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...831...41W__Dai_&_Liu_2012_Instance_1 | Our results have immediate stimulations for further research. First, although here we have studied the SNe Ic-BL not associated with GRBs, the main conclusion can be equally applied to GRB-SNe. It is usually believed that the central engines of GRBs are black holes (Popham et al. 1999; Narayan et al. 2001; Kohri & Mine... | [
"Dai & Liu 2012"
] | [
"Growing indirect observational evidence suggests that magnetars could act as the central engines of both LGRBs and short-duration GRBs"
] | [
"Future Work"
] | [
[
1157,
1171
]
] | [
[
975,
1109
]
] |
2021AandA...655A..22M__Hopkins_et_al._2014_Instance_1 | Despite the consensus on the importance of galactic winds in dwarf galaxy formation, large uncertainties persist in how the winds are driven. As the ISM physics is typically not resolved in full cosmological simulations (although some simulations are getting close, see e.g., Wheeler et al. 2019; Agertz et al. 2020), su... | [
"Hopkins et al. 2014"
] | [
"Different approaches of subgrid models were explored",
"to mechanical feedback where the momentum boost during the unresolved adiabatic phase is calibrated through small-scale ISM simulations and injected into the ISM",
"Simulations of dwarf galaxies in recent years have often adopted one of these approaches f... | [
"Background",
"Background",
"Motivation"
] | [
[
1164,
1183
]
] | [
[
638,
690
],
[
1001,
1162
],
[
1222,
1723
]
] |
2019AandA...621A..27F__Delvecchio_et_al._2015_Instance_1 | SMBHs and host galaxies share several properties. Both SMBHs and galaxies have exponential cut-offs at the high mass end of their co-moving space densities (e.g., Shankar et al. 2009; Ilbert et al. 2013; Kelly & Shen 2013). The population of both SMBHs and galaxies also exhibit mass downsizing whereby the oldest, in th... | [
"Delvecchio et al. 2015"
] | [
"Both observations and simulations have suggested that there may be a positive trend between the mean black hole accretion rate and star-formation rate (SFR; e.g.,"
] | [
"Compare/Contrast"
] | [
[
1056,
1078
]
] | [
[
893,
1055
]
] |
2016ApJ...824..142Q__Galvin_et_al._2008_Instance_1 | Current observations of the interstellar neutral helium trajectories by the Interstellar Boundary EXplorer (IBEX) (McComas et al. 2009) determined the inflow longitude of the interstellar wind to be
(Leonard et al. 2015), ∼757 (McComas et al. 2015),
(Bzowski et al. 2015), and
(Schwadron et al. 2015... | [
"Galvin et al. 2008"
] | [
"However, recent observations of the pickup helium focusing cone using the Plasma and Suprathermal Ion Composition (PLASTIC",
"on board the Solar and Terrestrial Relations Observatory Ahead (STEREO A) spacecraft measured the peak density and determined the inflow longitude to be"
] | [
"Uses",
"Uses"
] | [
[
720,
738
]
] | [
[
596,
718
],
[
740,
892
]
] |
2019ApJ...871L..22W__Alexandrova_2008_Instance_2 | In analogy to the hydrodynamic case, the nonlinear coherent vortex structure also plays an important role in plasma dynamics and transport processes (Hasegawa & Mima 1978; Shukla et al. 1985; Petviashvili & Pokhotelov 1992; Horton & Hasegawa 1994). These vortices tend to have a long lifetime and are widely observed in ... | [
"Alexandrova 2008"
] | [
"After first being reported in the Earth’s magnetosheath"
] | [
"Background"
] | [
[
1552,
1568
]
] | [
[
1470,
1525
]
] |
2016ApJ...817..152X__Vreeswijk_et_al._2004_Instance_1 | The connection between long-duration GRBs (LGRBs) and SNe was predicted theoretically (Colgate 1974; Woosley 1993) and has been verified observationally (e.g., Galama et al. 1998; Hjorth et al. 2003; see a review in Woosley & Bloom 2006). They usually happen in the star formation regions of the galaxies (e.g., Paczyńsk... | [
"Vreeswijk et al. 2004"
] | [
"Therefore, GRB afterglows are good probes of burst environment and the interstellar dust and gas in distant, star-forming galaxies"
] | [
"Motivation"
] | [
[
921,
942
]
] | [
[
726,
856
]
] |
2017ApJ...835...94O__Martin_et_al._1994_Instance_1 | In this paper, we performed statistical analyses on the chirality and the magnetic configurations (inverse-polarity versus normal polarity) of the solar filaments that erupted on the solar disk from 2010 May 13 to 2015 December 31 covering both the rising phase and the beginning of the declining phases of solar cycle 2... | [
"Martin et al. 1994"
] | [
"The determination of the magnetic configuration is also based on a method proposed by Chen et al. (2014), i.e., those filaments that follow Martin's Rule",
"are of the inverse-polarity type, and those that disobey Martin's Rule are of the normal-polarity type."
] | [
"Uses",
"Uses"
] | [
[
638,
656
]
] | [
[
483,
636
],
[
658,
761
]
] |
2021ApJ...910...86R__Zitrin_et_al._2015_Instance_1 | One of the major endeavors of modern observational cosmology is to paint a coherent picture of the history of the universe. To this end, the final frontier remains the identification and characterization of the first sources that appeared in the universe, those which played a significant role in reionizing the intergal... | [
"Zitrin et al. 2015"
] | [
"Complementing these observations, the spectroscopic confirmation",
"of over a dozen sources has seen impressive advances with ground-based spectroscopy (e.g., probing the rest-frame UV and FIR with Keck/MOSFIRE, VLT/X-Shooter, and ALMA), particularly for the brightest and rarest objects."
] | [
"Background",
"Background"
] | [
[
1064,
1082
]
] | [
[
948,
1012
],
[
1264,
1484
]
] |
2021MNRAS.506...52O__Carroll,_Press_&_Turner_1992_Instance_1 | The SFG population bias factor, bSFG may be calculated from the ratio of galaxy to dark matter correlation functions, i.e:
(27)$$\begin{eqnarray*}
b_{\rm SFG}^2(z) &=& \frac{\xi _{\rm g}(r, z)}{\xi _{\rm DM}(r, z)} \nonumber \\
&=& \left(\frac{r_0(z)}{8} \right)^{\iota } \, \frac{J_2}{\sigma _8^2 \,\,... | [
"Carroll, Press & Turner 1992"
] | [
"and $\\mathcal {G}(z) = g(z)/g_0$, with g(z) as the growth factor at redshift z and g0 = g(z = 0) (e.g."
] | [
"Uses"
] | [
[
610,
638
]
] | [
[
507,
609
]
] |
2016AandA...592A..74S__Sobolewska_&_Papadakis_(2009)_Instance_1 | In Fig. B.1 we plot the soft X-ray light curves for our candidate highly variable AGN using available X-ray data taken by the satellite missions Einstein, ROSAT, XMM, Suzaku and Swift. The count rates were obtained from different archives including HEASARC, the XMM Science Archive, the Swift UKSSDC and from our own Swi... | [
"Sobolewska & Papadakis (2009)"
] | [
"found a positive correlation between flux and spectral slope for a sample of bright RXTE AGN in the 2–10 keV band. This could affect the relative fluxes seen in our sample which are plotted in Fig. B.1. We have attempted to quantify this for the different detectors used in the creation of our light curves."
] | [
"Uses"
] | [
[
697,
726
]
] | [
[
727,
1034
]
] |
2016ApJ...826..117Y__Roux_&_Webb_2009_Instance_1 | Traditionally, the Parker transport equation (Parker 1965) was used to model pickup ion acceleration at the SWTS when using a transport theory approach. However, interesting Voyager results, such as strongly fluctuating pitch-angle anisotropies upstream, the detection of highly anisotropic intensity spikes at the SWTS,... | [
"le Roux & Webb 2009"
] | [
"In response, shock acceleration transport models were developed in recent years based on the numerical solutions of the focused transport equation",
"to take advantage of the fact that focused transport is not restricted to small pitch-angle anisotropies."
] | [
"Background",
"Background"
] | [
[
1206,
1225
]
] | [
[
985,
1131
],
[
1227,
1332
]
] |
2017MNRAS.470..713M__Farinelli_et_al._2012_Instance_1 | Thereafter, we proceeded to fit the broad-band spectrum with the analytical model ‘COMPMAG’ and its updated version. The ‘COMPMAG’ model has many spectral parameters that were impossible to constrain simultaneously. Especially, β if left free preferred a value >0.9 in the fit, which is greater than the maximum possible... | [
"Farinelli et al. 2012"
] | [
"The fit also provided a low value of electron temperature (kT) consistent with the high value of β obtained"
] | [
"Similarities"
] | [
[
1269,
1290
]
] | [
[
1160,
1267
]
] |
2021AandA...650A..56R__Johnson_et_al._2017_Instance_1 | The GRMHD model library is limited in that it has only a few discrete parameter values for the magnetization, black hole spin, and electron temperature distributions. Apart from increasing the number of discrete values, one could think about ways to interpolate between these using, for example, machine learning techniq... | [
"Johnson et al. 2017"
] | [
"The variability within the GRMHD models was found to be an important limitation for constraining black hole parameters, as attested by, for example, the small difference in recovered parameters between the EHT2021 and EHT2021+ arrays. The analysis pipeline may be extended to include a characterization of the sourc... | [
"Future Work",
"Future Work"
] | [
[
879,
898
]
] | [
[
438,
812
],
[
942,
1029
]
] |
2015MNRAS.451..353R__Naray_et_al._2006_Instance_1 | The Λ cold dark matter(ΛCDM) paradigm (Blumenthal et al. 1984) predicted cuspy DM density profiles in the centre of galaxies (Navarro, Frenk & White 1996) and recent results with higher resolution seem to suggest a shallower DM density profile (Navarro et al. 2004, 2010). None the less, the past and newer developments ... | [
"Kuzio de Naray et al. 2006"
] | [
"Many other authors, in an attempt to contribute to the solution of the cuspy-core problem, performed the RC decomposition considering a constant M/L"
] | [
"Background"
] | [
[
977,
1003
]
] | [
[
574,
722
]
] |
2016ApJ...826..168X__Ilgner_&_Nelson_2008_Instance_1 | MRI is considered to be the most promising mechanism driving angular-momentum transport in protoplanetary disks (Balbus & Hawley 1991; Brandenburg et al. 1995; Hawley et al. 1995; Balbus et al. 1996; Balbus & Hawley 1998). However, protoplanetary disks are cold, dense, and, therefore, poorly ionized. The low level of i... | [
"Ilgner & Nelson 2008"
] | [
"Investigations show the layered accretion in the inner disk, where the midplane region is “dead” due to low ionization while the surface layer is “active” due to sufficient ionization"
] | [
"Background"
] | [
[
1361,
1381
]
] | [
[
1090,
1273
]
] |
2017ApJ...846...28R__Kopparapu_et_al._2013_Instance_1 | A question of relevance to life on other planets is whether the Snowball catastrophe occurs at lower radiative forcing at low or high obliquity. There is some conflict in the literature on the role of the Snowball bifurcation in planetary habitability. On the one hand, defining habitability in terms of surface liquid w... | [
"Kopparapu et al. 2013"
] | [
"The traditional habitable zone concept assumes a planet with a functioning silicate-weathering feedback and a positive CO2 greenhouse effect",
"Global glaciation may be triggered on such a planet through a rapid drawdown of atmospheric CO2 that reduces q below the thresholds at which the non-Snowball states disa... | [
"Background",
"Background"
] | [
[
970,
991
]
] | [
[
807,
947
],
[
994,
1169
]
] |
2022MNRAS.515...22J__Newman_et_al._2013_Instance_1 | In Fig. 5, we consider how the velocity dispersion profile scales with radius. Specifically, we plot the power-law index (η) versus the central velocity dispersion (σ0). The vast majority of the galaxies with σ0 ≲ 2.45 are BGGs and these have negative η values. This includes most of the Romulus galaxies (red filled and... | [
"Newman et al. 2013"
] | [
"For σ0 ≳ 2.45, the spread of η for the observed galaxies (e.g.",
"broadens and spans both positive and negative η values. In fact, majority of the galaxies tend to have positive ηs. This change in behaviour is well known."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
690,
708
]
] | [
[
619,
681
],
[
715,
870
]
] |
2018AandA...616A..72W__Käpylä_et_al._2012_Instance_1 | The Sun, our nearest late-type star exhibits a magnetic activity cycle with a period of around 11 yr. The cyclic magnetic field is generated by a dynamo operating below the surface, where it converts the energy of rotating convective turbulence into magnetic energy. We are still far from fully understanding the solar d... | [
"Käpylä et al. 2012"
] | [
"Nowadays, global simulations of convective dynamos are able to reproduce cyclic magnetic fields and dynamo solutions resembling many features of the solar magnetic field evolution"
] | [
"Similarities"
] | [
[
1376,
1394
]
] | [
[
1174,
1353
]
] |
2021ApJ...909...18F__Hon_et_al._2020_Instance_1 | The mechanisms of CL-AGNs are still debated. Early explanations mainly focus on the change in obscuration (Bianchi et al. 2005), while some recent studies favor the change of accretion rate (Stern et al. 2018; Sniegowska et al. 2020). Photoionization research shows that the CL behavior in CL quasars can be fully explai... | [
"Hon et al. 2020"
] | [
"Several groups have been devoted to searching for new CL-AGNs, and tens of candidates have been discovered based on large optical and X-ray surveys, such as the Sloan Digital Sky Survey (e.g.,"
] | [
"Background"
] | [
[
1017,
1032
]
] | [
[
760,
952
]
] |
2021ApJ...909...86X__Mouël_et_al._2017_Instance_1 | The level of solar activity is typically represented by the number or area of sunspots. On the other hand, the “rush-to-the-pole” behavior of PCFs is believed to be one of the precursors for the next solar maximum (Altrock 2014). Figure 3 shows the maximum sunspot numbers (SILSO World Data Center 1914–2020) in comparis... | [
"Le Mouël et al. 2017"
] | [
"Note that even in longer time spans, such as from cycle 1 to 24, the sunspot number seems to vary periodically in different periods, like the often-discussed Gleissberg cycle"
] | [
"Background"
] | [
[
716,
736
]
] | [
[
540,
714
]
] |
2021ApJ...912..106Y__Minchev_et_al._2013_Instance_2 | Our analysis on the LAMOST-RC stars by dissecting the MAPs shows that the chemical bimodality is observed throughout the Galactic disk, and the high- and low-[α/Fe] sequences are corresponding to the thick and thin disks of the Milky Way, respectively. How to explain the formation mechanism of the stellar thin and thic... | [
"Minchev et al. 2013"
] | [
"Radial migration of stars via cold torquing, also known as “churning,” by a bar and spiral waves",
"then allows for the populations to spatially overlap in the solar neighborhood."
] | [
"Uses",
"Uses"
] | [
[
1487,
1506
]
] | [
[
1389,
1485
],
[
1508,
1587
]
] |
2021AandA...653A..32D__Kriek_et_al._2006_Instance_1 | The choice of SFH to infer evolutionary parameters intrinsically carries a degeneracy with the adopted functional form. A more direct approach is to quantify the light-weighted contribution of recent star formation by measuring the relative contribution to the integrated stellar spectrum of short-lived massive stars wi... | [
"Kriek et al. 2006"
] | [
"In Fig. 11 (upper panels) we show the evolution of the spectral break measured through the DB definition",
"as well as the relative strength (the ratio) between the two (lower left panel)."
] | [
"Uses",
"Uses"
] | [
[
1065,
1082
]
] | [
[
959,
1063
],
[
1132,
1212
]
] |
2016AandA...588A...2L__Mätzler_(1998)_Instance_2 | H2O ice on Pluto has long escaped spectroscopic detection, and based on initial New Horizons data appears to be exposed only in a number of specific locations, usually associated with red color, suggestive of water ice/tholin mix (Grundy et al. 2015; Cook et al. 2015). Nonetheless, water ice is likely to be ubiquitous ... | [
"Mätzler 1998"
] | [
"We use the Mishima et al. (1983) formulation (see Appendix of"
] | [
"Uses"
] | [
[
762,
774
]
] | [
[
700,
761
]
] |
2018MNRAS.477..957D__Slee_et_al._2001_Instance_1 | The role of cluster mergers in producing shocks underlying radio relics at cluster peripheries is well supported by observational evidence (Giovannini, Tordi & Feretti 1999; Bagchi et al. 2006; van Weeren et al. 2009; Venturi et al. 2013). A different class of relics, proposed to be fading radio galaxy lobes or such lo... | [
"Slee et al. 2001"
] | [
"Examples of relics in this category are those in",
"and Abell 85"
] | [
"Background",
"Background"
] | [
[
551,
567
]
] | [
[
434,
482
],
[
537,
549
]
] |
2016ApJ...830...15J__Mathieu_et_al._1997_Instance_1 | If PTFO 8-8695 is accreting material onto the star from a gas disk devoid of small grains, the excess Hα emission may result entirely from the accreting material whether or not there is a planetary companion present. This accretion-related emission would presumably be similar to Hα emission seen in other CTTSs, many of... | [
"Mathieu et al. 1997"
] | [
"A few CTTSs binaries are thought to potentially be accreting through accretion streams. These include DQ Tau",
"None of these stars shows the type of Hα variations seen in PTFO 8-8695 where the accretion-related emission appears to move from one side of the line profile to the other as it spirals onto one or bot... | [
"Background",
"Differences"
] | [
[
839,
858
]
] | [
[
710,
818
],
[
1035,
1251
]
] |
2018AandA...617A..86L__Tian_et_al._2016_Instance_1 | Using AIA intensity images in six EUV bandpasses, a differential emission measure (DEM) analysis (Cheng et al. 2012; Shen et al. 2015) is performed for the solar flare at 17:03:37 UT, when the oscillations are pronounced. Figure 8 panels b and c plot the DEM profiles in the flaring loop and the background corona, respe... | [
"Tian et al. 2016",
"Tian et al. 2016"
] | [
"The colored rectangles represent the errors of the DEM curve, which are calculated from 100 Monte Carlo (MC) realizations of the observational data",
"Finally, a number density ratio (rd = n0/ne) of ∼0.02 between outside and inside of the flaring loop is determined, which is very close to the density contrast fr... | [
"Uses",
"Similarities"
] | [
[
676,
692
],
[
1942,
1958
]
] | [
[
508,
655
],
[
1756,
1940
]
] |
2022AandA...666A.141M__Hopkins_et_al._2006_Instance_1 | Many mechanisms that probably lead to quenching have been proposed, and surely we need some parameters to discriminate between these mechanisms. One of such critical parameters we are looking for is the quenching timescale, which varies from one mechanism to another. Most of these timescales are obtained from simulatio... | [
"Hopkins et al. 2006"
] | [
"Quasars’ lifetimes are not long ( 0.1 Gyr,"
] | [
"Background"
] | [
[
714,
733
]
] | [
[
671,
713
]
] |
2015ApJ...808...56M__Beaulieu_et_al._2011_Instance_2 | The field of extrasolar planetary transits is one of the most productive and innovative subject in astrophysics in the last decade. Transit observations can be used to measure the size of planets, their orbital parameters (Seager and Mallén-Ornelas 2003), and stellar properties (Mandel & Agol 2002; Howarth 2011), to st... | [
"Beaulieu et al. 2011"
] | [
"Conventional parametric techniques correct for this effect by dividing the measured flux by a polynomial function of the coordinates of the photometric centroid; some variants may include time-dependence (e.g.,"
] | [
"Background"
] | [
[
1928,
1948
]
] | [
[
1694,
1904
]
] |
2022MNRAS.513.2194I___2017_Instance_1 | There are several assumptions related to the FB origin. One of the first intriguing assumptions of the FB origin was the scenario of the evolution of the relativistic jet remnant. Presumably, relativistic jets existed during the recent activities of Sgr A* about 107 yr ago. These assumptions lead to many interesting di... | [
"Chernyshov et al.",
"2017"
] | [
"There is another possibility of the FB formation due to the tidal disruption of stars",
"and the acceleration of individual particles by the arising shock waves."
] | [
"Background",
"Background"
] | [
[
1010,
1027
],
[
1034,
1038
]
] | [
[
904,
989
],
[
1040,
1112
]
] |
2019ApJ...885..168O__Thomas_et_al._2004_Instance_1 | Tidal heating of Io has been shown to be responsible for its widespread volcanism. The tidal heating rate of Jupiter’s tidally locked moon,
, driven by forced eccentricities, e, locked by Europa and Ganymede’s Laplace resonance with Io, is the dominant interior heating source. Similarly, the tidal heating of an e... | [
"Thomas et al. 2004"
] | [
"At Io, the total neutral volcanic content (SO2, SO, NaCl, KCl, Cl, and dissociation products) ejected to space (Section 4.2.1) by the incident plasma is estimated to be, on average, ∼1000 kg s−1 (e.g.,"
] | [
"Background"
] | [
[
1315,
1333
]
] | [
[
1113,
1314
]
] |
2020ApJ...901...41S__Laursen_et_al._2013_Instance_1 | Observations have shown that the shape of the Lyα line is diverse. It includes broad damped absorption profiles, P-Cygni profiles, double-peak profiles, pure symmetric emission profiles, and combinations thereof (Kunth et al. 1998; Mas-Hesse et al. 2003; Shapley et al. 2003; Møller et al. 2004; Noll et al. 2004; Tapken... | [
"Laursen et al. 2013"
] | [
"Later, numerical algorithms based on Monte Carlo techniques were developed to solve radiative transfer for more general cases. Now theoretical studies mostly rely on them (e.g.,"
] | [
"Background"
] | [
[
1027,
1046
]
] | [
[
640,
817
]
] |
2022MNRAS.514.1961R__Prochaska_&_Zheng_2019_Instance_2 | Along with the time-domain detections, we identified J173438.35-504550.4 as a potential host galaxy for FRB 20201123A using robust statistical treatment given the relatively small localization error region. At face value, the low redshift of J173438.35-504550.4 appears at odds with the large dispersion measure for FRB ... | [
"Prochaska & Zheng 2019"
] | [
"Allowing for the maximum value of this interval (which would imply a significant foreground galaxy halo), we recover a minimum host contribution of ${\\rm DM}_{\\rm host, min} \\approx 60~\\rm pc~cm^{-3}$. This is consistent with estimates for host galaxy contributions from theoretical and empirical treatments"
] | [
"Similarities"
] | [
[
1493,
1515
]
] | [
[
1184,
1491
]
] |
2022ApJ...927..145S__Cui_et_al._2012_Instance_1 | It is generally thought that the stellar halo of the Milky Way (MW) contains the fossil record of the MW’s formation history imprinted in its kinematical and chemical properties. Since Eggen et al. (1962) showed a model of the MW’s formation process from the kinematic analysis of halo stars in the solar neighborhood, m... | [
"Cui et al. 2012"
] | [
"Since Eggen et al. (1962) showed a model of the MW’s formation process from the kinematic analysis of halo stars in the solar neighborhood, many studies of this Galactic fossil component have been carried out using a large number of newly available halo samples, with their assembly requiring considerable observati... | [
"Background",
"Background",
"Background"
] | [
[
750,
765
]
] | [
[
179,
557
],
[
742,
748
],
[
872,
881
]
] |
2020MNRAS.498..385J__Roman-Duval_et_al._2010_Instance_1 | In the upper panel of Fig. 17, we demonstrate that the mass distribution of GMCs in each galaxy reproduces the upper limit of ∼3 to 8 × 106 M⊙ observed by Rosolowsky et al. (2003) in M33, by Freeman et al. (2017) in M83 and by Miville-Deschênes et al. (2017) and Colombo et al. (2019) in the Milky Way. This upper limit ... | [
"Roman-Duval et al. 2010"
] | [
"Above the turnover, the GMC mass function has a power-law form with β ∼ 1.9, close to the observed range of β ∈ [1.6, 1.8] for clouds in the Milky Way"
] | [
"Compare/Contrast"
] | [
[
976,
999
]
] | [
[
761,
911
]
] |
2016MNRAS.459.3585G__Tiengo_&_Mereghetti_2007_Instance_1 | In the following, we consider an NS with mass MNS = 1.5 M⊙ and radius RNS = 12 km, which is compatible with expectations from modern equations of state such as APR or BSk21 models (Akmal, Pandharipande & Ravenhall 1998; Goriely, Chamel & Pearson 2010). The value of the radius is also in agreement with the estimates der... | [
"Tiengo & Mereghetti 2007"
] | [
"The rotational period of RX J1856 is P = 7 s and the X-ray pulsed fraction is the lowest among the XDINSs, ∼1.3 per cent"
] | [
"Background"
] | [
[
647,
671
]
] | [
[
525,
645
]
] |
2020MNRAS.491.5406T__Chisholm_et_al._2017_Instance_1 | We show the mass-loading factors required to simultaneously reproduce the stellar metallicity and SFR of passive galaxies in the bottom panel of Fig. 9. We find that the mass-loading factor strongly decreases with increasing stellar mass. This anticorrelation between stellar mass and λeff is qualitatively consistent wi... | [
"Chisholm et al. 2017"
] | [
"This anticorrelation between stellar mass and λeff is qualitatively consistent",
"as well as other observational evidence (e.g."
] | [
"Similarities",
"Similarities"
] | [
[
625,
645
]
] | [
[
239,
317
],
[
558,
603
]
] |
2022MNRAS.512.4280P__Umetsu_et_al._2016_Instance_2 | The fifth force, propagated by the scalar degree of freedom, affects the Poisson equations associated to the Newtonian potential Φ, as well as the relativistic one, Ψ, according to (Kobayashi, Watanabe & Yamauchi 2015; Crisostomi & Koyama 2018; Dima & Vernizzi 2018),
(1)$$\begin{eqnarray*}
\frac{\text{d} \Phi (r)}{\te... | [
"Umetsu et al. 2016"
] | [
"Moreover, the GR analyses with lensing and internal kinematics of both clusters indicate that the total mass profile is well fitted by the NFW model"
] | [
"Similarities"
] | [
[
2351,
2369
]
] | [
[
2180,
2328
]
] |
2020MNRAS.493.5413K__Dubey_et_al._2009_Instance_1 | As we describe in Section 2 the case of TNDWs propagating in a plasma with equal mass fraction of 12C and 16O (CO) and density of ρ0,7 ≈ 1,1 which is typical for Type Ia supernovae, is particularly challenging for full-star simulations. In addition to the problem that the burning length-scale is much smaller than the t... | [
"Dubey et al. 2009"
] | [
"We test in Section 2 two available one-dimensional (1D) codes:",
"and a modified version of the Eulerian, 1D hydrodynamic flash4.0 code with thermonuclear burning",
"against the ρ0,7 = 1 case.",
"We show that with resolutions that are typical for multidimensional full-star simulations, the V1D and the flash ... | [
"Uses",
"Uses",
"Uses",
"Compare/Contrast"
] | [
[
711,
728
]
] | [
[
416,
478
],
[
592,
688
],
[
731,
757
],
[
758,
994
]
] |
2016MNRAS.462.1415C__Lu_et_al._2014_Instance_1 | Over the last 15 yr, our understanding of how galaxies form and evolve has improved substantially. The combination of technological and theoretical progress has brought this field into a new era: advances in observational techniques (e.g. multi-object spectroscopy, efficient near-infrared CCDs) have enabled multiwavele... | [
"Lu et al. 2014"
] | [
"This progress has led to a general consensus about the main physical ingredients required to describe the evolution of the galaxy population (e.g."
] | [
"Background"
] | [
[
790,
804
]
] | [
[
615,
761
]
] |
2017ApJ...834L..13W__Chang_et_al._2012_Instance_1 | Thanks to their short spectral lags, cosmological distances, and very high-energy photons, GRBs have been viewed as the most promising sources for studying LIV effects (Amelino-Camelia et al. 1998; Ellis et al. 2006; Jacob & Piran 2008). In the past, various limits on LIV have been obtained from the spectral time lags... | [
"Chang et al. 2012"
] | [
"In the past, various limits on LIV have been obtained from the spectral time lags of individual GRBs or a large sample of GRBs (e.g.,"
] | [
"Background"
] | [
[
619,
636
]
] | [
[
239,
372
]
] |
2022MNRAS.512.1499R__Holmbeck_et_al._2019_Instance_1 | The differences in composition are reflected in the final abundances after r-process nucleosynthesis, shown in Fig. 15. The abundances are obtained using a grid of pre-computed trajectories with SkyNet (Lippuner & Roberts 2017), as discussed in detail in Radice et al. (2018b). We normalize the relative abundances by fi... | [
"Holmbeck et al. 2019"
] | [
"Indeed, variability between the yields of different mergers is required to explain observed abundances in metal-poor stars"
] | [
"Uses"
] | [
[
795,
815
]
] | [
[
671,
793
]
] |
2021AandA...656A..79K__Matsumoto_et_al._(1990)_Instance_1 | Theoretical single-ionization cross-sections for the Ar2+ ion are compared to the experimental data in Fig. 2. The cross-sections for other two levels, 3P1 and 3P0, are in close agreement with the values from 3P2 and are therefore not presented. The cross-sections of the direct process are evaluated in the potential of... | [
"Matsumoto et al. (1990)"
] | [
"Measurements from Muller et al. (1980), Danjo et al. (1984), Mueller et al. (1985), and",
"demonstrated onsets below the ionization threshold."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
632,
655
]
] | [
[
544,
631
],
[
656,
707
]
] |
2015MNRAS.447.3936M__Grigorieva_et_al._2007_Instance_1 | We now analyse whether release of this entrapped CO is possible, and quantify it using simple assumptions. In the Fomalhaut ring, the rate at which large planetesimals in the belt are being ground down, which is the same as the rate at which small dust grains are being replenished, has been estimated as 6.0 × 1017 kg y... | [
"Grigorieva et al. 2007"
] | [
"The rate at which water vapour will be released is da/dt ∼ 1.5 × 10−3 μm yr−1 (scaled to the distance of the ring, from the result of",
"), where a is the vertical thickness of the layer."
] | [
"Uses",
"Uses"
] | [
[
1176,
1198
]
] | [
[
1042,
1175
],
[
1198,
1248
]
] |
2021MNRAS.503...13Z__Asplund_et_al._2000_Instance_1 | Although the method developed here is not identical to the means by which SONG determines radial velocity from the observed spectra, it simulates the SONG observations sufficiently well. First, the set of fictitious Fe i lines carefully chosen in this work is able to represent the properties of most Fe i lines seen bet... | [
"Asplund et al. 2000"
] | [
"Due to the complicated physical processes involved in spectral line formation in a 3D atmosphere (e.g.",
"it is difficult to quantify higher order effects beyond the linear relation between $\\mathfrak {v}$ and Wλ; that is, the systematic uncertainty of the linear fitting."
] | [
"Uses",
"Compare/Contrast"
] | [
[
970,
989
]
] | [
[
867,
969
],
[
992,
1158
]
] |
2022MNRAS.510.6085L__Tafalla_&_Hacar_2015_Instance_1 | Filamentary structures have been found at almost all size scales in the Galaxy. Massive, long filamentary dark clouds are commonly found inside giant molecular clouds (GMCs; e.g. Bergin & Tafalla 2007; André et al. 2014, and references therein), such as the dark clouds L1495 in the Taurus cloud complex (e.g. Chapman et... | [
"Tafalla & Hacar 2015"
] | [
"Dense cores, where stars form, are located along or at the intersections of some of these fine substructures (e.g."
] | [
"Background"
] | [
[
1605,
1625
]
] | [
[
1469,
1583
]
] |
2022MNRAS.517.1313M__Krumholz_&_McKee_2005_Instance_1 | Star formation is an inefficient process, as evidenced by observed gas depletion times,1 which are two orders of magnitude above the dynamical time, both in galaxies (e.g. Leroy et al. 2017; Utomo et al. 2018), and in individual giant molecular clouds (GMCs) (e.g. Krumholz & Tan 2007; Evans, Heiderman & Vutisalchavakul... | [
"Krumholz & McKee 2005"
] | [
"Theoretical models explain this inefficiency through a combination of mechanisms that provide support against gravitational collapse, including turbulence, magnetic fields, stellar feedback, and dynamical stabilization"
] | [
"Background"
] | [
[
604,
625
]
] | [
[
384,
602
]
] |
2022MNRAS.515.5495M__Gallazzi_et_al._2008_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... | [
"Gallazzi et al. 2008"
] | [
"Currently, a limited number of observations",
"are available to explore the environment dependence of the metallicity"
] | [
"Background",
"Background"
] | [
[
1138,
1158
]
] | [
[
1093,
1136
],
[
1205,
1275
]
] |
2019AandA...625A.114J__Tacconi_et_al._2018_Instance_1 | Although most galaxies have an implied SFR that scatters within a factor two around the MS, some do show a significantly higher SFR. Those objects also exhibit a higher gas content, shorter gas depletion times (e.g., Genzel et al. 2015; Schinnerer et al. 2016; Tacconi et al. 2013, 2018), and higher dust temperatures (e... | [
"Tacconi et al.",
"2018"
] | [
"Although most galaxies have an implied SFR that scatters within a factor two around the MS, some do show a significantly higher SFR. Those objects also exhibit a higher gas content, shorter gas depletion times (e.g.,"
] | [
"Background"
] | [
[
261,
275
],
[
282,
286
]
] | [
[
0,
216
]
] |
2015AandA...576A...5C__Christen_&_Müller_(2003)_Instance_1 | Using the CASSIS2 software, we detected 8 lines of glycolaldehyde, 31 lines of the aGg′ conformer of ethylene glycol, and 26 lines of methyl formate (see Table 1). The glycolaldehyde and methyl formate transitions are taken from the JPL spectroscopic database (Pickett et al. 1998), while the ethylene glycol transitions... | [
"Christen & Müller (2003)"
] | [
"The predictions are based on experimental data from",
"for ethylene glycol"
] | [
"Uses",
"Uses"
] | [
[
551,
575
]
] | [
[
375,
426
],
[
576,
595
]
] |
2017ApJ...837..109L__parsec,_Cisternas_et_al._2013_Instance_1 | It has been generally believed (see Kormendy & Ho 2013; Kormendy 2016, for recent reviews) that, unlike massive galaxies at high redshifts (e.g.,
) whose evolution is driven by a major merger, low-redshift galaxies largely evolve through secular evolution (i.e., in a slow and gentle manner) driven by internal pro... | [
"Cisternas et al. 2013"
] | [
"It has also been generally believed accordingly that most activity (namely active galactic nuclei—AGNs) of supermassive black holes (BHs) at the centers of galaxies at low redshifts",
"appear to be fueled by the random accretion of gas via internal, secular processes working close to the BH (say, within a few hu... | [
"Background",
"Background"
] | [
[
941,
962
]
] | [
[
534,
715
],
[
799,
940
]
] |
2021AandA...656A.148R__in_2012_Instance_1 | After the gravitational collapse and if the total mass of the individual cloud is approximately the mass of the Sun (2 × 1030 Kg; (van Dishoeck 2014), a new astrophysical system forms that is dominated gravitationally by a low-mass protostar known as a young stellar object (YSO). The protostar is in the center of the s... | [
"Jørgensen et al. 2012"
] | [
"Additionally, glycolaldehyde (C2 H4O2), the simplest form of sugar and one of the first intermediates in the formose reaction",
", has also been detected in this object for the first time in space in 2012"
] | [
"Background",
"Background"
] | [
[
1728,
1749
]
] | [
[
1503,
1628
],
[
1651,
1726
]
] |
2021ApJ...909...65K__Liu_et_al._2014_Instance_1 | Various groups around the world have proposed different models to explain the formation of these two peculiar classes of SNe Ia. Sub-Chandrasekhar limiting-mass WDs were believed to be formed by merging two sub-Chandrasekhar mass WDs (double-degenerate scenario), leading to another sub-Chandrasekhar mass WD, exploding ... | [
"Liu et al. 2014"
] | [
"On the other hand, the super-Chandrasekhar WDs were often explained by incorporating different physics, such as a",
"presence of charge in the WDs"
] | [
"Background",
"Background"
] | [
[
720,
735
]
] | [
[
406,
519
],
[
689,
718
]
] |
2015MNRAS.451.1528P__Brun_et_al._2014_Instance_1 | Currently, there is an extensive data base of observations of magnetic activity on the main-sequence stars (see e.g. reviews by Donati & Landstreet 2009; Reiners 2012). Cool stars with outer convective envelope are of particular interests because they are Sun-like. It is believed that the magnetic activity on the solar... | [
"Brun et al. 2014"
] | [
"and the 3D numerical simulations",
"show that parameters of the differential rotation and convection, e.g. the typical size and turnover time of convective flows, depend on the general stellar parameters, such as mass, age, the spectral class and the rotation rate."
] | [
"Background",
"Background"
] | [
[
859,
875
]
] | [
[
757,
789
],
[
912,
1141
]
] |
2015AandA...579A..51B__Egan_et_al._1998_Instance_1 | Even though the understanding of high-mass star formation has made tremendous progress over the past decade (Beuther et al. 2007; Zinnecker & Yorke 2007; Klessen 2011; Tan et al. 2014), the initial conditions are still poorly constrained. It is known, that stars predominantly form in clusters (Lada & Lada 2003), which ... | [
"Egan et al. 1998"
] | [
"They were discovered as dark silhouettes against the galactic background at 8 and 15 μm with the Midcourse Space Experiment (MSX,"
] | [
"Uses"
] | [
[
1317,
1333
]
] | [
[
1187,
1316
]
] |
2019MNRAS.488.5029H__Malhotra_et_al._2001_Instance_2 | For the first time, we detected [C ii] 158-μm emission from a GRB host galaxy at z > 2. This is the second detection of [C ii] 158-μm emission among known GRB host galaxies, following GRB 980425 (Michałowski et al. 2016). The [C ii] 158-μm fine structure line is the dominant cooling line of the cool interstellar medium... | [
"Malhotra et al. 2001"
] | [
"The comparison sample is compiled from the literature up to z ∼ 3"
] | [
"Uses"
] | [
[
1410,
1430
]
] | [
[
1343,
1408
]
] |
2019AandA...630A.131M__Molina_et_al._2009_Instance_1 | X-rays emerging from active galactic nuclei (AGNs) are the result of an inverse-Compton process occurring in the proximity of the central black hole (BH), where optical-UV photons arising from the accretion disc are inverse-Compton scattered by hot electrons in an optically thin, compact corona (e.g. Haardt & Maraschi ... | [
"Molina et al. 2009",
"Molina et al. 2009"
] | [
"Such a Comptonisation mechanism accounts for the power-law-like shape of the X-ray primary continuum emission and the high-energy roll-over observed in various nearby AGNs (e.g.",
"while similar works were performed on INTEGRAL data (e.g."
] | [
"Background",
"Background"
] | [
[
630,
648
],
[
1511,
1529
]
] | [
[
389,
566
],
[
1432,
1489
]
] |
2021ApJ...906..105C__Huang_et_al._2019_Instance_1 | Even though Ω is only a function of Ψ, the physical connection between the two at the foot-point is not very obvious.9
9
They may be constrained by proper boundary conditions (e.g., Contopoulos et al. 2013).
Likely most researchers, here we assume that they generally follow the ansatz
13
In the region approachin... | [
"Huang et al. 2019"
] | [
"Physically, it is the rotation that develops a toroidal magnetic field and a poloidal electric field in the lab frame (or the inertial frame), which seems to imply that Φ would not be chosen arbitrarily and would be self-consistently determined by the MHD equations, given the Ψ and Ω specified (e.g.,"
] | [
"Background"
] | [
[
1526,
1543
]
] | [
[
1171,
1472
]
] |
2018AandA...611A..74R__Grady_et_al._2013_Instance_1 | In this context, MWC 758 (HD 36112) offers a unique environment to probe the existence of planetary companions and to explore the connection between disk structures and planet formation. MWC 758 is a young stellar object (3.5 ± 2 Myr, Meeus et al. 2012) at a distance of 151
$^{+9}_{-8}$
151
−9
+8
4
pc (Ga... | [
"Grady et al. 2013"
] | [
"Based on its SED, MWC 758 has been classified as a pre-transition disk"
] | [
"Background"
] | [
[
1120,
1137
]
] | [
[
1048,
1118
]
] |
2022AandA...661A..10B__Ghirardini_et_al._2021a_Instance_4 | It is also possible that these clusters have a smaller extent and can just be missed by our extent selection as our detection algorithm sets the extent to zero if it is smaller than 6 (Brunner et al. 2022). Following the method presented in Ghirardini et al. (2021a), we estimated several dynamical properties of the clu... | [
"Ghirardini et al. 2021a"
] | [
"The distribution of number density, core radius, and concentration parameter remains the same, indicating that the population of clusters in the point source catalog is more compact than the extent-selected sample. The extent-selected sample does not show a clear bias toward cool-core clusters or clusters with a c... | [
"Compare/Contrast",
"Differences"
] | [
[
1967,
1990
]
] | [
[
1566,
1965
],
[
1993,
2039
]
] |
2017ApJ...849..109P__Lee_et_al._2014_Instance_1 | Lastly, we model the evolution of the ejecta discussed in Section 2.2 into circumstellar profiles discussed in Section 2.3. We use our cosmic-ray hydrodynamics code, hereafter called ChN to model the evolution of the ejecta to an age of
t
SNR
=
400
yr. ChN is a Lagrangian hydrodynamics code that includes ... | [
"Lee et al. 2014"
] | [
"and have coupled the code to SN ejecta models"
] | [
"Uses"
] | [
[
575,
590
]
] | [
[
528,
573
]
] |
2022MNRAS.509.5155R__Richard_et_al._2009_Instance_1 | In addition to being useful laboratories for studying the evolution of galaxies in dense environments, galaxy clusters can be effective gravitational lenses (for a review, see Kneib & Natarajan 2011). Gravitational lensing is the deflection of light by intervening mass, that can produce highly magnified and distorted i... | [
"Richard et al. 2009"
] | [
"The large mass and solid angle covered by highly concentrated galaxy clusters make them ideal gravitational lenses, which can be used as ‘cosmic telescopes’ to observe very distant galaxies (e.g."
] | [
"Uses"
] | [
[
546,
565
]
] | [
[
350,
545
]
] |
2020MNRAS.498.6069P__Dressler_1980_Instance_1 | The present Universe is full of galaxies that come in various shapes and sizes with different mass, luminosity, colour, star formation rate (SFR), metallicity, and H i content. Understanding the galaxy properties and their evolution is an important goal of cosmology. The modern galaxy surveys, 2dF Galaxy Redshift Surve... | [
"Dressler 1980"
] | [
"For example, the well-known density–morphology relation reveals that the ellipticals are preferably found inside the dense groups and clusters, whereas the spirals are intermittently distributed in the fields"
] | [
"Background"
] | [
[
964,
977
]
] | [
[
715,
923
]
] |
2015MNRAS.446.3002B__Diemand,_Moore_&_Stadel_2004_Instance_1 | We recall that the velocity anisotropy profile is given by a combination of the radial and tangential velocity dispersion:
(15)
\begin{equation}
\beta _{\rm ani}(r)\equiv 1-\frac{\bar{v_{\theta }^2}(r)}{\bar{v_r^2}(r)}\,.
\end{equation}
Due to the lack of observational constraints on this quantity, the first anisotr... | [
"Diemand, Moore & Stadel 2004"
] | [
"More recently, indications of radial anisotropy in the outer regions of DM haloes have been obtained from numerical simulations (e.g."
] | [
"Background"
] | [
[
840,
868
]
] | [
[
706,
839
]
] |
2017MNRAS.471.3057M__Bovy_et_al._2016b_Instance_1 | We have performed the first detailed dissection of the stellar populations of the Milky Way disc in age, [Fe/H] and $\mathrm{[ \alpha \mathrm{/Fe]}}$ space, bridging the gap between the detailed observational understanding of MAPs (e.g. Bovy et al. 2012b, 2016b) and the plethora of studies of co-eval stellar population... | [
"Bovy et al.",
"2016b"
] | [
"We have performed the first detailed dissection of the stellar populations of the Milky Way disc in age, [Fe/H] and $\\mathrm{[ \\alpha \\mathrm{/Fe]}}$ space, bridging the gap between the detailed observational understanding of MAPs (e.g."
] | [
"Extends"
] | [
[
237,
248
],
[
256,
261
]
] | [
[
0,
236
]
] |
2021AandA...652A.117B__Rieder_&_Kenworthy_2016_Instance_1 | Ring systems are a ubiquitous feature in planetary systems – all the gas giants in the Solar System have ring systems around them of varying optical depths (see, e.g., Tiscareno 2013; Charnoz et al. 2018), and ring systems have been detected around minor planets (e.g., Chariklo; Braga-Ribas et al. 2014), so it is reaso... | [
"Rieder & Kenworthy 2016"
] | [
"In 2007, it displayed a complex symmetric dimming pattern of up to ~ 3 magnitudes during a 56 day eclipse. This has been attributed to the transit of a substellar companion (called “J1407 b”) with a mass of 60–100 MJup"
] | [
"Background"
] | [
[
1357,
1380
]
] | [
[
1137,
1355
]
] |
2020AandA...644A.159C__Titov_&_Lambert_2013_Instance_1 | In order to try to get insights into such systematics, we produced several variants of the ICRF3 S/X band frame by changing the reference epoch of the catalog or alternately by not considering Galactic acceleration in the modeling. Interestingly, the D2 and D3 glide terms for these variants were found to vary by severa... | [
"Titov & Lambert 2013"
] | [
"Interestingly, the D2 and D3 glide terms for these variants were found to vary by several tens of microarcseconds in the comparison to ICRF2, in line with the level of the systematics observed for those terms. Such findings are not unexpected since Galactic acceleration manifests itself as a dipolar deformation in... | [
"Similarities"
] | [
[
578,
598
]
] | [
[
232,
577
]
] |
2019ApJ...870...39V__Veron-Cetty_&_Veron_1986_Instance_1 | NGC 3557 is a bona fide southern-sky elliptical galaxy (E3) at a distance of 40 Mpc (1″ is 198 pc at this distance7
7
For distance derivations, we have assumed a cosmology model with H0 =73 km s−1 Mpc−1, Ωmatter = 0.27, and Ωvacuum = 0.73.
), and a member of a small group of galaxies (Brough et al. 2006). It has been ... | [
"Veron-Cetty & Veron 1986"
] | [
"Nuclear optical line emission has been reported from spectroscopy"
] | [
"Background"
] | [
[
827,
851
]
] | [
[
760,
825
]
] |
2020ApJ...889...15Y__Yang_et_al._2016b_Instance_1 | 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"
] | [
"There is some tentative evidences for alignment with respect to the magnetic field",
"in, e.g., the IRAS 4A system at cm wavelengths"
] | [
"Motivation",
"Motivation"
] | [
[
866,
883
]
] | [
[
559,
641
],
[
801,
847
]
] |
2018ApJ...860...24P__Warmuth_2015_Instance_1 | Figure 13 shows the temporal evolution of the density, ρ, plasma flow velocity, vx, position of the wave crest, PosA, phase speed, vw, and magnetic field component in the z-direction, Bz, for the primary waves in every different case of initial amplitude, ρIA. In Figure 13(a), we observe that the amplitude of the densi... | [
"Warmuth 2015"
] | [
"For the case of ρIA = 1.3 (magenta), a decrease of the amplitude of the primary can hardly be observed, as expected for low-amplitude wave"
] | [
"Similarities"
] | [
[
714,
726
]
] | [
[
574,
712
]
] |
2019AandA...623A..11P__Simm_et_al._2016_Instance_1 | Another clear difference for Ark 120 with the NT thin disc predictions is the variability. From the best simultaneous fit of the 2013 and 2014 observations, we infer a significant increase in mass accretion rate through the disc from 0.03 to 0.07 Lbol/LEdd in only one year, but a standard thin disc around a SMBH cannot... | [
"Simm et al. 2016"
] | [
"Similar rapid changes in the optical-UV flux are typically seen in other BLS1s, especially those at low Lbol/LEdd (e.g."
] | [
"Similarities"
] | [
[
979,
995
]
] | [
[
822,
941
]
] |
2021ApJ...914L..19Z__Metzger_et_al._2008_Instance_1 | Thermonuclear explosions and AICs of WDs in AGN disks are potential sources for future joint gravitational wave (GW), EM, and neutrino multi-messenger observations. In addition to AIC of WDs, another possible formation channel of millisecond magnetars in AGN disks is mergers of BNSs. Such a merger may produce a millise... | [
"Metzger et al. 2008"
] | [
"The mechanism by which a nascent millisecond magnetar might power a GRB jet has been studied in detail over the past decade"
] | [
"Background"
] | [
[
629,
648
]
] | [
[
473,
596
]
] |
2022AandA...668A..10F__Walker_et_al._2008_Instance_1 | The most common approaches to observe SPI are spectral observations of typical emission lines for stellar chromospheres and coronae. The earliest approach to observe SPI dates back to the early 2000’s and focused on non-thermal chromospheric Ca II H and K emissions (Shkolnik et al. 2003). Subsequent studies by Shkolnik... | [
"Walker et al. 2008"
] | [
"Other authors observed different systems and likewise saw chro-mospheric excess emissions"
] | [
"Background"
] | [
[
583,
601
]
] | [
[
492,
581
]
] |
2022MNRAS.514.2974M__Dadina_2007_Instance_1 | Active galactic nuclei (AGNs) are extragalactic sources that emit across the whole electromagnetic spectrum. Such systems are composite and each sub-structure has its own role in shaping the emerging spectrum (see Padovani et al. 2017, for a comprehensive review). It is ubiquitously accepted that the X-ray emission ori... | [
"Dadina 2007"
] | [
"In fact, the X-ray continuum in AGNs is well modelled by a power law with a high energy roll-over (e.g."
] | [
"Background"
] | [
[
1080,
1091
]
] | [
[
956,
1059
]
] |
2017AandA...608A..16R__Ravindranath_et_al._2006_Instance_1 | The measurement of clumps at redshifts beyond the peak of cosmic star formation is notoriously difficult. The identification of clumpy galaxies in the dominant population of irregular galaxies at high redshift dates back to the first deep Hubble Space Telescope (HST) images (e.g., Williams et al. 1996). Subsequent stud... | [
"Ravindranath et al. 2006"
] | [
"The fraction of clumpy galaxies was studied from z = 0 up to the most distant galaxies identified today at z ~ 10"
] | [
"Background"
] | [
[
831,
855
]
] | [
[
716,
829
]
] |
2020MNRAS.499.1788W__Wolfire_et_al._2003_Instance_2 | Owing to their brightness at rest-frame FIR wavelengths, the ionized and neutral species of Carbon, Nitrogen, and Oxygen are powerful diagnostic lines for tracing the ISM of nearby and distant galaxies. When combined with photodissociation region (PDR) models (Tielens & Hollenbach 1985), measurement of the emission fro... | [
"Wolfire et al. 2003"
] | [
"Another major coolant of the ISM is [O i]63 μm"
] | [
"Background"
] | [
[
1199,
1218
]
] | [
[
1151,
1197
]
] |
2021MNRAS.503..324M__Zhao_et_al._2019_Instance_1 | We first determined the orbital parameters for RS Ser, V449 Per, and V1095 Her. Further, we updated the parameters for V593 Cen and MR Del. Using the formula f = (Ωin – Ω1)/(Ωin – Ωout), we calculated the contact factors f for RS Ser, V593 Cen, and V1095 Her as 6.5 per cent, 40 per cent, and 53 per cent, respectively.... | [
"Zhao et al. (2019)"
] | [
"For V593 Cen, we updated the orbital parameters using more complete light curves. The orbital inclination of 83°.18 is similar to the result (82°.6) obtained by"
] | [
"Similarities"
] | [
[
580,
598
]
] | [
[
419,
579
]
] |
2020MNRAS.494.2851C__Dijkstra_et_al._2008_Instance_1 | Previously it has been postulated that the SMS formation by DC is only possible in atomic cooling haloes both with intense FUV irradiation and with primordial gas composition. Here we have shown that SMSs can form also in slightly metal-enriched cases as long as FUV irradiation is intense enough. This relaxation of the... | [
"Dijkstra et al. 2008"
] | [
"Using the critical intensity advocated by recent studies",
"this ranges from a few Gpc−3 (e.g.",
"to 10−6 to 10−4 Mpc−3"
] | [
"Compare/Contrast",
"Compare/Contrast",
"Compare/Contrast"
] | [
[
695,
715
]
] | [
[
534,
590
],
[
660,
694
],
[
753,
774
]
] |
2020MNRAS.492.3509B__Garsden_et_al._2015_Instance_1 | In the context of RI imaging techniques, the standard clean algorithm implements a non-linear, greedy approach to perform deconvolution in an iterative manner (Högbom 1974). Working pixelwise, clean implicitly assumes sparsity of the sought image, removing at each iteration, a fraction of the maximum intensity pixel co... | [
"Garsden et al. 2015"
] | [
"In addition to these clean-based approaches, recent developments in the field of compressive sensing (CS) applied for astronomical imaging have given birth to many imaging algorithms, particularly for RI",
"Leveraging optimization frameworks, these methods aim to solve the underlying image recovery problem by en... | [
"Background",
"Background"
] | [
[
776,
795
]
] | [
[
521,
724
],
[
817,
989
]
] |
2022MNRAS.517.5473G__Kapanadze_et_al._2018_Instance_1 | Various outbursts in GeV–TeV energies from 1ES 1959+650 have been reported by Fermi-LAT and several ground-based Cherenkov experiments like VERITAS, MAGIC, FACT (Albert et al. 2006; Aliu et al. 2014; Biland et al. 2016) including a new highest historical γ-ray activity, detected by MAGIC collaboration on 2016 June 13–1... | [
"Kapanadze et al. 2018"
] | [
"Unprecedented flux and spectral variability during these episodes have been observed"
] | [
"Background"
] | [
[
1132,
1153
]
] | [
[
1012,
1096
]
] |
2019MNRAS.488.5671I__Inoue_&_Iwata_2008_Instance_1 | While both Suprime-Cam/NB359 and HST/F336W trace LyC for sources at z > 3.06, NB359 has a narrower filter bandpass, and it preferentially captures ionizing photons closer to the Lyman limit (see Fig. 1). Because IGM attenuation varies as a function of wavelength, expected transmissions of photons through the IGM (here ... | [
"Inoue & Iwata 2008"
] | [
"These IGM transmissions are estimated from Monte Carlo simulations (",
") which generate 10 000 sightlines for redshifts consistent with the H i cloud distribution defined analytically by Inoue et al. (2014)."
] | [
"Uses",
"Uses"
] | [
[
657,
675
]
] | [
[
589,
657
],
[
675,
811
]
] |
2018MNRAS.477.4308R__Novak,_Ostriker_&_Ciotti_2011_Instance_1 | It is well known that the accretion on to compact objects may influence the nearby ambient around SMBHs in the centre of galaxies (e.g. Salpeter 1964; Fabian 1999; Barai 2008; Germain, Barai & Martel 2009). Together with the outflow phenomena, it is believed to play a major role in the feedback processes invoked by mod... | [
"Novak, Ostriker & Ciotti 2011"
] | [
"The problem of accretion on to an SMBH has been studied via hydrodynamical simulations (e.g."
] | [
"Background"
] | [
[
742,
771
]
] | [
[
549,
641
]
] |
2019MNRAS.485.5453S__Morlino_et_al._2012_Instance_1 | As well as being directly excited from the ground state, Balmer lines (intensity, line profile, polarization and so on) are affected by the conversion of Lyman lines to Balmer lines. For example, the absorption of Ly β by a hydrogen atom results in radiative excitation from 1s to 3p, and the excited atom can emit H α b... | [
"Morlino et al. 2012"
] | [
"Although such fundamental physics is well known, it has not been well studied in SNR shocks. In fact, it is usually assumed that the Ly β photons are at the limits of either completely optically thick or optically thin at SNR shocks, i.e. they are completely converted to H α photons or not at all (e.g."
] | [
"Compare/Contrast"
] | [
[
1050,
1069
]
] | [
[
699,
1002
]
] |
2020ApJ...899..120T__Chou_et_al._2008_Instance_1 | The energy dependent pulse arrival time can usually be observed in AMXPs. Soft lags are most often seen in AMXPs, where the pulse arrival times of the pulsations from softer energy bands lag compared to the ones from the harder energy bands. This phenomenon was first discovered by Cui et al. (1998) during the 1998 outb... | [
"Chou et al. 2008"
] | [
"Similar energy dependent pulse arrival time behavior can also be found in",
"and XTE J1807–294",
"with different break point energies."
] | [
"Background",
"Background",
"Background"
] | [
[
748,
764
]
] | [
[
528,
601
],
[
729,
746
],
[
766,
802
]
] |
2015ApJ...805....4Z__Terradas_et_al._2015_Instance_1 | Solar prominences or filaments are cool, dense plasmas embedded in the million-Kelvin corona (Mackay et al. 2010). The plasmas originate from the direct injection of chromospheric materials into a pre-existing filament channel, levitation of chromospheric mass into the corona, or condensation of hot plasmas from the ch... | [
"Terradas et al. 2015"
] | [
"Prominences are generally believed to be supported by the magnetic tension force of the dips in sheared arcades"
] | [
"Background"
] | [
[
569,
589
]
] | [
[
438,
549
]
] |
2019AandA...631A..88Y__Bohren_&_Huffman_(1998)_Instance_2 | Starting from the four aforementioned materials, we consider several composition mixtures and grain structures. For the sake of comparison, we first consider compact grains of purely a-Sil, a-C, or a-C:H. Subsequently, according to Köhler et al. (2015), we consider compact grains made of two thirds a-Sil and one third ... | [
"Bohren & Huffman 1998"
] | [
"For grains consisting of two or three materials, we first derive effective optical constants following the Maxwell Garnett mixing rule"
] | [
"Uses"
] | [
[
1542,
1563
]
] | [
[
1384,
1518
]
] |
2022AandA...663A..15W__Widmark_et_al._2021a_Instance_1 | The dynamics of stars can be related to the gravitational potential that they inhabit via the collisionless Boltzmann equation. For systems in a steady state with certain symmetry properties (typically spherical or axisymmetric) it is possible to find solutions to the phase-space distribution of a stellar tracer popula... | [
"Widmark et al. 2021a"
] | [
"The dynamics of stars can be related to the gravitational potential that they inhabit via the collisionless Boltzmann equation. For systems in a steady state with certain symmetry properties (typically spherical or axisymmetric) it is possible to find solutions to the phase-space distribution of a stellar tracer p... | [
"Background"
] | [
[
649,
669
]
] | [
[
0,
417
]
] |
2018AandA...618A.128C__Kenney_et_al._2004_Instance_1 | In addition to the galaxy mergers, the ram pressure may also induce AGN activity together to star formation in cluster galaxies (e.g., Poggianti et al. 2017; Marshall et al. 2018; Ramos-Martínez et al. 2018). The ram pressure, acting on galaxies in a galaxy cluster moving through the intra-cluster medium (ICM), can str... | [
"Kenney et al. 2004"
] | [
"A good example of this effect is the Virgo cluster, the closest rich galaxy cluster, considered a ram pressure stripping laboratory since a number of clearly ram pressure stripped galaxies have been observed (e.g.,"
] | [
"Background"
] | [
[
828,
846
]
] | [
[
613,
827
]
] |
2016MNRAS.463.4121T__Brouillet_et_al._2005_Instance_2 | Molecular line ratio diagrams for NGC 4710, NGC 5866 and a variety of other galaxies. Our data for NGC 4710 and NGC 5866 are shown as filled circles and squares, respectively, while our data for the nuclear discs and inner rings are shown in blue and red, respectively (black for the intermediate region). Upper and lowe... | [
"Brouillet et al. 2005"
] | [
"The HCN(1–0)/HCO+ ratios for M31 GMCs",
"are indicated by the turquoise shaded region in panels c and d."
] | [
"Uses",
"Uses"
] | [
[
1631,
1652
]
] | [
[
1592,
1629
],
[
1654,
1717
]
] |
2022MNRAS.516..731B__Hattori,_Valluri_&_Vasiliev_2021_Instance_1 | Now with the recent availability of high quality full 6D phase-space information for large numbers of sources, much effort has been made to decrease the uncertainties in the Milky Way mass estimate. Recent works using a tracer mass estimator with 6D phase-space information include Sohn et al. (2018, globular clusters),... | [
"Hattori, Valluri & Vasiliev 2021"
] | [
"Using Bayesian analysis to fit",
"and a similar distribution function analysis using 5D phase-space data from Gaia"
] | [
"Background",
"Background"
] | [
[
1157,
1189
]
] | [
[
720,
750
],
[
1075,
1155
]
] |
2018ApJ...866L...1S__Pecharromán_et_al._1999_Instance_2 | It was found that the complex dielectric function from Pecharromán et al. (1999) for the sample obtained by heating bayerite at 1273 K, assuming a spheroid with depolarization parameters of (0.35, 0.003), produced an opacity with 11, 20, 28, and 32 μm features, so this component was included in the models. However, wit... | [
"Pecharromán et al. (1999)"
] | [
"This was done using the complex dielectric function for the sample obtained by heating boehmite at 1173 K from",
"assuming a spheroid with depolarization parameters of (0.35, 0.035)."
] | [
"Uses",
"Uses"
] | [
[
680,
705
]
] | [
[
569,
679
],
[
707,
775
]
] |
2018ApJ...854...63O__Nakamura_et_al._2015_Instance_1 | Many of the earliest simulations of core-collapse supernovae used or were concerned with a general relativistic (GR) approach (Misner & Sharp 1964; Colgate & White 1966; May & White 1966; Wilson 1971; Bruenn 1985; Burrows 1988), and rightly so since neutron stars are sufficiently compact that GR dramatically effects th... | [
"Nakamura et al. 2015"
] | [
"While the importance of including GR gravity in simulations of core-collapse supernovae has always persisted in the literature and is in use in many current and state-of-the-art multidimensional, core-collapse supernova calculations",
"many modern simulations have used a purely Newtonian approximation for gravit... | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
930,
950
]
] | [
[
347,
579
],
[
747,
825
]
] |
2017MNRAS.464..635M__Ceverino_et_al._2012_Instance_1 | 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... | [
"Ceverino et al. 2012"
] | [
"This has been shown using",
"as well as cosmological simulations"
] | [
"Background",
"Background"
] | [
[
803,
823
]
] | [
[
467,
492
],
[
713,
748
]
] |
2021MNRAS.504.1473L__Muñoz,_Miranda_&_Lai_2019_Instance_1 | Large numbers of works have extensively studied the binary-disk system in the Newtonian regime with analytic methods (Paczynski 1977; Papaloizou & Pringle 1977; Kocsis, Haiman & Loeb 2012a, b) and hydrodynamical simulations (Lin & Papaloizou 1979; Artymowicz & Lubow 1994; MacFadyen & Milosavljević 2008; Mayama et al. 2... | [
"Muñoz, Miranda & Lai 2019"
] | [
"Large numbers of works have extensively studied the binary-disk system in the Newtonian regime with",
"and hydrodynamical simulations"
] | [
"Background",
"Background"
] | [
[
565,
590
]
] | [
[
0,
99
],
[
193,
223
]
] |
2021ApJ...910...82L__Schrijver_2001_Instance_1 | Similar results of the on-disk condensations are obtained to those of the on-disk quiescent coronal rain in AR closed loops in Hα (see Section 3.2). If we considered the AIA 304 Å observations alone, the on-disk condensation, and hence coronal rain events we report here would resemble those occurring in magnetically cl... | [
"Schrijver 2001"
] | [
"If we considered the AIA 304 Å observations alone, the on-disk condensation, and hence coronal rain events we report here would resemble those occurring in magnetically closed field lines",
"which are generally interpreted as a manifestation of the heating-condensation cycles due to thermal nonequilibrium",
"H... | [
"Compare/Contrast",
"Compare/Contrast",
"Compare/Contrast"
] | [
[
531,
545
]
] | [
[
149,
336
],
[
414,
529
],
[
588,
840
]
] |
2022MNRAS.514.5178D__Ruderman_&_Roberts_2002_Instance_1 | There are several natural scenarios for the initial flare-caused impulsive perturbation of an active region to develop into a quasi-periodic response, which includes the effects of resonance in closed coronal plasma structures (acting as resonators), dispersion of a wave-guide, and non-linearity/self-organization (McLa... | [
"Ruderman & Roberts 2002"
] | [
"More specifically, fast- and slow-mode magnetoacoustic waves in coronal plasma structures are well-known to be subject to a frequency-dependent damping by e.g. resonant absorption and thermal conduction (e.g."
] | [
"Uses"
] | [
[
953,
976
]
] | [
[
719,
927
]
] |
2018AandA...615A..77L__Tacconi_et_al._2010_Instance_1 | A different approach is to count the amount of baryonic material within the proto-cluster bounds associated with the member galaxies and attempt to relate that back to the overall mass of the structure, an approach which has been employed successfully at low redshift when the galactic baryonic content of cluster member... | [
"Tacconi et al. 2010"
] | [
"Here we additionally make the assumption that stellar mass comprises 50% of the baryonic content of galaxies by mass at these redshifts, a value broadly consistent with the few measurements made at or near these redshifts (e.g.,"
] | [
"Uses"
] | [
[
1362,
1381
]
] | [
[
1133,
1361
]
] |
2020ApJ...904..185O__Takakuwa_et_al._2014_Instance_1 | Recently, rotationally supported disks have been found not only in Class I sources but also in some Class 0 sources (e.g., Murillo et al. 2013; Yen et al. 2013, 2017; Ohashi et al. 2014; Tobin et al. 2015, 2016b, 2016a; Seifried et al. 2016; Aso et al. 2017; Lee et al. 2017; Okoda et al. 2018). In spite of these extens... | [
"Takakuwa et al. 2014"
] | [
"Moreover, the disk formation process has been revealed to be much more complicated for binary and multiple cases, both in observations"
] | [
"Background"
] | [
[
617,
637
]
] | [
[
441,
575
]
] |
2019ApJ...871..191O__Vaucouleurs_et_al._1991_Instance_1 | NGC 4418 is one of the closest and best-studied galaxies hosting CONs. It is an LIRG with its 8–1000 μm infrared luminosity (LIR) of 1.4 × 1011 L (Sanders et al. 2003)4
4
With our assumed distance, the luminosity is larger than the threshold for the LIRG classification of LIR = 1 × 1011 L (Sanders & Mirabel 1996). We ... | [
"de Vaucouleurs et al. 1991"
] | [
"In spite of its huge infrared luminosity, the host galaxy is classified from the optical morphology as an ordinary Sa-type galaxy ([R’]SAB[s]a;"
] | [
"Compare/Contrast"
] | [
[
1250,
1276
]
] | [
[
1106,
1249
]
] |
2017ApJ...849..149S__Lee_2004_Instance_1 | There is a similarity between the ISM and the young stellar structures identified here. First, similar to the young stellar structures, the ISM also displays irregular morphologies and contains large amounts of substructures (clouds, clumps, cores, filaments, etc.) that are hierarchically organized (Rosolowsky et al. 2... | [
"Lee 2004"
] | [
"Typical values are close to D2 = 1.4–1.5",
"which are consistent with the fractal dimension as derived for the young stellar structures."
] | [
"Similarities",
"Similarities"
] | [
[
794,
802
]
] | [
[
675,
715
],
[
922,
1014
]
] |
2017MNRAS.470..612F__Feng_etal._2016_Instance_1 | The millimetre bump in M87 as recently observed by the Atacama Large Millimeter/submillimeter Array can be naturally modelled by the synchrotron emission of the thermal electrons in the ADAF, which is different from the prediction of the jet model. Therefore, it provides an opportunity to explore the accretion process ... | [
"Feng etal. (2016)"
] | [
"In particular,",
"and Li etal. (2016) both found that the rotation measure predicted from the ADAF is roughly consistent with the observational values."
] | [
"Similarities",
"Similarities"
] | [
[
356,
373
]
] | [
[
341,
355
],
[
374,
507
]
] |
Subsets and Splits
No community queries yet
The top public SQL queries from the community will appear here once available.