] | [
[
0,
86
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[
126,
227
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] |
2022MNRAS.516.5712T__Krumholz_et_al._2015_Instance_1 | As discussed in Section 1, one of the primary motivations for this work is to attempt to understand the variations in apparent IMF that have been observed in early type galaxies (ETGs). While there are multiple lines of evidence for this variation, the most straightforward to extract from out simulations is the mass to... | [
"Krumholz et al. 2015"
] | [
"We calculate this by using the slug stellar population synthesis code"
] | [
"Uses"
] | [
[
619,
639
]
] | [
[
511,
580
]
] |
2020MNRAS.498.4906B__Mehringer_et_al._1992_Instance_1 | The large radiation field directly produced from young stellar objects can exert a significant pressure on the surrounding material. This radiation pressure, Prad, at a given position within an H ii region, is related to the bolometric luminosity, Lbol, of the stellar population and the distance, r, from each star to t... | [
"Mehringer et al. 1992"
] | [
"We use the $\\mathcal {N}_\\mathrm{LyC}$ for each H ii region as determined from the radio observations outlined in Table 2 (i.e.",
"and solve for the direct radiation pressure using equation (4)."
] | [
"Uses",
"Uses"
] | [
[
2806,
2827
]
] | [
[
2654,
2782
],
[
2854,
2917
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] |
2020AandA...637A..59A__Ziurys_et_al._(2018)_Instance_2 | Several molecules show a large discrepancy between the abundances derived from observations and calculated by chemical equilibrium, although it is not as severe as for the molecules discussed above. We refer to PN in O-rich stars and H2S in C-rich stars, which are indicated by hatched rectangles in Fig. 2. For PN in O-... | [
"Ziurys et al. (2018)"
] | [
"However, uncertainties on the observational and theoretical sides mean that the true level of disagreement is unclear. For example, while",
"derived a PN abundance of 10−8 relative to H2 in IK Tau, De Beck et al. (2013) and Velilla Prieto et al. (2017) derived higher abundances, (3–7) × 10−7, in this source."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
660,
680
]
] | [
[
522,
659
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[
681,
849
]
] |
2021AandA...654A..89P__Poutanen_&_Svensson_1996_Instance_1 | We now investigate relativistic reflection models with a primary Comptonisation continuum shape, which is more physical and has a sharper high-energy rollover compared to an exponential cutoff power law. In addition, such models have the advantage of having the hot corona temperature (kThot) as a physical parameter rat... | [
"Poutanen & Svensson 1996"
] | [
"Then, we consider the REFLKERR where the hard X-ray Comptonisation spectrum is computed with the COMPPS model",
"which appears to be a better description of thermal Comptonisation when compared to Monte Carlo simulations"
] | [
"Uses",
"Compare/Contrast"
] | [
[
836,
860
]
] | [
[
725,
834
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[
863,
970
]
] |
2022AandA...664A..45A__Bergh_2000_Instance_1 | We can compare Fig. 14 with the corresponding figure obtained by Mowlavi et al. (2019) in the Magellanic Clouds (see their Figs. 4 and 7 for the LMC and SMC, respectively) and in the Milky Way from DR2 data (their Fig. 10). Our conclusions here are similar: (i) There are far fewer C-rich than O-rich stars in the Galaxy... | [
"van den Bergh 2000"
] | [
"We derive a ratio ∼0.05, which is very similar to the average ratio derived in the disc of M 31 (see e.g."
] | [
"Similarities"
] | [
[
1204,
1222
]
] | [
[
1098,
1203
]
] |
2021MNRAS.507.2115M__Isanto_&_Polsterer_2018_Instance_1 | In astrophysics, the number of studies that apply ML techniques has risen substantially in the last years. Unsupervised learning algorithms have been used to identify different kinematic components of simulated galaxies (Obreja et al. 2018, 2019), to compare stellar spectra (Traven et al. 2017), to classify pulsars (Le... | [
"D’Isanto & Polsterer 2018"
] | [
"Supervised learning has been used",
"and to determine the redshift of galaxies"
] | [
"Background",
"Background"
] | [
[
631,
656
]
] | [
[
404,
437
],
[
557,
598
]
] |
2015MNRAS.450.4364N__Wu_et_al._2004_Instance_1 | Low- and intermediate-mass stars are formed by the gravitational collapse of the parental giant molecular cloud (GMC), followed by the accretion process (Palla 1996). During the accretion phase, material is ejected as well via collimated bipolar jets. However, when a YSO reaches 8 M⊙, the radiative flux becomes so inte... | [
"Wu et al. 2004"
] | [
"This seems to be the case for the outflows driven by young stars from a very broad mass range, as previous reported by several authors"
] | [
"Background"
] | [
[
874,
888
]
] | [
[
651,
785
]
] |
2019MNRAS.483.3022G__Mowlavi_et_al._2018_Instance_1 | LPVs are known to exist on sets of sequences in period–luminosity space (e.g. Wood et al. 1999; Wood 2000) depending on their variability type and pulsation mode. The primary periods of Mira-like variables lie on the commonly called C and C′ sequences (Ita et al. 2004; Spano et al. 2011) with C′ lying at a lower period... | [
"Mowlavi et al. 2018"
] | [
"The left-hand panel of Fig. 2 shows sources from Gaia’s DR2 LPV catalogue",
"chosen to lie within a 15° aperture of the LMC."
] | [
"Uses",
"Uses"
] | [
[
1181,
1200
]
] | [
[
1068,
1141
],
[
1202,
1249
]
] |
2019ApJ...883...88B__Kleint_et_al._2016_Instance_1 | The GALEX NUV observations span a wide wavelength range, from 1771 to 2831 Å. While these data provide no spectral information within that bandpass, we rely on solar and stellar flare studies to inform the likely contributors to the flare flux. The NUV spectral region has not had as many observational constraints as th... | [
"Kleint et al. 2016"
] | [
"Recent results from solar flares observed from space",
"demonstrate an NUV spectrum originating largely from Hydrogen Balmer continuum emission."
] | [
"Background",
"Background"
] | [
[
1256,
1274
]
] | [
[
1179,
1231
],
[
1276,
1364
]
] |
2020ApJ...892...53A__Dudas_et_al._2018_Instance_1 | These new limits, in conjunction with the inconsistency of isotropic flux interpretations, leave no room for an astrophysical interpretation of AAEs in the context of the standard model for time windows as short as 103 s. However, it has been shown that these events can be explained using physics beyond the standard mo... | [
"Dudas et al. 2018"
] | [
"However, it has been shown that these events can be explained using physics beyond the standard model, as many models suggest that AAEs lend support for axionic dark matter, sterile neutrinos, supersymmetry, or heavy dark matter"
] | [
"Compare/Contrast"
] | [
[
499,
516
]
] | [
[
222,
450
]
] |
2020ApJ...899..143C___2016_Instance_1 | Having constrained the estimated CME propagation by matching the observed and modeled fronts in this way, it was then possible to estimate the arrival time and velocity of each CME as it passed Venus and Earth. At Venus, the shock driven by CME-2 caught up with CME-1, showing a typical shock-ICME structure. According t... | [
"Rollett et al.",
"2016"
] | [
"Note that the minimum value of the drag parameters we used here is 1 × 10−9 km s−1, which was revealed as the lowest possible value"
] | [
"Uses"
] | [
[
1823,
1837
],
[
1844,
1848
]
] | [
[
1690,
1821
]
] |
2017ApJ...837..130V__Pasquini_et_al._2008_Instance_1 | From the X-ray point of view, old open clusters are interesting for a number of reasons. First, X-ray observations efficiently detect different classes of close, interacting binaries, enabling the study of processes such as tidal coupling and the link between X-rays and rotation. The X-ray luminosity of late-type stars... | [
"Pasquini et al. 2008"
] | [
"Nevertheless, an early ROSAT observation of the old open cluster M 67, which lies at ∼840 pc"
] | [
"Background"
] | [
[
879,
899
]
] | [
[
785,
877
]
] |
2017MNRAS.464..968S__Tacconi_et_al._2006_Instance_1 | 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"
] | [
"Earlier observations of the physical sizes of SMGs by CO detection and 1.4 GHz imaging suggest larger sizes (e.g."
] | [
"Compare/Contrast"
] | [
[
886,
905
]
] | [
[
772,
885
]
] |
2019MNRAS.482..988C__Zhang_et_al._2016_Instance_1 | The EW(λ8542)/EW(λ8498) values are obtained around ∼1.4 in the first observing night, which are somewhat smaller than the values around ∼1.6 derived in the second night, when a strong optical flare decay was detected (also see the Section 4.2). These low ratios are consistent with the values found for several other sta... | [
"Zhang et al. 2016"
] | [
"These low ratios are consistent with the values found for several other stars with strong chromospheric activity"
] | [
"Similarities"
] | [
[
492,
509
]
] | [
[
245,
357
]
] |
2018MNRAS.473.4566P__Papaderos_et_al._2006_Instance_1 | The young starburst inferred by the detections of high ionization emission line of He II λ4686 and the blue WR bump in this and previous works (Guseva et al. 2000; Brinchmann, Kunth & Durret 2008) is confirmed by the age estimates made here for the bright and faint regions in Mrk 22 as ∼4 and ∼10 Myr, respectively. Unl... | [
"Papaderos et al. 2006"
] | [
"For instance, shallow gradient in metallicity is seen in SBS 0335−052 (",
"while no significant variations were seen in Mrk 35"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1173,
1194
]
] | [
[
1102,
1173
],
[
1196,
1247
]
] |
2018ApJ...863..162M__Liu_et_al._2013_Instance_2 | NLFFF extrapolation provides the reconstructed coronal magnetic field for AR 11158 from 2011 February 13 − 2011 February 15 (Figures 1(d)–(f)). The field lines (yellow lines) within the core of the AR have arcade-like structure with a relatively strong twist mainly near the PIL. These figures show that the magnetic fie... | [
"Liu et al. 2013"
] | [
"However, our result is consistent with other NLFFF results"
] | [
"Similarities"
] | [
[
1352,
1367
]
] | [
[
1257,
1315
]
] |
2021AandA...655A..25Z__Shimizu_et_al._2019_Instance_1 | Outflows are ubiquitous in both luminous AGN and in local Seyfert galaxies, and occur on a wide range of physical scales, from highly ionised semi-relativistic winds and jets in the nuclear region at subparsec scales to galactic scale outflows seen in mildly ionised, molecular, and neutral gas (Morganti et al. 2016; Fi... | [
"Shimizu et al. 2019"
] | [
"In late-type AGN-host galaxies, the gas kinematics appears complex at all scales, showing several components such as bars, rings, and (warped) discs, with high velocity dispersion regions (e.g."
] | [
"Background"
] | [
[
1604,
1623
]
] | [
[
1410,
1603
]
] |
2019ApJ...885...79S__Burrows_et_al._1997_Instance_1 | However, this outward migration of the inner edge should stop at the corotation radius rco, where the Keplerian frequency of the disk equals the spin frequency of Jupiter. When rcav > rco, there will be two possibilities: the angular momentum will be transferred from Jupiter to the disk and then the gas accretion will ... | [
"Burrows et al. 1997"
] | [
"Although the current corotation radius is rco ≈ 2.25 RJ, Jupiter at its time of formation was much larger than it is today",
"and this means that the corotation radius was also larger than the current one if the conservation of the angular momentum of Jupiter is assumed. Considering the transport of the angular ... | [
"Uses",
"Uses"
] | [
[
611,
630
]
] | [
[
487,
609
],
[
654,
951
]
] |
2021ApJ...911...89M__Mozer_et_al._2020a_Instance_1 | Time domain structures (TDSs; electrostatic or electromagnetic electron holes, ion holes, solitary waves, double layers, nonlinear whistlers, etc.) are ∼1 ms pulses having significant electric fields parallel to the background magnetic field (Mozer et al. 2015). They are abundant through space, occurring along auroral ... | [
"Mozer et al. 2020a"
] | [
"TDSs are also expected along the Parker Solar Probe orbit"
] | [
"Background"
] | [
[
875,
893
]
] | [
[
816,
873
]
] |
2022AandA...662A..42M__Nóbrega-Siverio_et_al._2020a_Instance_1 | In this paper, we are interested not only in the mathematical properties of the ambipolar diffusion as a nonlinear diffusion process, but also in the inclusion of ambipolar diffusion terms in MHD codes. In astrophysics, over the past few decades, multidimensional MHD computer codes have been developed that model a vari... | [
"Nóbrega-Siverio et al. 2020a"
] | [
"The consideration of ambipolar diffusion processes in solar physics started many decades ago",
"but it has undergone a true explosion in terms of its use in large numerical models (e.g.",
"Such numerical calculations often encounter a problem: given the comparatively high values of χa in different cosmic envir... | [
"Motivation",
"Motivation",
"Motivation"
] | [
[
1197,
1225
]
] | [
[
747,
839
],
[
860,
949
],
[
1264,
1547
]
] |
2020AandA...643A..35P__Irwin_et_al._2007_Instance_2 | In order to achieve high photometric accuracy and be sensitive to low amplitude undulations, we adopted techniques from the exoplanet community, with the purpose of eliminating the systematic errors. When performing differential photometry (Sect. 3), accurate bias-subtraction and flat-fielding are of major importance. ... | [
"Irwin et al. 2007"
] | [
"For this reason, we obtained a considerable amount of biases (150−300 frames) and twilight flat-fields (25−100 frames) each night to reduce the Poisson noise to less than 0.2 mmag"
] | [
"Uses"
] | [
[
791,
808
]
] | [
[
610,
789
]
] |
2022MNRAS.509.3339K___2011_Instance_1 | Semi-analytical disc models indicate that the frequency of giant planets must increase with the mass of the host star between 0.2–1.5 M⊙ (Ida & Lin 2005; Kennedy & Kenyon 2008). However, this trend is expected to decrease above 1.5 M⊙ due to a smaller growth rate, longer migration time-scale, and shorter lifetime of th... | [
"Johnson et al.",
"2011"
] | [
"However, as rapidly rotating stars evolve off the main sequence they slow down considerably and become much cooler making it relatively easy to search for planets around them. This fact was exploited by dedicated planet searches around intermediate mass sub-giants leading to dozens of planet discoveries"
] | [
"Background"
] | [
[
1004,
1018
],
[
1032,
1036
]
] | [
[
698,
1002
]
] |
2022MNRAS.515..185O__Gutcke_et_al._2022_Instance_1 | While gas cooling and stellar feedback can transform dark matter cusps to cores, it is energetically challenging for this process to create large dark matter cores (typically >500 pc) in the very smallest ‘ultra-faint’ dwarfs, since they form so few stars (M* 105 M⊙; Peñarrubia et al. 2012; Garrison-Kimmel et al. 2013... | [
"Gutcke et al. 2022"
] | [
"Most studies to date find that cusp-core transformations are challenging at the likely mass-scale of UFDs (M200c ∼ 109 M⊙; M* ∼ 105 M⊙; e.g."
] | [
"Compare/Contrast"
] | [
[
905,
923
]
] | [
[
724,
864
]
] |
2018ApJ...854..137S__Manuel_et_al._2014_Instance_1 | Ulysses was launched on 1990 October 6 and orbited the Sun with a latitude varying from −80° to 80° and a solar distance ranging from ∼1 au to ∼5 au (Heber et al. 2009). The Kiel Electron Telescope (KET) on board Ulysses measured electrons in the energy range from ∼3 MeV to above 300 MeV, and protons and helium nuclei ... | [
"Manuel et al. 2014"
] | [
"However, different works used different mono-energetic bins to represent this channel, e.g.,",
"2.5 GV"
] | [
"Differences",
"Differences"
] | [
[
856,
874
]
] | [
[
665,
757
],
[
790,
796
]
] |
2015MNRAS.452.2731S__Stroe_et_al._2013_Instance_4 | The H α studies of Umeda et al. (2004) and Stroe et al. (2014a, 2015) are tracing instantaneous (averaged over 10 Myr) SF and little is known about SF on longer time-scales and the reservoir of gas that would enable future SF. An excellent test case for studying the gas content of galaxies within merging clusters with ... | [
"Stroe et al. 2013"
] | [
"This is probably ram pressure caused by the relative motion of galaxies with respect to the ICM"
] | [
"Background"
] | [
[
2017,
2034
]
] | [
[
1920,
2015
]
] |
2019MNRAS.490.5478W__Kurtovic_et_al._2018_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... | [
"Kurtovic et al. 2018"
] | [
"The influence of tidal truncation is therefore limited to stellar multiples, either in bound systems"
] | [
"Background"
] | [
[
883,
903
]
] | [
[
764,
864
]
] |
2020MNRAS.494.5110B__Troja_et_al._2018_Instance_2 | Following the short gamma-ray burst (sGRB) associated with this event, GRB 170817A (Abbott et al. 2017a,b; Goldstein et al. 2017), radio emission was anticipated as the associated merger outflow interacted with the circum-merger medium. Monitoring the radio emission could therefore provide crucial information on the en... | [
"Troja et al. 2018"
] | [
"The fitted radio spectral index α1 from this study is −0.53 ± 0.04, consistent with broad-band spectral indices determined using radio, optical, and X-ray data at various epochs, where the typical value is approximately −0.58 (e.g."
] | [
"Similarities"
] | [
[
1702,
1719
]
] | [
[
1425,
1656
]
] |
2021ApJ...922..224L__Jain_et_al._2015_Instance_1 | Theoretically, coronal loops are made up of magnetically confined denser and hotter plasma, and can thus support modes of oscillations (Aschwanden 1987; Roberts 2008). These oscillations are closely related to the physical properties of their host coronal loops and may open a new window for detecting the inhomogeneous ... | [
"Jain et al. 2015"
] | [
"Along with an increasing number of observational cases, the study of fast kink oscillations in coronal loops has been significantly advanced"
] | [
"Background"
] | [
[
1318,
1334
]
] | [
[
1058,
1198
]
] |
2017ApJ...837...97L__Grillo_et_al._2015_Instance_1 | The newly discovered arcs and new spectroscopic redshifts have been incorporated into updated HFF+ versions of the Abell 2744 and MACSJ0416.1-2403 lensing models (Table 5); many of these have
(see Figure 8 for a comparison of the arc redshift distributions adopted by the pre-HFF and new HFF+ lensing models; Cypr... | [
"Grillo et al. 2015"
] | [
"see Figure 8 for a comparison of the arc redshift distributions adopted by the pre-HFF and new HFF+ lensing models;"
] | [
"Uses"
] | [
[
577,
595
]
] | [
[
200,
315
]
] |
2022AandA...666A.190S__Velichko_et_al._1995_Instance_1 | For our dataset of absolute magnitudes, we used data collected at the Institute of Astronomy of V. N. Karazin Kharkiv National University within the long-term observational programme to study asteroid magnitude-phase curves (Shevchenko et al. 2010, 2012, 2014a, 2016; Slyusarev et al. 2012). We also used some observatio... | [
"Velichko et al. 1995"
] | [
"We also used some observational data obtained within several other programmes"
] | [
"Uses"
] | [
[
631,
651
]
] | [
[
292,
369
]
] |
2015MNRAS.451.4290S__Governato_et_al._2004_Instance_1 | Hydrodynamical simulations of evolving galaxies allow us to calibrate these diagnostics by measuring their observability given a set of formation scenarios and physical processes (e.g. Jonsson et al. 2006; Rocha et al. 2007; Lotz et al. 2008a; Bush et al. 2010; Narayanan et al. 2010; Hayward et al. 2013; Snyder et al. ... | [
"Governato et al. 2004"
] | [
"It has only recently become widespread to model the formation of galaxies ab initio (e.g."
] | [
"Background"
] | [
[
656,
677
]
] | [
[
566,
655
]
] |
2022MNRAS.515.5495M__Genel_2016_Instance_1 | The stellar metallicity in the Universe evolves with redshift (Mannucci et al. 2010; Sommariva et al. 2012; Krumholz & Dekel 2012; Dayal, Ferrara & Dunlop 2013; Madau & Dickinson 2014). The metallicity at a high redshift (z > 2) is much smaller in comparison to the low redshift Universe z 2. The first-generation stars... | [
"Genel 2016"
] | [
"Currently, a limited number of observations",
"are available to explore the environment dependence of the metallicity, and most of our current understandings are based on simulations"
] | [
"Background",
"Background"
] | [
[
1341,
1351
]
] | [
[
1093,
1136
],
[
1205,
1340
]
] |
2022AandA...664A.127S__Lefebvre_et_al._2008_Instance_1 | Efforts have been made to model the signals caused by different sources of stellar variability within the RV time series (e.g., Tuomi et al. 2013; Rajpaul et al. 2015; Davis et al. 2017; Simola et al. 2019). Several solutions have been successfully proposed in order to deal with stellar oscillations and granulation phe... | [
"Lefebvre et al. 2008"
] | [
"Several solutions have been successfully proposed in order to deal with stellar oscillations and granulation phenomena, such as:",
"using daytime spectra of the Sun in order to measure the solar oscillations (e.g.,"
] | [
"Background",
"Background"
] | [
[
648,
668
]
] | [
[
208,
336
],
[
543,
625
]
] |
2021MNRAS.507.5567D__Guo_et_al._2019_Instance_1 | The source shows some preferred tracks in its movement along the HID. Dips occur as the source is in the SUL regime, either from SUL2 or from SUL3 regions; ingress and egress times populate the D3 and D2 spectra, whereas the D1 spectrum comes from the time segments characterized by the lowest count rate (deep dip). We ... | [
"Guo et al. 2019"
] | [
"This picture is consistent with the observed low temperature, large radius, and super-Eddington luminosity (see"
] | [
"Similarities"
] | [
[
1225,
1240
]
] | [
[
1053,
1164
]
] |
2021MNRAS.500..786D__Delgado_&_Perez_1997_Instance_1 |
xstar predicts O to be progressively ionized through all its possible ionization stages as the central UV-X-ray source is approached providing a natural explanation for the absence of broad forbidden ${[}{\rm O\, \small{III}}{]}$ emission lines. No $[{\rm O\, \small{II}}]\, {\lambda }\, {\lambda }$3727, 3729 emission ... | [
"Delgado & Perez 1997"
] | [
"However, there are two notable discrepancies between the HST observations and the xstar model predictions. The first is that the $[{\\rm O\\, \\small{III}}]\\, {\\lambda }$5008 emission line is observed to be 230 per cent brighter than predicted by xstar. This excess emission could be attributed to the extended so... | [
"Compare/Contrast"
] | [
[
1076,
1096
]
] | [
[
635,
1026
]
] |
2019AandA...621A..27F__DeGraf_et_al._2017_Instance_1 | It is difficult to isolate the impact of mass and environment on the rate and timing of quenching. Mass quenching is more important at earlier times in the evolution of galaxies and may be more important in denser regions (e.g., Peng et al. 2010; Muzzin et al. 2012; Lee et al. 2015; Darvish et al. 2016, 2018; Kawinwani... | [
"DeGraf et al. 2017"
] | [
"Volonteri et al. (2015b) suggest that in the merger phase, the AGN dominates the bolometric luminosity but the accretion can be very stochastic (see also"
] | [
"Background"
] | [
[
725,
743
]
] | [
[
548,
701
]
] |
2021ApJ...919..133P__Ravishankar_et_al._2019_Instance_1 | The inversion of the Fourier transform from limited data is a well-known problem in several imaging domains like, for instance, medical imaging (McGibney et al. 1993; Bronstein et al. 2002; Sutton et al. 2003; Fessler 2007; Gallagher et al. 2008; Lustig et al. 2008), crystallography (Eisebitt et al. 2004; Marchesini et... | [
"Ravishankar et al. 2019"
] | [
"This image reconstruction problem inspired several computational approaches like",
"and machine learning"
] | [
"Background",
"Background"
] | [
[
726,
749
]
] | [
[
400,
480
],
[
686,
706
]
] |
2019MNRAS.485.3600A__Bignall_et_al._2015_Instance_1 | Having eliminated calibration or observational effects as the cause of the spectral changes, it must be that either (1) the configuration of the sources themselves has changed or (2) the interstellar scintillation has caused time-variable focusing and defocusing of the polarized substructure in the radio jets (e.g. Ric... | [
"Bignall et al. 2015"
] | [
"Interstellar scintillation (ISS) is difficult to distinguish from intrinsic variability without fully time-resolved data (see e.g.",
"and references therein), and can coexist with it"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
571,
590
]
] | [
[
440,
570
],
[
591,
639
]
] |
2018AandA...610A..15J__Tregloan-Reed_et_al._2015_Instance_1 | Figure 2 shows the geometry used within our model. The center of the stellar sphere is located at the origin of the three-dimensional spherical coordinate system. PyTranSpot does not take into account a fractional area correction, as used within the WD code (Wilson & Devinney 1971; Wilson 1979, 1990, 2008, 2012). We ar... | [
"Tregloan-Reed et al. 2015"
] | [
"However, to obtain precise photometric transit and spot parameters, we recommend the use of a planetary pixel radius between 15 and 50 pixels"
] | [
"Uses"
] | [
[
599,
624
]
] | [
[
456,
597
]
] |
2022MNRAS.509.5340B__Masci_et_al._2019_Instance_1 | We run forced photometry at these SN locations using a pipeline, hereafter known as the zuds pipeline1 (Dhawan et al. 2021), which performs aperture photometry using the astropy affiliated package PhotUtils (Bradley et al. 2019), using a 6-pixel diameter aperture on the difference images. The reference images for the d... | [
"Masci et al. 2019"
] | [
"From the IPAC forced-photometry service",
"at the same locations, we obtain the metadata for each observation, including the magnitude limit mlim of the observation, the seeing of the observation, and the standard deviation σpix on the background at the pixel on which the SN is located."
] | [
"Uses",
"Uses"
] | [
[
1192,
1209
]
] | [
[
1151,
1190
],
[
1211,
1455
]
] |
2020AandA...634L...8K__Ramos_et_al._2018_Instance_1 | The second data release (DR2) of the ESA Gaia mission has provided the largest available 6D phase-space (positions and velocities) dataset for 7.2 million stars brighter than GRVS = 12 mag (Gaia Collaboration et al. 2018b), making possible precise studies of the Milky Way structure and kinematics on large scales. Gaia ... | [
"Ramos et al. 2018"
] | [
"A large number of kinematic arches with various morphologies not known prior to Gaia were found"
] | [
"Background"
] | [
[
790,
807
]
] | [
[
693,
788
]
] |
2016AandA...588A.132T__Padilla_et_al._2014_Instance_1 | Most of the recent observational efforts to understand galaxy evolution have been focused on determining the history of cosmic star formation, gas density evolution, metallicity evolution, and mass growth of the Universe (Daddi et al. 2004; Mannucci et al. 2010; Madau & Dickinson 2014; Tomczak et al. 2014; Bouwens et a... | [
"Padilla et al. 2014"
] | [
"In parallel, theoretical works and simulations have tried to explain the physical mechanisms that reproduce the measured global properties"
] | [
"Background"
] | [
[
984,
1003
]
] | [
[
768,
906
]
] |
2016ApJ...821..107G__Gloeckler_&_Fisk_2015_Instance_1 | 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... | [
"Gloeckler & Fisk 2015"
] | [
"In Equation (3), ΔE denotes the width of the respective energy bin; for the typical radial velocity of solar wind in the flanks and the downwind hemisphere of the inner heliosheath, we assumed uR = 140 km s−1 as measured by Voyager 2, whereas uR = 40 km s−1 for the heliosheath in the Voyager 1 direction"
] | [
"Uses"
] | [
[
1029,
1050
]
] | [
[
700,
1004
]
] |
2019AandA...630A..37S__Behar_et_al._2017_Instance_1 | Solar wind velocity distribution moments are described in Behar et al. (2017). The ion density nsw is the moment of order 0, and the ion bulk velocity usw (a vector) appears in the moment of order 1, the flux density
$n_{\mathrm{sw}} \ \underline{\mathbf{u}_{\mathrm{sw}}}$
n
sw
u
sw
_
. The bulk speed ... | [
"Behar et al. (2017)"
] | [
"Solar wind velocity distribution moments are described in"
] | [
"Background"
] | [
[
58,
77
]
] | [
[
0,
57
]
] |
2016MNRAS.459.3998L__Blanton_&_Roweis_2007_Instance_1 | In this subsection, we first use our measured CLFs to infer the conditional stellar mass functions and then use the results to study the stellar mass contents of dark matter haloes. To convert luminosity into stellar mass, one typically uses a mass-to-light relation based on galaxy colour (e.g. Bell et al. 2003). This ... | [
"Blanton & Roweis 2007"
] | [
"The constant, 4.64, is the r-band magnitude of the Sun in the AB system"
] | [
"Uses"
] | [
[
1462,
1483
]
] | [
[
1389,
1460
]
] |
2020MNRAS.491.5759H__Dodson-Robinson_&_Salyk_2011_Instance_1 | More recently, Long et al. (2018) performed an analysis on 32 discs in the Taurus star-forming region using ALMA. From this sample 12 discs containing axisymmetric structure were identified. This structure takes the form of dark band bright ring pairs, emission bumps and cavities. Overall 19 gap ring pairs were identif... | [
"Dodson-Robinson & Salyk 2011"
] | [
"Assuming the width of the gaps corresponds to 4RHill"
] | [
"Uses"
] | [
[
907,
935
]
] | [
[
853,
905
]
] |
2017MNRAS.464.4534Q__Schmidt_et_al._2012_Instance_1 | Space missions have traditionally focused on performing spectropolarimetric observations measuring the four Stokes parameters in a narrow spectral window where one or two photospheric absorption lines of interest are present. For instance, see Hinode/SP (Tsuneta et al. 2008; Lites et al. 2013), SDO/HMI (Pesnell, Thomps... | [
"Schmidt et al. 2012"
] | [
"On the contrary, ground-based telescopes usually have instruments which can cover several spectral lines simultaneously, e.g.",
"Gregor/GRIS"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
774,
793
]
] | [
[
430,
555
],
[
739,
750
]
] |
2019ApJ...875..129K__Smith_et_al._2013_Instance_1 | We used the
band high-resolution spectra of Arcturus and μ Leo, obtained with WINERED, to estimate the microturbulence and iron abundance with a precision similar to that of previous results from spectra at different wavelengths. Our lists of Fe i lines in the 0.91–1.33 μm range will be useful for obtaining the ... | [
"Smith et al. 2013"
] | [
"One of the major error sources is the uncertainty in ξ in various studies, including ours, based on spectra at different wavelengths",
"to the H band"
] | [
"Uses",
"Uses"
] | [
[
830,
847
]
] | [
[
611,
743
],
[
798,
811
]
] |
2017AandA...605A..96D__Goździewski_et_al._2016_Instance_1 | In this article, I present an analytical model of resonant chains. Analytical models have already been proposed, in particular to study the dynamics of the Laplace resonance (1:2:4 chain) between Io, Europa, and Ganymede (e.g., Henrard 1983). However, while several numerical studies have been dedicated to the capture o... | [
"Goździewski et al. 2016"
] | [
"Recently, Papaloizou (2015) proposed a semi-analytical model of three-planet resonances taking into account only the interactions between consecutive planets in the chain, with a particular focus on the Kepler-60 system (12:15:20 resonant chain, see also"
] | [
"Background"
] | [
[
788,
811
]
] | [
[
512,
766
]
] |
2021AandA...654A..34B__Grassi_et_al._2014_Instance_1 | The simulations presented in this work have been performed with the publicly available hydrodynamic code GIZMO (Hopkins 2015), which is a descendant of GADGET2 (Springel 2005). The code evolves the magneto-hydrodynamics equations for the gas including a constrained-gradient divergence-cleaning method (Hopkins & Raives ... | [
"Grassi et al. 2014"
] | [
"For the purpose of this study, we equipped the code with an on-the-fly non-equilibrium chemical network, which was implemented via the public chemistry library KROME"
] | [
"Uses"
] | [
[
544,
562
]
] | [
[
377,
542
]
] |
2017ApJ...836..124D__Davenport_et_al._2015_Instance_1 | In Table 3, we list the physical parameters of our model (not including the normalizations for each telescope and each eclipse), and in Tables 4 and 5 we show the resulting best-fit model and the 16th and 84th percentiles (approximately 1σ) for each parameter for each season. We are able to fit our measured light curve... | [
"Davenport et al. 2015"
] | [
"Since the rotation period of the secondary star should not change (and the effect of differential rotation for star spots at different latitudes is small for M dwarfs",
"we conclude that the star-spot signal cannot be originating on the secondary component."
] | [
"Uses",
"Uses"
] | [
[
1005,
1026
]
] | [
[
837,
1003
],
[
1029,
1116
]
] |
2019MNRAS.486.1781R__Fossati_et_al._1998_Instance_1 | Blazars are a peculiar class of active galactic nuclei (AGNs) that have their relativistic jets pointed close to the line of sight to the observer with angle ≤ 10° (Antonucci 1993; Urry & Padovani 1995). They are classified as flat-spectrum radio quasars (FSRQs) and BL Lacerate (BL Lac) objects based on the strength of... | [
"Fossati et al. 1998"
] | [
"The broad-band spectral energy distribution (SED) of blazars is characterized by a two-hump structure, one peaking at low energies in the optical/IR/X-ray region and the other one peaking at high energies in the X-ray/MeV region"
] | [
"Background"
] | [
[
1801,
1820
]
] | [
[
1571,
1799
]
] |
2018MNRAS.475.3419A__Davis_et_al._1999_Instance_1 | 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"
] | [
"One possibility to solve this issue is that the potential Psyche asteroid family was created at an early time, e.g. within the first 500 Myr of Solar system history",
"This would allow the family fragments to be ground down by collisional evolution and be unobservable today. The same models show that, even in th... | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1531,
1548
]
] | [
[
1365,
1529
],
[
1551,
1815
]
] |
2019AandA...627A.173V__Epstein_et_al._(2014)_Instance_1 | Since the age determination using asteroseismology relies on the mass-age relation that red giants follow, this means that the method is biased by any event that changes the stellar mass, such as mass accretion from a companion or stellar mergers (blue stragglers or stars rejuvenated by accretion, e.g. Boffin et al. 20... | [
"Epstein et al. (2014)"
] | [
"The first study to determine masses for a sample of metal-poor halo giants with both seismic information",
"and chemistry from high-resolution APOGEE",
"spectra, was by",
"The authors used scaling relations at face value and reported masses larger (M > 1 M⊙) than what would be expected for a typical old pop... | [
"Background",
"Background",
"Background",
"Background",
"Similarities",
"Background"
] | [
[
973,
994
]
] | [
[
752,
856
],
[
892,
933
],
[
957,
972
],
[
996,
1141
],
[
1142,
1252
],
[
1253,
1363
]
] |
2016AandA...589A..73R__Kurucz_1992_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... | [
"Kurucz 1992"
] | [
"Theoretical stellar libraries like, e.g. BaSeL",
"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."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
770,
781
]
] | [
[
722,
768
],
[
884,
1049
]
] |
2020MNRAS.492..821C__Masters_et_al._2014_Instance_1 | As a general remark, whether the locally calibrated metallicity diagnostics are applicable to high-redshift galaxies is still a matter of great debate. Diagnostics that are expected to be little affected by the ionization conditions of the gas (see e.g. Dopita et al. 2016) have been suggested to be valuable for high-re... | [
"Masters et al. 2014"
] | [
"However, since such diagnostics usually involve the [N ii]/[O ii] or the [N ii]/[S ii] line ratios, they are strongly dependent on the assumed relation between the N/O ratio as a function of the oxygen abundance O/H, which is affected by a large scatter and whose evolution with cosmic time and/or dependence on gal... | [
"Compare/Contrast"
] | [
[
1185,
1204
]
] | [
[
745,
1183
]
] |
2020AandA...637A..44N__Kerszberg_et_al._2017_Instance_1 | Among the existing IACT systems, HESS has the largest FoV and hence provides the highest sensitivity for the diffuse γ-ray flux. Its electron spectrum analysis technique could be directly used to obtain a measurement of the diffuse Galactic γ-ray flux above energies of several TeV in the Galactic Ridge (|l| 30°, |b| ... | [
"Kerszberg et al. (2017)"
] | [
"This is illustrated in Fig. 5, where thick blue and red data points show mild high-energy excesses of the electron spectra derived by Kraus (2018),",
", Kerszberg (2017) over broken power-law models derived from the fits to lower energy data."
] | [
"Uses",
"Uses"
] | [
[
634,
657
]
] | [
[
486,
633
],
[
657,
748
]
] |
2019ApJ...887...26O__Garon_et_al._2019_Instance_1 | In an effort to understand the character of RG encounters with ICM shocks and the observable consequences, we have initiated an MHD simulation study of such interactions. The simulations include passive, but energy-dependent transport of CRe, so that resulting radio synchrotron properties can be modeled appropriately. ... | [
"Garon et al. 2019"
] | [
"NATs, which are especially common in clusters, (e.g.,",
"result from sustained relative motion between an RG and its ambient ICM; that is, the RG effectively evolves in a wind that deflects the RG jets and their discharge downwind."
] | [
"Background",
"Background"
] | [
[
597,
614
]
] | [
[
522,
575
],
[
616,
790
]
] |
2016ApJ...826..106G__Mazzarella_et_al._2012_Instance_1 | The galaxy merging process can cause enhanced accretion onto the central SMBHs and thus initiate activity. One or both of the dual SMBHs may be active or re-activated. Simulations (e.g., Van Wassenhove et al. 2012) suggest that simultaneous activity is mostly expected at the late phases of mergers, at or below 10 kpc s... | [
"Mazzarella et al. 2012"
] | [
"The number of convincing dual AGN systems, mostly detected by X-ray and radio observations (e.g.,",
"are relatively few compared to the theoretically predicted abundance"
] | [
"Differences",
"Differences"
] | [
[
856,
878
]
] | [
[
609,
706
],
[
949,
1017
]
] |
2021MNRAS.503.2973C__Carvalho_et_al._2020_Instance_1 | As a first approximation, we consider that most part of the accretion luminosity is emitted in the soft X-ray spectrum (10 eV–10 keV), thus, soft X-ray luminosity is simply estimated by using the mass accretion parameter, $\dot{m}$(1)$$\begin{eqnarray*}
L_{\rm AC}= \frac{GM\dot{m}}{R},
\end{eqnarray*}$$where M and R ... | [
"Carvalho et al. 2020"
] | [
"Mass–radius relation is employed to estimate radius in case of white dwarfs and neutron stars (see e.g."
] | [
"Uses"
] | [
[
658,
678
]
] | [
[
437,
540
]
] |
2019MNRAS.484.3785B__Huchra_&_Sargent_1973_Instance_1 | Once we have the completeness corrections, we can estimate the relative luminosity function of SNe Ia, which we show in Fig. 3. In the left panel we show the observed distribution of absolute magnitudes. The black histogram shows the full sample, and the red histogram shows the volume-limited sample; the dot--dashed bl... | [
"Huchra & Sargent 1973"
] | [
"We convert the ASAS-SN distributions into estimates of the true luminosity function using the V/Vmax method"
] | [
"Uses"
] | [
[
647,
668
]
] | [
[
524,
631
]
] |
2016AandA...592A..19C__Davies_et_al._1993_Instance_1 | The downsizing scenario is evident in several cases of galaxy evolution (Fontanot et al. 2009). In the case of ETGs at z ~ 0, one of the first pieces of observational evidence can be referred to the studies of Dressler et al. (1987), Faber et al. (1992) and Worthey et al. (1992), who found more massive elliptical galax... | [
"Davies et al. 1993"
] | [
"Subsequent studies found the same trend of [α/Fe] with mass",
"leading to the dominant interpretation that in more massive ETGs, the duration of star formation was substantially shorter than in less massive ones, with timescales short enough (e.g. 0.5 Gyr) to avoid the dilution of the α element abundance (produc... | [
"Background",
"Background"
] | [
[
650,
668
]
] | [
[
564,
623
],
[
739,
1165
]
] |
2017AandA...604A.112G__Hansen_2010_Instance_1 | In stars, there are two components to describe the tidal interaction, equilibrium tides and dynamical tides. Equilibrium tides correspond to a large-scale hydrostatic adjustment of a body and the resulting flow due to the gravitational field of a given companion (Zahn 1966; Remus et al. 2012). It is usually employed in... | [
"Hansen 2010"
] | [
"In this model, the dissipation of the kinetic energy of the equilibrium tide inside the star is often taken to be constant throughout the system evolution and calibrated on observations"
] | [
"Background"
] | [
[
769,
780
]
] | [
[
582,
767
]
] |
2016ApJ...827..104S__Risaliti_&_Lusso_2015_Instance_1 | Using these quasar survey data, Clowes et al. (2013), Nadathur (2013), Einasto et al. (2014), and Park et al. (2015) found very large quasar groups and discussed the cosmological implications of the existence and properties of these extreme objects. Nadathur (2013), Einasto et al. (2014), and Park et al. (2015) pointed... | [
"Risaliti & Lusso 2015"
] | [
"The quasar survey data are also used for studies to constrain cosmological parameters"
] | [
"Background"
] | [
[
914,
935
]
] | [
[
810,
895
]
] |
2018MNRAS.481..533L__Ilić,_Kovačević_&_Popović_2009_Instance_1 | We refer to models for which the pressure P depends on the radial distance r from the central continuum source,
(2)
\begin{eqnarray*}
P(r)\propto r^{-s} \, ,
\end{eqnarray*}
as pressure-law models. In this work, we examine two limiting cases, s = 0 and s = 2, representing constant density and constant ionization ... | [
"Ilić, Kovačević & Popović 2009"
] | [
"We make the simplifying assumption that the cloud temperature does not vary with radius; for solar composition, photoionization equilibrium is achieved at temperatures T ∼ 104 K across a wide range of ionization parameter (equation 5), and the gas temperature will therefore vary weakly with radius (e.g."
] | [
"Uses"
] | [
[
1217,
1247
]
] | [
[
899,
1203
]
] |
2018AandA...614A..66S__Jiang_et_al._2008_Instance_1 | Virtually all formulas that are currently used to estimate the merger time, τmer, are based on the idealised Chandraseckhar (1943) description of the deceleration caused by dynamical friction on a point mass (representing the satellite) travelling through an infinite, uniform, and collisionless medium (representing the... | [
"Jiang et al. 2008"
] | [
"or parametric equations tuned by direct comparison with the outcome of numerical simulations of collisions of live galaxy pairs (e.g."
] | [
"Background"
] | [
[
713,
730
]
] | [
[
551,
684
]
] |
2018MNRAS.477L..80K__Colella_&_Woodward_1984_Instance_1 | The numerical schemes in this work are essentially the same as those in Kuroda et al. (2016). Regarding the metric evolution, we evolve the standard BSSN variables (Shibata & Nakamura 1995; Baumgarte & Shapiro 1999; Marronetti et al. 2008) with a finite-difference scheme in space and with a Runge–Kutta method in time, ... | [
"Colella & Woodward 1984"
] | [
"Regarding the radiation-hydrodynamic evolution, the conservation equation $\\Delta_\\alpha T^{\\alpha \\beta }_{\\rm (total)}=0$ is solved using the piecewise parabolic method"
] | [
"Uses"
] | [
[
608,
631
]
] | [
[
436,
606
]
] |
2016MNRAS.457..212S__Singh,_Sami_&_Dadhich_2003_Instance_1 | One of the first and simplest proposed Friedmann–Robertson–Walker (FRW) cosmological model is the Λ cold dark matter (ΛCDM) universe, which involves Einstein's cosmological constant Λ. This standard model of cosmology, which is also referred to as the concordance model, assumes that the total energy density ρ of the un... | [
"Singh, Sami & Dadhich 2003"
] | [
"Other sources of dark energy include scalar fields such as",
"and phantom fields"
] | [
"Background",
"Background"
] | [
[
3218,
3244
]
] | [
[
3061,
3119
],
[
3198,
3216
]
] |
2020ApJ...893..124Z___2017_Instance_1 | The terrestrial magnetosheath, downstream of the bow shock generated by the interaction between the supersonic solar wind and the Earth’s magnetosphere, is representative of turbulence downstream of collisionless plasma shock in the universe. Usually, the downstream sheath regions have larger density, temperature, mean... | [
"Huang et al.",
"2017"
] | [
"Usually, the downstream sheath regions have larger density, temperature, mean magnetic intensity, and compressibility, and higher plasma β, as compared to the upstream solar wind"
] | [
"Background"
] | [
[
482,
494
],
[
501,
505
]
] | [
[
243,
421
]
] |
2019ApJ...870...70S__Bosch_2016_Instance_1 | The large differences noted in Figure 9 are surely related to the different approximations underlying both the complex hydrodynamical simulations of ILLUSTRIS-1 and our simplified approach. As recently discussed by Chua et al. (2017), the distribution of noncollisional matter (i.e., stars and DM) can effectively cool d... | [
"Jiang & van den Bosch 2016"
] | [
"The large differences noted in Figure 9 are surely related to the different approximations underlying both the complex hydrodynamical simulations of ILLUSTRIS-1 and our simplified approach.",
"A key role is also played by the host cluster itself, because the mass profile of this latter becomes steeper and steepe... | [
"Compare/Contrast",
"Compare/Contrast",
"Compare/Contrast"
] | [
[
958,
984
]
] | [
[
0,
189
],
[
618,
957
],
[
987,
1189
]
] |
2022AandA...663L...4L___2020_Instance_2 | While previous studies mainly focused on the optical-UV properties of a MAD in RLAGNs, for the first time we try to investigate their X-ray properties in this work. The origin of X-ray emission in RLAGNs is still under debate, which may come from a corona, jet, or both. In observations, there is a big difference betwee... | [
"Gupta et al.",
"2020"
] | [
"The sample of",
"was X-ray selected (and optically selected for the sample of Zhu et al. 2021), which may lead to the radio jet power being very feeble compared to the bolometric luminosity in most of the RLAGNs."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1579,
1591
],
[
1599,
1603
]
] | [
[
1565,
1578
],
[
1605,
1800
]
] |
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