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 |
|---|---|---|---|---|---|---|
2017MNRAS.470..755H__Cox_et_al._2008_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... | [
"Cox et al. 2008"
] | [
"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"
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[
1006,
1021
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[
648,
900
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2018MNRAS.473.1633K__Fremling_et_al._2014_Instance_1 | Kochanek (2009) examined the statistical properties expected for surviving binary companions to SNe assuming passively evolving systems (i.e. no binary interactions). As already noted, the companions are generally significantly fainter than the exploding star, although this is frequently not the case for stripped SN pr... | [
"Fremling et al. 2014"
] | [
"As already noted, the companions are generally significantly fainter than the exploding star, although this is frequently not the case for stripped SN progenitors – for Type Ibc SNe, it should not be surprising to find that the binary companion is more visually luminous than the SN progenitor. This point is of con... | [
"Background"
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[
622,
642
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[
167,
553
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2022MNRAS.509..693R__Foreman-Mackey_et_al._2013_Instance_1 | We detect 1.33 mm continuum extended emission originating from HD 36546 (see Fig. 3). Peak and integrated flux, size, and inclination are reported in Table 2. Once deconvolved from the beam, the major axis of the disc spans 180 au, compatible with the size reported from scattered light observations (semimajor axis of 8... | [
"Foreman-Mackey et al. 2013"
] | [
"In order to estimate a temperature for the dust, we have fitted a modified blackbody to the available photometry at wavelengths longer than 10 µm (AKARI, WISE, IRAS, Herschel)3 and the new ALMA photometry using the emcee Affine Invariant Markov chain Monte Carlo Ensemble sampler implementation"
] | [
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] | [
[
1168,
1194
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[
872,
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]
] |
2016AandA...591L...7B__Kruit_(1994)_Instance_1 | We created 10 000 3D models of galaxies, each with an exponential disc plus a Sérsic bulge. We adopted the following functional form for the exponential disc (López-Corredoira et al. 2002): (1)\begin{equation} \label{eq:Corredoira} \rho(R,z)=\rho_{\mathrm{0}}\cdot\exp{\Bigg(\frac{-R}{h_{R}}\Bigg)}\cdot \exp{\Bigg(\fra... | [
"de Jong & van der Kruit (1994)"
] | [
"Graham (2001) analysed a sample of 86 face-on disc-dominated galaxies previously selected by"
] | [
"Uses"
] | [
[
890,
920
]
] | [
[
797,
889
]
] |
2017MNRAS.464..183N__Biviano_&_Katgert_2004_Instance_1 | Other important result we reported in Section 3.3 is the reversing behaviour of red and blue galaxies with respect to velocity and groupcentric distances segregation, with redshift. Regarding velocity segregation, the preceding paragraph provides a qualitative scenario. Now, to explain the spatial segregation, we shoul... | [
"Biviano & Katgert 2004"
] | [
"hus, both survival and replenishment of galaxies should be expected over the time, and two important factors come into play: (i) the accretion rate of galaxies; and (ii) the orbital dependence of galaxy properties (e.g."
] | [
"Uses"
] | [
[
830,
852
]
] | [
[
610,
829
]
] |
2021ApJ...914L..19Z__McKernan_et_al._2012_Instance_1 | Massive stars are believed to exist in the accretion disks of active galactic nuclei (AGNs). Such AGN stars and compact objects can be either the result of in situ formation inside the accretion disk or be captured from the nuclear star clusters around the AGNs (e.g., Artymowicz et al. 1993; Collin & Zahn 1999; Goodman... | [
"McKernan et al. 2012"
] | [
"The disk of an AGN provides a natural environment for stars and compact objects to accrete materials and to migrate within it (e.g.,"
] | [
"Background"
] | [
[
1050,
1070
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] | [
[
917,
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2015MNRAS.453.3414A__the_1999_Instance_1 | Filippenko & Chornock (2001) first presented the dynamical estimate of mass of the source to be around 7.4 ± 1.1 M⊙. Recently, Radhika & Nandi (2014) claimed that the mass of XTE J1859+226 is perhaps in between 6.58 and 8.84 M⊙ which is similar to the prediction of Shaposhnikov & Titarchuk (2009), although the lower ma... | [
"Radhika & Nandi (2014)"
] | [
"Recently,",
"claimed that the mass of XTE J1859+226 is perhaps in between 6.58 and 8.84 M⊙ which is similar to the prediction of Shaposhnikov & Titarchuk (2009)",
"although the lower mass limit is estimated as 5.4 M⊙ by Corral-Santana et al. (2011)."
] | [
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[
127,
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[
299,
384
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2017AandA...607A..71G__Hansen_&_Oh_(2006)_Instance_1 | An implication of the respective escape fractions of the two regimes is visible in Fig. 12. Here we show several values of NHI,cl for the static setup using τd,cl = 10-4 (empty symbols) and τd,cl = 1 (filled symbols), which correspond to metallicities of \hbox{$Z/Z_\odot = 0.63\left(\tau_{\rm d}/10^{-4}\right)\left(10^... | [
"Hansen & Oh (2006)"
] | [
"Also shown in Fig. 12 (with a black [gray] solid line for the low [high] dust content) is the proposed analytic solution for fesc by",
"(18)\\begin{equation} f_{\\rm esc}^{\\rm HO06} = 1/{\\rm cosh}(\\!\\sqrt{2 N_{\\cl}\\epsilon}), \\label{eq:fescHO06} \\end{equation}fescHO06=1/cosh(2Nclϵ),where for Ncl we used ... | [
"Uses",
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[
733,
751
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[
600,
732
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[
751,
1197
]
] |
2020MNRAS.498.5299M__Bernardeau,_Waerbeke_&_Mellier_2003_Instance_1 | From the early days of detection the weak lensing (Munshi et al. 2008) studies have matured to a point where weak lensing results from Euclid are expected to constrain the cosmological parameters to sub-per cent accuracy. However, weak lensing at smaller angular scales probes the non-linear regime of gravitational clus... | [
"Bernardeau, Waerbeke & Mellier 2003"
] | [
"Early studies concentrated on measurements of higher order correlation hierarchy in the angular space due to small survey size"
] | [
"Background"
] | [
[
1441,
1476
]
] | [
[
1271,
1397
]
] |
2019MNRAS.485.2235B__Schmalzing_&_Buchert_1997_Instance_1 | Analyses of 21-cm signals are mainly based on traditional N-point correlation statistics. Beyond the simplest two-point function (power spectrum), higher-order correlations are quite non-trivial to calculate and sometimes they suffer from conceptual challenges. On the other hand, the Minkowski functionals (MFs) are ext... | [
"Schmalzing & Buchert 1997"
] | [
"On the other hand, the Minkowski functionals (MFs) are extremely useful tools in quantitatively describing the morphology because, in principle, they contain information on all the higher-order moments.",
"Since then they have been extensively employed to study the morphology of the large-scale structure of the ... | [
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2018ApJ...867...55X__Acero_et_al._2015_Instance_1 | During the likelihood analysis, the normalizations and spectral parameters of all sources within 5° of 3FGL J1640.4-4634c, as well as the normalizations of the two diffuse backgrounds, are left free. First, we create a Test Statistic (TS) map by subtracting the emission from the sources and backgrounds in the best-fit ... | [
"Acero et al. 2015"
] | [
"Next, we adopt the position of 3FGL J1640.4-4634c provisionally provided by the 3FGL catalog"
] | [
"Uses"
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[
731,
748
]
] | [
[
637,
729
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] |
2020AandA...637A..44N__Kraus_(2018)_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| ... | [
"Kraus (2018)"
] | [
"This is illustrated in Fig. 5, where thick blue and red data points show mild high-energy excesses of the electron spectra derived by",
"Kerszberg et al. (2017), Kerszberg (2017) over broken power-law models derived from the fits to lower energy data."
] | [
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"Uses"
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[
620,
632
]
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[
486,
619
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[
634,
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2020MNRAS.495.4845C__Bernardi_et_al._2016_Instance_1 | The exploration of the Universe out to times earlier than the point of complete reionization is rapidly advancing. One of the most informative probes of these epochs is the 21-cm line produced by hydrogen atoms in the neutral intergalactic medium (IGM) at redshifts z > 6. This line redshifts to frequencies below 200 MH... | [
"Bernardi et al. 2016"
] | [
"Other global 21-cm experiments, including the Large-Aperture Experiment to Detect the Dark Ages",
"provide upper limits on the signal from Cosmic Dawn and the Epoch of Reionization (EoR), ruling out some extreme astrophysical scenarios."
] | [
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2018AandA...610A..61P__Glampedakis_et_al._2006_Instance_1 | It was soon realized that these frequencies are probably related to oscillations of the neutron star, and several groups tried to identify them as elastic oscillations of the crust (Duncan 1998; Messios et al. 2001; Strohmayer & Watts 2005; Piro 2005; Sotani et al. 2007; 2013, 2016; Samuelsson & Andersson 2007, 2009; S... | [
"Glampedakis et al. 2006"
] | [
"It was soon realized that these frequencies are probably related to oscillations of the neutron star, and several groups tried to identify them as",
"Alfvén oscillations"
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2020ApJ...893...54Y___2021_Instance_1 | The polarimetric observations with ALMA at 0.87 mm toward B335 were conducted during 2016 to 2018, consisting of 13 successful executions (project code: 2015.1.01018.S). In the observations, 40–47 antennae were used in the configurations with baseline lengths ranging from 15 to 1400 m. The pointing center was α(J2000) ... | [
"McMullin et al. 2007"
] | [
"The data were manually calibrated by the EA ARC node using the Common Astronomy Software Applications (CASA) of the version 5.1.1"
] | [
"Uses"
] | [
[
977,
997
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[
846,
975
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2021ApJ...922..140R__Hughes_et_al._1998_Instance_1 | We fit the total foreground absorption column by applying two-component multiplicative absorption models, tbabs and tbnew.
8
8
https://pulsar.sternwarte.uni-erlangen.de/wilms/research/tbabs/
The absorption component tbabs accounts for the Galactic absorption column N
H,Gal, and it is fixed at N
H,Gal = 6 × 1020 cm−... | [
"Hughes et al. 1998"
] | [
"Recent measurements of the LMC abundances based on the X-ray spectral analysis of SNRs",
"suggest ∼50% lower LMC abundance values for O, Ne, Mg, and Fe than the previously estimated values",
"Our derived shock parameters are consistent (within statistical uncertainties), assuming either set of these LMC abunda... | [
"Differences",
"Differences",
"Differences"
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[
847,
865
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[
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705
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[
868,
1001
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2021MNRAS.506.3313G__Bluck_et_al._2014_Instance_1 | The B/T ratio of a galaxy is the fraction of total luminosity contributed by the bulge component of the galaxy. Bulges are the central component of disc galaxies which appear as central bright cores in galaxy images or as excess-light over the disc light in the inner region of galaxy light profiles. The B/T ratio is an... | [
"Bluck et al. 2014"
] | [
"The B/T ratio is an important indicator of galaxy structure and is well correlated with several other physical quantities of interest in studies of galaxy evolution, such as",
"stellar mass, and star formation rate"
] | [
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301,
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554,
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2019ApJ...887..174V__Barkana_&_Loeb_2001_Instance_1 | Supermassive black holes (SMBH) with masses M• ∼ 109–1010
are recognized to be present at redshifts as high as z ≃ 6–7.5, when the universe was 650–800 Myr young (Fan et al. 2003; Willott et al. 2010; Mortlock et al. 2011; Bañados et al. 2014, 2018; Wu et al. 2015; Decarli et al. 2018; Izumi et al. 2019)—in total... | [
"Barkana & Loeb 2001"
] | [
"In this scenario SMBHs have to begin growing even earlier than the very first stars are assumed to have appeared (see discussion in"
] | [
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[
1150,
1169
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[
1018,
1149
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2018MNRAS.476.2591V__Patton_et_al._2016_Instance_1 | Galaxy interactions represent a fundamental component of our current view of hierarchical galaxy evolution. Studies based on both observations and simulations have shown that galaxy collisions and mergers can dramatically affect the galaxies undergoing the interaction, by, e.g. triggering nuclear activity (e.g. Kennicu... | [
"Patton et al. 2016"
] | [
"Studies based on both observations and simulations have shown that galaxy collisions and mergers can dramatically affect the galaxies undergoing the interaction, by, e.g.",
"disrupting morphologies (e.g."
] | [
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[
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108,
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520,
549
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2021MNRAS.505..435S___2020_Instance_1 | Detections of ionic, atomic, and molecular species in exoplanetary atmospheres serve as a unique and strong diagnostic of those chemical and dynamical processes driving their formation and evolution. Their detection and abundance measurements could act as indicators of planetary formation scenarios and reveal connectio... | [
"Hoeijmakers et al.",
"2020"
] | [
"A whole host of ions, atoms, and molecules have been detected through a variety of, often complementary, techniques,",
"and high resolution spectroscopic techniques (e.g."
] | [
"Background",
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1343,
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880,
996
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1193,
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2020MNRAS.497.3504T__Migliori_et_al._2017_Instance_1 | Galactic BHXBs offer excellent laboratories in which to study jet interaction zones, as their jets evolve on day to month time-scales, they are located at nearby distances, and they are thought to be good analogues for AGNs. Given their incredible diagnostic potential, over the last couple of decades there have been ma... | [
"Migliori et al. 2017"
] | [
"To date, several candidate jet–ISM interaction sites have been identified;",
"XTE J1550–564",
"From these past works, it is clear that finding and confirming interaction sites can be incredibly difficult and often observationally expensive (e.g. requiring deep, wide-field radio continuum observations)."
] | [
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1346,
1554
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2020MNRAS.499.4158G__Fialkov_&_Loeb_2016_Instance_1 | In 2018, a deep spectral feature centred at 78 MHz was reported by the EDGES collaboration (Bowman et al. 2018). The feature was presented as the long sought-after 21-cm absorption feature seen against the CMB during the CD at z ∼ 17. The location of this putative absorption trough is consistent with redshift predictio... | [
"Fialkov & Loeb 2016"
] | [
"However, the depth of the feature is ΔT21 ∼ 0.5 K ($99{{\\ \\rm per\\ cent}}$ confidence level), which is two to three times stronger and considerably wider (Δν ∼ 19 MHz) than that predicted by the most optimistic astrophysical models (e.g."
] | [
"Differences"
] | [
[
768,
787
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] | [
[
475,
712
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] |
2018MNRAS.479.3254V___2000_Instance_2 | The lifetime of molecular clouds (MCs) remains an active research topic in the study of the interstellar medium and star formation, and most recent studies, both observational and theoretical, place this lifetime at a few times 107 yr for clouds in the 105–106M⊙ mass range (e.g. Blitz & Shu 1980; Kawamura et al. 2009; ... | [
"Palla & Stahler",
"2000"
] | [
"Vázquez-Semadeni, González-Samaniego & Colín (2017) have recently shown that the simulations of Colín et al. (2013) in fact produce stellar age histograms highly resemblant of the observed ones"
] | [
"Similarities"
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[
2092,
2107
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[
2114,
2118
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[
1897,
2090
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2017MNRAS.469.3108C__Diamond-Stanic_et_al._2012_Instance_1 | Still unconstrained are the mechanisms that are able to modify both SF and morphology and their corresponding time-scales. Several hypotheses have been proposed to explain the quenching of the SF in blue galaxies, such as gas stripping (e.g. Gunn & Gott 1972), morphological or gravitational quenching (Martig et al. 200... | [
"Diamond-Stanic et al. 2012"
] | [
"Moreover, in massive galaxies, the role of AGNs in influencing galaxy evolution and quenching SF is supported by several observations"
] | [
"Background"
] | [
[
672,
698
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[
495,
628
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] |
2022MNRAS.517.1218L__Barnes_&_Hernquist_1996_Instance_1 | Several consortia have been actively approaching the question based on large photometric and spectroscopic surveys such as 2dF and SDSS, covering large sky areas and redshift ranges (Lewis et al. 2002; Balogh et al. 2004; Kauffmann et al. 2004; Poggianti et al. 2017). All these efforts have found indisputable evidence ... | [
"Barnes & Hernquist 1996"
] | [
"On the other side, we have the tidal (gravitational) mechanisms occurring",
"or among neighbour galaxies"
] | [
"Background",
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[
1132,
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[
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[
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1116
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2021ApJ...920L..31N__Sterling_et_al._2017_Instance_1 | But if, as our studies in this Letter indicate, microstreams might be the result of accumulated and persistent velocity enhancements resulting from a series of switchbacks, then it could be that individual switchbacks result from coronal jets, and the microstreams are a consequence of a series of such jet-driven switch... | [
"Sterling et al. 2017"
] | [
"In fact, homologous jets, continuing for hours at a time, have been commonly observed (e.g.,"
] | [
"Background"
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719,
739
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[
557,
649
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] |
2017ApJ...839...56T___2013_Instance_2 | Mid-infrared and millimeter polarimetric observation has so far been considered as the best method to probe the magnetic field. This is because if aspherical grains in disks become aligned with the magnetic field as is the case in the interstellar medium (ISM), the polarization vector arising from thermal emission of t... | [
"Hughes et al.",
"2013"
] | [
"More evolved disks do not show a degree of linear polarization larger than 0.5%"
] | [
"Background"
] | [
[
1143,
1156
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[
1163,
1167
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[
1062,
1141
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2019MNRAS.487..475C__Ward-Thompson_et_al._2009_Instance_2 | We attempted to find a correlation between the mean magnetic field and the outflow and minor axis of the cloud CB 17. Relative orientations between various quantities of CB 17 are presented in the first row of Table 6, along with a comparative study of the same for some dark clouds. The first column gives the cloud ID ... | [
"Ward-Thompson et al. 2009"
] | [
"and a similar phenomenon has also been observed in the case of",
"CB 3"
] | [
"Similarities",
"Similarities"
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[
2811,
2836
]
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[
2643,
2705
],
[
2805,
2809
]
] |
2019MNRAS.487.1210T__McNamara_&_Nulsen_2007_Instance_1 | On larger scales, the clusters in which BCGs reside can generally be divided into two categories: cool core clusters, which exhibit very peaked surface brightness distributions at X-ray wavelengths, and non cool core clusters, with similar overall X-ray luminosities but with smoother, less peaked X-ray surface brightne... | [
"McNamara & Nulsen 2007"
] | [
"Since cool core clusters have short radiative cooling time-scales on the order of 108 yr in their centres (e.g.",
"starbursts are expected to be common at the centre of such clusters."
] | [
"Uses",
"Uses"
] | [
[
606,
628
]
] | [
[
473,
584
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[
668,
736
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2022MNRAS.515.1942D___2022b_Instance_1 | Comparison of 1D marginal posterior distributions over the parameters S8 ≡ σ8(Ωm/0.3)0.5, σ8 and Ωm, from DES Y3 data as well as other experiments, and consistency tests for this work (in blue). (a) Constraints obtained from the harmonic (this work) and real (Amon et al. 2022; Secco et al. 2022) space analyses of DES Y... | [
"Hamana et al.",
"2022b"
] | [
"Comparison of 1D marginal posterior distributions over the parameters S8 ≡ σ8(Ωm/0.3)0.5, σ8 and Ωm, from DES Y3 data as well as other experiments, and consistency tests for this work (in blue).",
"Constraints from other weak lensing surveys, namely HSC Y1",
"are shown in grey"
] | [
"Compare/Contrast",
"Compare/Contrast",
"Compare/Contrast"
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[
532,
545
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[
552,
557
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[
0,
194
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452,
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654,
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2018AandA...614A..56B__Chung_et_al._2007_Instance_1 | The studies of emission lines, however, which for wide-field cameras require specific and expensive narrow-band (NB) filters of large physical size, have thus far been limited to pointed observations. Very deep Hα observations of a few galaxies in nearby clusters, including our recent observations with MegaCam, have le... | [
"Chung et al. 2007"
] | [
"They have shown that the ionised phase appears to be an ideal tracer of stripped gas in dense regions: approximately 50% of late-type galaxies show extended (~50 kpc) tails of ionised gas with surface brightness Σ(Hα) of approximately a few 10−18 erg s−1 cm−2 arcsec−2",
"while only a handful of galaxies have ext... | [
"Background",
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[
726,
743
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[
357,
625
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[
652,
724
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2022MNRAS.513.4361M__Zdziarski,_Johnson_&_Magdziarz_1996_Instance_1 | The relxillDCp model combines the ionized disc reflection code xillverDCp (García et al. 2013, 2016) with the convolution model relconv (Dauser et al. 2013). The relconv model determines the relativistic effects in the reflection spectrum and assumes a broken power-law emissivity profile for the illumination of the dis... | [
"Zdziarski, Johnson & Magdziarz 1996"
] | [
"Since relxillDCp considers the thermal Comptonization model nthComp",
"as the irradiating (primary) continuum, we replaced the zpowerlw continuum with nthComp."
] | [
"Uses",
"Uses"
] | [
[
1596,
1631
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] | [
[
1527,
1594
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[
1659,
1747
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] |
2016ApJ...827..107P__Padoan_&_Nordlund_1999_Instance_1 | To estimate the total integrated intensity of a shock-excited molecular line coming from a GMC, the shock models are scaled up so that the total energy dissipated in shocks is equal to the expected turbulent energy dissipation rate of the molecular cloud, as done in Basu & Murali (2001) and Pon et al. (2012). The dissi... | [
"Padoan & Nordlund 1999"
] | [
"For this paper, κ is taken to be equal to 1, in agreement with numerical simulations of decaying turbulence"
] | [
"Uses"
] | [
[
791,
813
]
] | [
[
604,
711
]
] |
2019MNRAS.487.1626Q__Fender_2006_Instance_1 | In the coupled ADAF-jet model, the accretion flow ADAF and the jet are connected by a defined parameter, $\eta \equiv \dot{M}_{\rm jet}/\dot{M}$, and $\dot{M}_{\rm jet}$ is input by assuming a value of, η, which is free parameter in the present model. The half-opening angle ϕ of the jet in the low/hard state of NS-LMXB... | [
"Fender 2006"
] | [
"Observationally, the bulk Lorentz factor of the jet in the low/hard state of X-ray binaries can be restricted in a relatively narrow range and the velocity of the jet is mildly relativistic, i.e. Γjet ≲ 2. More strictly, the bulk Lorentz factor is restricted to be as Γjet ≲ 1.67",
"and Γjet ≲ 1.2"
] | [
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[
801,
812
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[
484,
763
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[
785,
799
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2016ApJ...817..117S__Brisken_&_Zirin_1997_Instance_1 | Running penumbral waves in velocity and intensity observations were first reported by Giovanelli (1972) and Zirin & Stein (1972). Later, they were found in the photosphere as well (Musman et al. 1976), but there they appear to be more intermittent and to have higher radial phase velocity (40–90 km s−1) than the waves i... | [
"Brisken & Zirin 1997"
] | [
"A similar effect is also found in measurements of the propagation velocity of travelling waves"
] | [
"Background"
] | [
[
1010,
1030
]
] | [
[
914,
1008
]
] |
2017ApJ...837..127G__Kasliwal_et_al._2015_Instance_1 | Even though the physical processes giving rise to the flaring emission of blazars remain debatable, considerable progress has been made in characterizing the statistical properties of blazar variability at different wavelengths, and in different time domains. In particular, it has been demonstrated repeatedly that the ... | [
"Kasliwal et al. 2015"
] | [
"In particular, it has been demonstrated repeatedly that the power spectral density (PSD) of blazar light curves is, in general, of a power-law form"
] | [
"Background"
] | [
[
812,
832
]
] | [
[
260,
407
]
] |
2021MNRAS.502..915C__Ogilvie_2014_Instance_1 | Under the Applegate model, the change in orbital period is directly related to the change in the companion star’s gravitational quadrupole moment Q (Applegate & Patterson 1987),
(8)$$\begin{eqnarray*}
\frac{\Delta P_{\rm orb}}{P_{\rm orb}} = -9\frac{\Delta Q}{M_{\rm c} A^2},
\end{eqnarray*}$$where A = x(1 + q)/sin i ... | [
"Ogilvie 2014"
] | [
"For solar-type stars k2 ∼ 0.035"
] | [
"Uses"
] | [
[
867,
879
]
] | [
[
834,
865
]
] |
2015AandA...576A..26K__Hathaway_&_Rightmire_2010_Instance_1 | We have seen that some of our runs show clear activity cycles. Therefore we expect to see a corresponding modulation of the flow. In Fig. 13, we show for Run A the temporal variation of the mean large-scale magnetic field (\hbox{$\mean B$}B) normalized by Beq, the latitudinal component of the meridional circulation uθ(... | [
"Hathaway & Rightmire 2010"
] | [
"This kind of weak anti-correlation between the activity cycle and the meridional flow has been found in solar observations"
] | [
"Similarities"
] | [
[
1118,
1143
]
] | [
[
977,
1099
]
] |
2022AandA...659A.180G__Stangalini_et_al._2014_Instance_1 | The reasons for studying the dynamic properties of small-scale magnetic fields in the quiet photosphere are manifold. Firstly, magnetic fields provide an opportunity to probe some aspects inherent to turbulent convection (see, e.g. Abramenko et al. 2011; Lepreti et al. 2012; Giannattasio et al. 2013, 2014a,b; Giannatta... | [
"Stangalini et al. 2014"
] | [
"The reasons for studying the dynamic properties of small-scale magnetic fields in the quiet photosphere are manifold. Firstly, magnetic fields provide an opportunity to probe",
"and energy propagation to the upper atmospheric layers (see, e.g.",
"that cannot be addressed otherwise from an observational point o... | [
"Motivation",
"Motivation",
"Motivation"
] | [
[
629,
651
]
] | [
[
0,
174
],
[
451,
516
],
[
861,
932
]
] |
2021MNRAS.504.5840F__Eriksen_et_al._2007_Instance_1 | 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"
] | [
"In particular, the analysis of CMB data, most notably from the Wilkinson Microwave Anisotropy Probe",
"and Planck",
"experiments, has not yet provided conclusive evidence for the hypothesis of Cosmological Isotropy"
] | [
"Background",
"Background",
"Background"
] | [
[
576,
590
],
[
597,
601
]
] | [
[
308,
407
],
[
436,
446
],
[
477,
574
]
] |
2018MNRAS.478.3890B__Heckman_et_al._2017_Instance_1 | Rather than AGN feedback, it is possible that the effects we are seeing are from a different process coeval or prior to the onset of AGN accretion. Several works have pointed out that AGN activity coincides with a recent starburst, with the AGN having significant accretion events at least ∼200 Myr after the starburst h... | [
"Heckman et al. 2017"
] | [
"Several works have pointed out that AGN activity coincides with a recent starburst, with the AGN having significant accretion events at least ∼200 Myr after the starburst has occurred",
"giving the neutral material time to propagate out to the impact parameters probed by COS-AGN"
] | [
"Background",
"Background"
] | [
[
514,
533
]
] | [
[
148,
331
],
[
420,
512
]
] |
2019ApJ...871...58T__Charbonnel_&_Lagarde_2010_Instance_2 | We derived stellar parameters, [C/M], and [N/M] using SLAM. To avoid bad fits at the edges of the parameter space, we exclude stars with spectral S/N in the g band less than 50, and metallicity less than −1.4. The derived C and N abundances are shown in Figure 8. Clearly, in the top panel, the CH-strong, CH-normal, and... | [
"Charbonnel & Lagarde 2010"
] | [
"Stars with brighter K-band absolute magnitudes tend to have higher [N/Fe] and lower [C/Fe] (middle and bottom panels of Figure 8), which is consistent with extra-mixing theory and observation"
] | [
"Similarities"
] | [
[
1299,
1324
]
] | [
[
1085,
1276
]
] |
2016AandA...589A..44G__within_2000_Instance_2 | W51e2 is the strongest and best-studied HC HII region in the W51 Main cluster, and it is believed to be powered by an O8-type young star (e.g., Shi et al. 2010a). A number of interferometric studies conducted with varying angular resolutions, at centimetre (cm) and (sub)millimetre (mm) bands, identified molecular and i... | [
"Zhang & Ho 1997"
] | [
"Higher angular resolution observations of the (3, 3) NH3 absorption line (0\\hbox{$\\farcs$}.̋3 beamsize) showed signatures of rotation within 2000 AU based on a position-velocity (pv) diagram"
] | [
"Background"
] | [
[
774,
789
]
] | [
[
582,
772
]
] |
2022AandA...658A..78S__Rosen_&_Krumholz_2020_Instance_1 | Molecular outflows are a common and essential component in the formation process of low- and high-mass stars. In the past 40 yr, astronomers have mapped outflows in the whole mass range of young stellar objects (YSOs; e.g., Frank et al. 2014; Bally 2016; Anglada et al. 2018; Ray & Ferreira 2021). Magnetohydrodynamical ... | [
"Rosen & Krumholz 2020"
] | [
"Here, for instance, the presence of a magnetic field leads to the formation of early outflows. These reduce the radiation pressure, which allows the protostar mass to grow further"
] | [
"Background"
] | [
[
749,
770
]
] | [
[
543,
722
]
] |
2020AandA...644L...7G__Magdis_et_al._2020_Instance_3 | As in G18, we compiled existing constraints on the molecular gas fraction fgas of quiescent and pSB galaxies from recent literature, namely: local QGs consisting of the ATLAS3D (Young et al. 2011; Cappellari et al. 2013; Davis et al. 2014) and HRS (Boselli et al. 2014; Lianou et al. 2016) ETG samples as well as the sam... | [
"M20"
] | [
"Here we adopted an intermediate value between the solar and supersolar G/Ds used in",
"and we increased the error bars of these points to include both the solar and supersolar confidence estimates."
] | [
"Uses",
"Uses"
] | [
[
2112,
2115
]
] | [
[
2028,
2111
],
[
2117,
2227
]
] |
2018ApJ...853L..34B__Kóspál_et_al._2014_Instance_1 | With the identification of the ∼6.6 day stellar rotation period, the question remains, what is origin of the ∼9.0 day signal in the periodogram? Because of K2’s large pixel size, we considered the possibility of contamination from additional sources in the field and found that images from DSS, Galex, 2MASS, WISE, and P... | [
"Kóspál et al. 2014"
] | [
"Although hotspots located at the foot of accretion streams can affect RV measurements mimicking the signal of an orbiting body",
"Johns-Krull et al. (2016) specifically looked for these signals and found no evidence that hotspots produced the RV signals seen in photospheric absorption lines."
] | [
"Uses",
"Uses"
] | [
[
1882,
1900
]
] | [
[
1754,
1880
],
[
1932,
2094
]
] |
2020MNRAS.499.4394M__Bate_et_al._2014_Instance_2 | For these four remaining FHSC candidates (L1451-mm, MC35-mm, SM1N, and Oph A-N6) that have been observed at intermediate scales (few 100 au to few 1000 au) a final confirmation of their true evolutionary state requires higher resolution observations. For L1451-mm, the compact outflow needs to be resolved to investigate... | [
"Bate et al. 2014"
] | [
"As for the density profile, simulations of the FHSC stage show a flat inner region, corresponding to the FHSC structure and extending up to ∼10 au"
] | [
"Compare/Contrast"
] | [
[
1630,
1646
]
] | [
[
1462,
1608
]
] |
2017MNRAS.466.3961S__Grcevich_&_Putman_2009_Instance_1 | Other important components of the X-ray sky are X-ray binaries, the hot gas present in our own Galaxy and the extragalactic hot gas. Amongst these X-ray sources, the large hot gas reservoir (Tvir ∼ 107 K) filling the space between the galaxies in the clusters, known as the ICM, has been observed in its X-ray emission f... | [
"Grcevich & Putman 2009"
] | [
"Some of the recent observations and studies",
"indicate that the CGM can account for a good fraction of the baryons in these galaxies."
] | [
"Background",
"Background"
] | [
[
836,
858
]
] | [
[
791,
834
],
[
1001,
1088
]
] |
2021MNRAS.508.4429C__Hobbs_et_al._2010_Instance_1 | We explore another mechanism that can possibly result in torque reversals in the neutron star on long time-scales. It has been known for a long time that radio pulsars (which are usually isolated systems) show unexplained stochastic deviations in their spin-down behaviour (known as ‘timing noise’) on varied time-scales... | [
"Hobbs et al. 2010"
] | [
"From power spectrum analysis, significant periodicities ranging from about 1.4 to 10 yr were found in PSR B1540−06, PSR B1642−03, PSR B1818−04, PSR B1826−17, PSR B1828−11, and PSR B2148+63"
] | [
"Uses"
] | [
[
893,
910
]
] | [
[
703,
891
]
] |
2016AandA...592A..19C__Maraston_et_al._(2009)_Instance_2 | Since the star-formation histories of galaxies (ETGs included, e.g. De Lucia et al. 2006; Maraston et al. 2009) can be stochastic and include multiple bursts, we also verify the full-spectrum fitting capabilities to retrieve more complex SFHs. In particular, we take an 11 Gyr old composite stellar population with an ex... | [
"Maraston et al. (2009)"
] | [
"In all cases, we consider a solar metallicity for the main SF episode and, according to the results of",
"a subsolar metallicity (Z = 0.004) for the later one."
] | [
"Uses",
"Uses"
] | [
[
772,
794
]
] | [
[
669,
771
],
[
796,
849
]
] |
2016ApJ...819...97T__Gordon_et_al._1987_Instance_1 | The ReTOF results from irradiated phosphine and deuterated methane ice provide crucial information regarding the mechanism of formation for methylphosphanes by analyzing the intensities of various isotopologues. Figure 8 shows the possible formation routes that would lead to each of the three observed isotopologues of ... | [
"Gordon et al. 1987"
] | [
"If the carbene is formed in its first excited singlet state (a1A1), the insertion is barrierless"
] | [
"Uses"
] | [
[
757,
775
]
] | [
[
659,
755
]
] |
2021ApJ...911...59L__Kereš_et_al._2005_Instance_1 | In addition to the galaxy colors (e.g., Baldry et al. 2004; Bell et al. 2004; Borch et al. 2006; Xue et al. 2010; Salim 2014; Lee et al. 2015; Wang et al. 2017), there are other indicators characterizing the star formation nature of galaxies, e.g., the morphology (Strateva et al. 2001; Barro et al. 2013, 2014; Pan et a... | [
"Kereš et al. 2005"
] | [
"Using these indicators, a number of studies have found that the color or SFR transition of galaxies is associated with the consumption of their gas content (e.g.,"
] | [
"Background"
] | [
[
735,
752
]
] | [
[
572,
734
]
] |
2017MNRAS.469.3738S__Wargelin_etal._2004_Instance_1 | For the spectral fitting, the astrophysical background components are determined from a simultaneous fit to data from the RASS4 (Snowden etal. 1997). The extraction region for the RASS data is an annulus from 0.7 to 1 around the cluster centre (for NGC4636, NGC1399 and A3526 r500 is larger than 0.7, so the RASS data we... | [
"Wargelin etal. 2004"
] | [
"As shown by comparisons to dark moon observations only particle events are recorded in the stow position"
] | [
"Background"
] | [
[
835,
854
]
] | [
[
706,
810
]
] |
2020ApJ...894..107I__Gibb_et_al._2004_Instance_1 | AFGL 2136 IRS 1 (also referred to as CRL 2136, G17.64+0.16, and IRAS 18196−1331) is a luminous (1.0 × 105 L; Lumsden et al. 2013), high-mass (45 ± 10 M; Maud et al. 2019) protostar that is believed to be in the latter stages of its evolution due to a variety of observed characteristics (Boonman & van Dishoeck 2003; Mau... | [
"Gibb et al. 2004"
] | [
"The cool molecular envelope exhibits ice and dust absorption bands"
] | [
"Background"
] | [
[
1228,
1244
]
] | [
[
1098,
1164
]
] |
2018MNRAS.476.1412I__Yuan,_Quataert_&_Narayan_2003_Instance_1 | There have been a number of analytical solutions and numerical studies for rotating flows with viscous angular momentum transport (e.g. Shakura & Sunyaev 1973; see reviews by Pringle 1981; Kato, Fukue & Mineshige 2008, references therein). Among those, we here focus on accretion flows which cannot lose internal energy ... | [
"Yuan, Quataert & Narayan 2003"
] | [
"Sagittarius A* (Sgr A*) is inferred to be accreting at a rate of 10−3 to $10^{-2}\\ \\dot{M}_{\\rm B}$ (e.g."
] | [
"Uses"
] | [
[
722,
751
]
] | [
[
616,
721
]
] |
2021AandA...654A.124W__Tanvir_et_al._2017_Instance_2 | The first multi-messenger GW event was discovered on 17 August, 2017. About 1.7 s after the GW170817 signal detected by LIGO and Virgo (Abbott et al. 2017a), the Fermi Gamma-ray Burst Monitor was successfully triggered by GRB 170817A (Abbott et al. 2017b; Goldstein et al. 2017; Zhang et al. 2018) and subsequently a lar... | [
"Tanvir et al. 2017"
] | [
"In more detail, the existence of a “blue” and possibly also a “purple” component in the AT 2017gfo emission further indicated that the merger product of the GW170817 event is very likely to be a hypermassive NS, which lasted for at least a few hundred milliseconds, as an immediately formed black hole can only be a... | [
"Background"
] | [
[
1949,
1967
]
] | [
[
1533,
1880
]
] |
2022MNRAS.509.1010R__Laughlin_&_Adams_1998_Instance_1 | Recent work by Longmore, Chevance & Kruijssen (2021) has revealed an intriguing correlation between stellar phase-space density and the architecture of planetary systems, in particular the multiplicity. This work followed a similar analysis by Winter et al. (2020), which uncovered a correlation between stellar phase-sp... | [
"Laughlin & Adams 1998"
] | [
"The origin of this correlation is puzzling, as stellar clustering is expected to affect mostly the outer part of planetary systems in very dense environments"
] | [
"Compare/Contrast"
] | [
[
1189,
1210
]
] | [
[
1030,
1187
]
] |
2015MNRAS.448.1644S__Rines_&_Diaferio_2006_Instance_1 | Despite a number of attempts of employing aspherical models for the matter distribution in the analysis of X-ray and lensing observations of galaxy clusters (see e.g. Corless, King & Clowe 2009; Samsing, Skielboe & Hansen 2012; Sereno et al. 2013), all dynamical methods are based on spherical symmetry. As the first ste... | [
"Rines & Diaferio 2006"
] | [
"which is one of the commonly used methods of mass determination in galaxy clusters (see e.g."
] | [
"Background"
] | [
[
946,
967
]
] | [
[
829,
921
]
] |
2015AandA...576A...5C__Jørgensen_et_al._2012_Instance_3 | The relative abundances of the three species are derived from the column densities in Table 2 and are compared with other star-forming regions and comets in Table 3. The (CH2OH)2/CH2OHCHO abundance ratio of ~0.3–0.5 previously derived in IRAS 16293 by Jørgensen et al. (2012) was revised. Indeed, the assignment in Jørge... | [
"Jørgensen et al. 2012"
] | [
"This new estimate is consistent with the ratio expected between the aGg′ and gGg′ conformers under thermal equilibrium conditions at 300 K, the excitation temperature of glycolaldehyde derived in IRAS 16293"
] | [
"Similarities"
] | [
[
1044,
1065
]
] | [
[
836,
1042
]
] |
2016MNRAS.462.3441D__Namouni_1999_Instance_2 | In principle, Fig. 5, central panel G, shows that (469219) 2016 HO3 may have been locked in a Kozai–Lidov resonance with ω librating about 270° for nearly 100 kyr and probably more. Because of the Kozai–Lidov resonance, both e (central panel E) and i (central panel F) oscillate with the same frequency but out of phase ... | [
"Namouni 1999"
] | [
"see equations 3 in",
"these are based on the vector eccentricity and the vector inclination."
] | [
"Background",
"Background"
] | [
[
1126,
1138
]
] | [
[
1107,
1125
],
[
1141,
1211
]
] |
2016ApJ...832...57P__Parashar_et_al._2009_Instance_1 | We employ two types of kinetic codes, hybrid particle-in-cell (PIC) and full PIC simulations. Both types make use of the P3D family of codes (Zeiler et al. 2002), in hybrid PIC (e.g., Parashar et al. 2011) mode, and fully kinetic PIC mode (e.g., Wu et al. 2013b). All simulations discussed here are performed in the 2.5D... | [
"Parashar et al. 2009"
] | [
"The initial condition is the Orszag–Tang vortex (OTV) (e.g.,"
] | [
"Uses"
] | [
[
1174,
1194
]
] | [
[
1069,
1129
]
] |
2022AandA...662A..42M__Vázquez_2007_Instance_2 | A number of fundamental results have been rigorously proved in the mathematical literature concerning the asymptotic behaviour in time of some of the solutions of the porous medium equation and related equations (e.g. Kamin & Vázquez 1991; Bernis et al. 1993; Hulshof et al. 2001). What is of interest for us here is, pr... | [
"Vázquez 2007"
] | [
"also, ‘convergence’ is meant in the sense that the Lp norm of the difference between the actual solution and the ZKBP function tends to zero as t → ∞ faster than a negative power of the time with an exponent which is a function of n, m, and p (e.g. −1/3 for n = 2 and m = 3 in the L2 norm; see details in the book b... | [
"Background"
] | [
[
1283,
1295
]
] | [
[
966,
1282
]
] |
2022MNRAS.517.5744G__Caro_et_al._2016_Instance_1 | The CO photodesorption yield reaches its highest value when this ice is deposited at low temperatures (down to 7 K, the lowest temperature studied experimentally) and decreases gradually at higher deposition temperatures (Öberg et al. 2007; Öberg et al. 2009; Muñoz Caro et al. 2010, 2016; Sie et al. 2022). The explanat... | [
"Muñoz Caro et al.",
"2016"
] | [
"The CO photodesorption yield reaches its highest value when this ice is deposited at low temperatures (down to 7 K, the lowest temperature studied experimentally) and decreases gradually at higher deposition temperatures",
"The explanation for this phenomenon motivated further research."
] | [
"Background",
"Motivation"
] | [
[
260,
277
],
[
284,
288
]
] | [
[
0,
220
],
[
308,
371
]
] |
2017ApJ...835..169O___2016_Instance_1 | Recent MIR studies have provided us with a much more realistic view of the central part of the AGNs. Spitzer studies of nearby Compton-thick AGNs have shown that even Compton-thick AGNs, especially low-luminosity ones, often show only modest to moderate silicate absorption at
μm (e.g., Hao et al. 2007; Goulding ... | [
"Stalevski et al.",
"2016"
] | [
"On the other hand, if the torus is made of a collection of clouds, each cloud is heated to ∼300 K to emit MIR emission while absorbing the background light when the foreground cloud is cooler than the one behind. The radiation transfer effect among the clouds significantly reduces the net silicate absorption even ... | [
"Differences"
] | [
[
910,
926
],
[
933,
937
]
] | [
[
485,
830
]
] |
2021AandA...648A...3K__Lonsdale_et_al._2003_Instance_1 | LoTSS is currently mapping all of the northern sky to a high sensitivity and resolution (S150MHz ~ 0.1 mJy beam−1 and FWHM ~ 6′′) at the relatively unexplored 120–168 MHz frequencies. In parallel with this, LOFAR is also undertaking deep observations of best studied multi-wavelength, degree scale fields in the northern... | [
"Lonsdale et al. 2003"
] | [
"The first three LoTSS Deep Fields are the European Large-Area ISO Survey-North 1 (ELAIS-N1",
"Lockman Hole, and Boötes",
"these were chosen to have extensive multi-wavelength coverage from past and ongoing deep, wide-area surveys sampling the X-ray",
"and to infrared (IR; e.g.",
"wavelengths"
] | [
"Background",
"Background",
"Background",
"Background",
"Background"
] | [
[
1078,
1098
]
] | [
[
460,
550
],
[
573,
597
],
[
620,
746
],
[
1052,
1077
],
[
1204,
1215
]
] |
2020MNRAS.493.4950S__Haines_et_al._2015_Instance_1 | In the framework of the hierarchical formation of structures, clusters of galaxies are continuously accreting galaxies. It has been suggested that in this process of falling, galaxies could undergo different physical processes that could affect the star formation even before they reach the cluster. Consequently, to ful... | [
"Haines et al. 2015"
] | [
"Several observations have shown that properties of galaxies such as star formation, gas content, and colour are affected by the cluster environment at large clustercentric distances (e.g."
] | [
"Background"
] | [
[
842,
860
]
] | [
[
507,
694
]
] |
2020AandA...641A.155V__Puglisi_et_al._2019_Instance_1 | The scenario presented above has been formulated in various flavors to individually explain several of the properties reported here. The main addition of this work, namely the excitation of CO in distant main-sequence and starburst galaxies, fits in the general picture that we sketched. The ensemble of properties and c... | [
"Puglisi et al. 2019"
] | [
"This proved to be a useful distinction and an excellent predictor of several trends",
"but recent results, including our present and previous analysis",
"show that the demarcation between starburst and main-sequence galaxies is more blurred that we previously considered."
] | [
"Compare/Contrast",
"Compare/Contrast",
"Compare/Contrast"
] | [
[
729,
748
]
] | [
[
551,
634
],
[
664,
727
],
[
751,
868
]
] |
2017AandA...604A.118T__Zaritsky_et_al._1994_Instance_1 | In the Local Universe, most of our current knowledge of chemical distributions in disc galaxies comes from studies of the ISM via observations of HII regions or young stellar populations. Current observations are consistent with the metallicity profiles of the ISM having negative metallicity gradients, on average. Meta... | [
"Zaritsky et al. 1994"
] | [
"Metallicity gradients in units of dex kpc-1 determine tight correlations with the global properties of galaxies such as the stellar mass or the size, which are erased when normalised by a characteristics radius such as the half-mass radius (e.g."
] | [
"Background"
] | [
[
562,
582
]
] | [
[
316,
561
]
] |
2020ApJ...897...73M__Coburn_2001_Instance_1 | Some of the accretion-powered X-ray pulsars showed additional features in emission between the 10 and 20 keV energy bands and more rarely in absorption between 8 and 10 keV in their respective residuals when fitted with a variety of continuum models (Coburn et al. 2002). Coburn et al. (2002) argued that such features m... | [
"Coburn 2001"
] | [
"For example, it was observed that a single emission line at around 14 keV can fit two features around 10 and 20 keV for",
"Her X-1",
"In the case of GRO J2058+42, an introduction of a single Gaussian emission line in this range of energies could not appropriately fit the spectrum."
] | [
"Uses",
"Uses",
"Compare/Contrast"
] | [
[
579,
590
]
] | [
[
414,
533
],
[
570,
577
],
[
777,
924
]
] |
2017MNRAS.470.4099B__Smith_et_al._2003_Instance_1 | Numerical simulations using the N-body method are the primary instrument used to probe the non-linear regime of structure formation in cosmology and provide the basis for all theoretical predictions for the distribution of dark matter at the corresponding physical scales. Over the last few decades, such simulations hav... | [
"Smith et al. 2003"
] | [
"In this context ‘scale-free’ cosmological models, in which both the expansion law and the power spectrum characterizing the initial fluctuations are simple power laws, have the advantage of relative simplicity, and they have for this reason been studied quite extensively in the literature (see e.g."
] | [
"Background"
] | [
[
1179,
1196
]
] | [
[
789,
1088
]
] |
2022ApJ...928...18Z__Eastwood_et_al._2017_Instance_1 | The intensity of a geomagnetic storm is the result of the sustained interaction between the solar wind and the magnetosphere during the main phase of a storm. The most outstanding advantage of empirical formulae is their simplicity for space weather forecast: By inputting the solar wind parameters responsible for the m... | [
"Eastwood et al. 2017"
] | [
"Extreme geomagnetic storms can cause widespread interference and damage to technological systems",
"and then lead to significant economic loss (e.g.,"
] | [
"Background",
"Background"
] | [
[
1050,
1070
]
] | [
[
819,
915
],
[
951,
1000
]
] |
2016MNRAS.461.4317M__Zharikov_et_al._2008_Instance_1 | Finally, we compared the extinction-corrected upper limit on the optical flux of the PSR J0633+0632 PWN (Section 2.1) with its unabsorbed 0.3–10 keV X-ray flux. This is $F_{\rm X}^{{\rm pwn}} = 2.92^{+0.79}_{-0.81} \times 10^{-13}$ erg cm−2 s−1 (Abdo et al. 2013), computed by fitting the PWN area with an ellipse of sem... | [
"Zharikov et al. 2008",
"Zharikov et al. 2008"
] | [
"Our upper limit on the Fopt/Fx for the PSR J0633+0632 PWN is above the values obtained for the other PWNe, which are typically ∼ 0.02–0.04, apart from the Crab PWN which has an Fopt/Fx ∼ 2",
"This is also the case for the PSR J1124−5916 PWN"
] | [
"Differences",
"Compare/Contrast"
] | [
[
1265,
1285
],
[
2220,
2240
]
] | [
[
1075,
1263
],
[
2170,
2218
]
] |
2015MNRAS.446.4168R__Kroupa_2014_Instance_1 | The IGIMF theory (Kroupa et al. 2013) predicts a coupling between some properties of a galaxy (the SFR and the metallicity) and the IMF. Since the IMF in turn strongly affects the dynamical evolution of the galaxy, the feedback between galaxy evolution and IMF is difficult and the fully complexity of a variable IMF has... | [
"Kroupa 2014"
] | [
"Also the dependence of the IMF on the SFR is nowadays observationally well established"
] | [
"Background"
] | [
[
1180,
1191
]
] | [
[
1017,
1103
]
] |
2019MNRAS.484.1487E__Roca-Fabrega_et_al._2013_Instance_2 | Since the manifold spirals arise in a system of reference which corotates with the bar, the manifold theory in its basic form predicts that the spiral arms should have the same pattern speed as the bar. This remark seems to come in conflict with observations both in our Galaxy (as reviewed e.g. in Bland-Hawthorn & Gerh... | [
"Roca-Fabrega et al. 2013"
] | [
"but see also a noticeable exception in"
] | [
"Differences"
] | [
[
1081,
1105
]
] | [
[
1042,
1080
]
] |
2021ApJ...919..140S__Bartos_et_al._2017_Instance_2 | Resonant dynamical friction may have applications beyond the relaxation of IMBHs examined in this paper. It may affect all objects in stellar clusters much more massive than the individual constituents of the disk, if present, including massive stars, stellar mass black holes (BHs), or the center of mass of massive bin... | [
"Bartos et al. 2017"
] | [
"An interesting implication is that, if BHs settle into the disk, they interact dynamically and form BH–BH binaries efficiently, and frequent dynamical interactions and gas effects drive the BHs to merger, producing gravitational waves (GWs) detectable by LIGO, VIRGO, and KAGRA"
] | [
"Background"
] | [
[
1010,
1028
]
] | [
[
703,
980
]
] |
2021AandA...645A.141V__Metcalfe_et_al._2016_Instance_1 | This paper presents the results of our study of the effect of a dynamically adapting heat-conduction prescription, based on Kramers opacity law, in conjunction with semi-global MHD simulations. The main aim is to determine the effect of this prescription on the two major transitions reported in numerical studies (e.g.,... | [
"Metcalfe et al. 2016"
] | [
"The fact that simulations usually produce anti-solar differential rotation for the solar rotation rate could indicate that the Sun is in a transitional regime (e.g.,",
"or could also mean that simulations still cannot fully capture the true rotational influence on turbulent convection in the Sun."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1054,
1074
]
] | [
[
868,
1033
],
[
1077,
1205
]
] |
2020ApJ...889...15Y__Yang_et_al._2016b_Instance_2 | Although each one of the four aforementioned mechanisms has some observational support in certain systems, there is not a single mechanism that can explain all observed polarization in protoplanetary disks. Alignment with respect to the local radiation anisotropy (“k-RAT alignment” thereafter) is best supported by the ... | [
"Yang et al. 2016b"
] | [
"But there is no well-resolved system that matches the theoretical expectations (see, e.g.,"
] | [
"Motivation"
] | [
[
1062,
1079
]
] | [
[
950,
1040
]
] |
2016MNRAS.455..449H__McGaugh_2012_Instance_1 | With only six free parameters, the standard Λ cold dark matter (ΛCDM) cosmological model fits no less than 2500 multipoles in the cosmic microwave background (CMB) angular power spectrum (Planck Collaboration XVI 2014), the Hubble diagram of Type Ia supernovae, the large-scale structure matter power spectrum, and even ... | [
"McGaugh 2012"
] | [
"Nevertheless, it still faces numerous challenges on galaxy scales. Among these, the most important ones are",
"for dwarf galaxies, the tightness of the baryonic Tully–Fisher relation"
] | [
"Motivation",
"Motivation"
] | [
[
879,
891
]
] | [
[
526,
633
],
[
806,
877
]
] |
2019MNRAS.488.5029H__Stacey_et_al._2010_Instance_3 | For the first time, we detected [C ii] 158-μm emission from a GRB host galaxy at z > 2. This is the second detection of [C ii] 158-μm emission among known GRB host galaxies, following GRB 980425 (Michałowski et al. 2016). The [C ii] 158-μm fine structure line is the dominant cooling line of the cool interstellar medium... | [
"Stacey et al. 2010"
] | [
"The comparison sample is compiled from the literature up to z ∼ 3"
] | [
"Uses"
] | [
[
1479,
1497
]
] | [
[
1343,
1408
]
] |
2017MNRAS.472.1152R__Cenko_et_al._2010_Instance_1 | 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"
] | [
"There have been searches for a periodic signal in the prompt emission of GRBs with a number of instruments with no success, for example:",
"and Burst Alert Telescope (BAT) GRBs"
] | [
"Background",
"Background"
] | [
[
1227,
1244
]
] | [
[
756,
892
],
[
1189,
1225
]
] |
2020ApJ...889L..10M__McKay_et_al._2018_Instance_2 | As stated earlier, during review of this manuscript Croviser et al. announced in a CBET a tentative water production rate approximately five times larger than our reported value. While the brief nature of the CBET precludes a detailed comparison, we discuss some possible reasons for this discrepancy. At the high airmas... | [
"McKay et al. 2018"
] | [
"At certain geocentric velocities the cometary [O i] 6300 Å emission sits on top of a strong telluric absorption, and at high airmass inaccurate removal of this feature can result in a decrease in the measured flux and therefore production rate. This was observed for C/2012 S1 (ISON)"
] | [
"Compare/Contrast"
] | [
[
1349,
1366
]
] | [
[
1064,
1347
]
] |
2020MNRAS.493.4950S__Linden_et_al._2010_Instance_1 | In the framework of the hierarchical formation of structures, clusters of galaxies are continuously accreting galaxies. It has been suggested that in this process of falling, galaxies could undergo different physical processes that could affect the star formation even before they reach the cluster. Consequently, to ful... | [
"von der Linden et al. 2010"
] | [
"Several observations have shown that properties of galaxies such as star formation, gas content, and colour are affected by the cluster environment at large clustercentric distances (e.g."
] | [
"Motivation"
] | [
[
814,
840
]
] | [
[
507,
694
]
] |
2020MNRAS.496..152R__Springel_&_Hernquist_2002_Instance_1 | From observations it is known that the interstellar gas has a complex structure with different phases – a hot volume-filling phase and a dense cold gas phase – both of which should be represented in galaxy formation simulations (see Naab & Ostriker 2017; Tumlinson et al. 2017). To model this, we treat the gas as a mult... | [
"Springel & Hernquist 2002"
] | [
"Here, Ai,j are the entropic functions of the particles"
] | [
"Uses"
] | [
[
701,
726
]
] | [
[
645,
699
]
] |
2021MNRAS.504.5702W__Werk_et_al._2014_Instance_1 | Another notable accretion-regulated halo property is gas temperature, with the CGM of haloes nominally having both a hot and cold-phase. The hot coronal gas phase (at ≈Tvir) originates from the virial shock-heating of gas accreting high-mass haloes ($M_{\rm halo}\gtrsim 10^{12}\, \mathrm{M}_{\odot }$; e.g. Rees & Ostri... | [
"Werk et al. 2014"
] | [
"A cold-phase of the CGM at ≈104 K has also been observed, but its origins are less clear"
] | [
"Motivation"
] | [
[
548,
564
]
] | [
[
331,
419
]
] |
2021MNRAS.508.2583Z__Schöier_et_al._2002_Instance_1 | Located in the star-forming region ρ-Ophiuchi, inside the dark cloud L1689N and at a distance of 141 pc (Dzib et al. 2018), IRAS16293−2422 is a well-studied Young Stellar Object (YSO) classified as a Class 0 source with less than 104 yr (Andre, Ward-Thompson & Barsony 1993), and represents one of the very early stages ... | [
"Schöier et al. 2002"
] | [
"It was the first source identified as a hot corino",
"based on the detection of Complex Organic Molecules (COMs) in the source, which was later supported by follow-up studies"
] | [
"Background",
"Background"
] | [
[
597,
616
]
] | [
[
348,
398
],
[
445,
565
]
] |
2020ApJ...898...52M__Elmegreen_&_Scalo_2004_Instance_1 | Idealized simulations have the advantage of carefully controlled conditions but the disadvantages that the turbulence is driven in an artificially prescribed manner to maintain a fixed overall turbulent amplitude and the processes leading to cloud formation and destruction are not followed. In reality, GMCs form due to... | [
"Elmegreen & Scalo 2004"
] | [
"Turbulence on scales less than the scale height of the warm–cold ISM likely originates primarily due to the feedback from young stars"
] | [
"Background"
] | [
[
843,
865
]
] | [
[
708,
841
]
] |
2020MNRAS.497..302T__Watarai_2006_Instance_1 | In this paper, we explore the conditions required for hyper-Eddington accretion on to a BH when both radiative and mechanical feedback operate simultaneously, performing two-dimensional (2D) hydrodynamical simulations with multifrequency radiation transfer. We conduct a comprehensive survey on the parameter dependence ... | [
"Watarai 2006"
] | [
"To model mechanical feedback, we adopt a phenomenological model proposed by Ostriker et al. (2010), while radiative feedback is treated by adopting the standard and slim disc model"
] | [
"Uses"
] | [
[
700,
712
]
] | [
[
470,
650
]
] |
2019AandA...630A..30L__Hässig_et_al._(2015)_Instance_3 | The many unexpected surprises of comet 67P/Churyumov-Gerasimenko (hereafter 67P) revealed by the historic Rosetta mission highlight the importance of observing the evolution of comets throughout their orbits. One of the surprises was the drastic heterogeneity in both the major and minor volatile species in the coma tha... | [
"Hässig et al. (2015)"
] | [
"As reported in",
", the intensity of H2O in the coma dominated the overall signal, with maxima in the H2O signal every ~6 h, about twice during a rotation.",
"Interestingly, however, CO2 and CO displayed a separate additional maximum when the H2O signal was near its minimum. This independent maximum in CO2 and... | [
"Background",
"Background",
"Motivation"
] | [
[
1070,
1090
]
] | [
[
1055,
1069
],
[
1090,
1227
],
[
1228,
1546
]
] |
2021AandA...645A..99C__analysis,_Uttley_et_al._(2011)_Instance_2 | X-ray reverberation in black hole X-ray binaries was first robustly detected in GX 339–4 by Uttley et al. (2011) when the source was in its hard state. Previous studies of GX 339–4 pointed to the approximate central mass being ≥6 M⊙ (e.g. Hynes et al. 2003) and a small disc inclination angle (De Marco et al. 2015). Mil... | [
"Uttley et al. (2011)"
] | [
"According to the time-lag analysis,",
"found that the disc thermal emission (∼0.3–0.7 keV, soft band) leads the power-law variations (∼0.7–1.5 keV, hard band) on long timescales (> 1s)."
] | [
"Background",
"Background"
] | [
[
779,
799
]
] | [
[
743,
778
],
[
800,
946
]
] |
2022ApJ...929...65I__Ikhsanov_2002_Instance_1 | Our parameter range reaches into the “propeller” regime, where the azimuthal velocity of the star’s outer magnetosphere exceeds the Keplerian velocity at disk truncation (Romanova et al. 2005), i.e., where the disk is truncated near and outside of the corotation radius. Observations of the propeller regime have been di... | [
"Ikhsanov 2002"
] | [
"The propeller regime has been investigated both analytically"
] | [
"Background"
] | [
[
708,
721
]
] | [
[
578,
638
]
] |
2016ApJ...833....7Y__Owen_&_Wu_2013_Instance_3 | 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"
] | [
"In this paper, we adopt Mpi = 20 M⊕ and Mpf = 10 M⊕ nominally (close to the standard model adopted in"
] | [
"Similarities"
] | [
[
2228,
2242
]
] | [
[
2126,
2227
]
] |
2021MNRAS.504.5992M__Ho_et_al._2015_Instance_1 | Characterizing and understanding the distribution and transport of chemical elements inside galaxies is a critical aspect of galaxy evolution. Successive generations of star formation enrich the interstellar medium (ISM) with metals. Therefore, the spatial distribution of chemical abundances in galaxies is a powerful t... | [
"Ho et al. 2015"
] | [
"Negative radial metallicity gradients have been widely observed in the low-redshift galaxy population (e.g."
] | [
"Background"
] | [
[
956,
970
]
] | [
[
783,
890
]
] |
2017MNRAS.464..635M__Dekel_et_al._2009_Instance_3 | The basic idea, summarized in Dekel et al. (2009), is that during VDI, the high surface density of gas and ‘cold’ young stars, Σ, drives the Toomre Q parameter below unity, Q ∼ σΩ/(πGΣ) ≲ 1, where σ is the 1D velocity dispersion and Ω is the angular frequency, a proxy to the epicyclic frequency κ, which is related to t... | [
"Dekel et al. 2009"
] | [
"Gravitational interactions in the perturbed disc drive turbulence causing the disc to self-regulate in a marginally stable state with Q ≲ 1",
"that can last for more than a Gyr so long as the accretion is not interrupted."
] | [
"Background",
"Background"
] | [
[
1368,
1385
]
] | [
[
1227,
1366
],
[
1517,
1595
]
] |
2019MNRAS.490.5722W__Remus_et_al._2013_Instance_2 | Since it is infeasible to observe the evolution of individual galaxies over time, theoretical approaches focusing on understanding the formation of ETGs have made use of numerical simulations to trace the evolution of individual galaxies. Through zoom-in and cosmological simulations, a consensus has emerged between the... | [
"Remus et al. 2013"
] | [
"Apart from cosmological simulations, dedicated zoom-in simulations",
"have revealed that dry mergers that dominate the passive evolution of ETGs below z ≈ 2 could make the total density profile shallower than isothermal"
] | [
"Background",
"Background"
] | [
[
1836,
1853
]
] | [
[
1713,
1779
],
[
1855,
2004
]
] |
2021MNRAS.503.2776Y__Ajith_et_al._2007_Instance_1 | In order to investigate the signal-to-noise ratio (SNR), ρ of NS–WD binaries for LISA-type space GW detectors, we calculate the averaged square SNR $\overline{\rho ^{2}}$ over the sky location, inclination, and polarization as
(30)$$\begin{eqnarray*}
\overline{\rho ^{2}} = \int _{f_{1}}^{f_{2}}\frac{4\cdot \frac{4}{5... | [
"Ajith et al. 2007"
] | [
"We calculate the GW amplitudes A(f) of NS–WD binaries using the phenomenological (PhenomA) waveform model in the Fourier domain"
] | [
"Uses"
] | [
[
830,
847
]
] | [
[
701,
828
]
] |
2022ApJ...924...42N__Torres_et_al._2013_Instance_1 | In this model, the pulsar associated with the PWN loses its rotational energy via a pulsar wind composed of magnetic and high-energy particles to power the high-energy physical process inside the nebula (Atoyan & Aharonian 1996; Fang & Zhang 2010). The relativistic wind of particles driven by the pulsar is blown into t... | [
"Torres et al. 2013"
] | [
"According to the review of the leptonic model (see, e.g.,",
"the electrons injected into PWNe are accelerated by the pulsar magnetosphere and the termination shock. Therefore, the relativistic particles injected into the PWNe are also assumed as two different power-law components from the pulsar magnetosphere an... | [
"Uses",
"Uses"
] | [
[
866,
884
]
] | [
[
765,
822
],
[
887,
1174
]
] |
2015AandA...584A.103S__Chamel_et_al._2011_Instance_3 | Douchin & Haensel (2001; DH) formulated a unified EoS for NS on the basis of the SLy4 Skyrme nuclear effective force (Chabanat et al. 1998), where some parameters of the Skyrme interaction were adjusted to reproduce the Wiringa et al. calculation of neutron matter (Wiringa et al. 1988) above saturation density. Hence, ... | [
"Chamel et al. 2011"
] | [
"and a comparison with the other EoSs of the BSk family",
"and the RMF family",
"shall be left for future study."
] | [
"Future Work",
"Future Work",
"Future Work"
] | [
[
1963,
1981
]
] | [
[
1907,
1961
],
[
2047,
2065
],
[
2088,
2119
]
] |
2021ApJ...922L..11H__Castaing_et_al._1990_Instance_1 | Most of these observations are consistent with the general understanding that, for increasing distance from the Sun, the turbulent power-law spectrum expands toward larger scales (Bavassano et al. 1982; Bruno & Carbone 2013; Chen et al. 2020). However, spectral properties may be misleading, as it is not possible to une... | [
"Castaing et al. 1990"
] | [
"Intermittency is related to the scale-dependent shape of the probability distribution function of the increments Δϕ",
"This, additionally, implies the existence of nonvanishing odd moments."
] | [
"Background",
"Background"
] | [
[
1028,
1048
]
] | [
[
911,
1026
],
[
1051,
1121
]
] |
2016MNRAS.459..277S__Ensslin_et_al._1998_Instance_1 | Diffuse synchrotron emission associated with ultrarelativistic particles and magnetic fields in the intracluster medium (ICM) primarily consists of radio haloes and radio relics (see Ferrari et al. 2008; Brüggen et al. 2012; Feretti et al. 2012; Brunetti & Jones 2014 for recent reviews). It is thought that radio haloes... | [
"Ensslin et al. 1998",
"Ensslin et al. 1998"
] | [
"whereas radio relics are apparently associated with localized, post-merger shock-fronts",
"and the Coma cluster",
"an apparent link is seen between radio galaxies and radio relics."
] | [
"Background",
"Background",
"Background"
] | [
[
736,
755
],
[
1643,
1662
]
] | [
[
647,
734
],
[
1621,
1641
],
[
1664,
1729
]
] |
2015MNRAS.450.3458C__Cichowolski_et_al._2001_Instance_2 | The kinetic energy stored in the CO shell can be estimated as $E_{\rm kin} = 0.5\, M_{\rm shell}\, V^2_{\rm exp}$, where Vexp is the expansion velocity of the shell and Mshell is the total (molecular, atomic, and ionized) shell mass. Adopting an expansion velocity equal to half the velocity interval where the structure... | [
"Cichowolski et al. (2001)"
] | [
"Although",
"concluded that WR 130 could have alone created the observed structure, it is important to note that they did not take into account the molecular mass present in the shell, which considerably increases the kinetic shell energy."
] | [
"Differences",
"Differences"
] | [
[
599,
624
]
] | [
[
590,
598
],
[
625,
851
]
] |
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