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 |
|---|---|---|---|---|---|---|
2021MNRAS.501.4035R__Vigren_&_Galand_2013_Instance_1 | The study of cometary plasma composition has been subjected to a great interest after the ion mass spectrometer onboard Giotto spacecraft detected many peaks in the mass range 12 and 120 amu (Balsiger et al. 1986; Krankowsky et al. 1986; Mitchell et al. 1987; Altwegg et al. 1993). By developing photochemical models, nu... | [
"Vigren & Galand 2013"
] | [
"Several modelling works on this comet have shown that ion composition in the coma varies based on the sublimation rate of the nucleus"
] | [
"Background"
] | [
[
1242,
1262
]
] | [
[
1107,
1240
]
] |
2022MNRAS.512.2222V__Granato_et_al._2004_Instance_1 | As for the ETGs, which are spheroid-dominated, most of these that are more massive than ∼2 × 1010 M⊙ are old, implying that the SF has strongly declined long time ago and no recent bursts of SF have occurred. Early formation and rapid quenching mechanisms are expected for those galaxies, where the quenching mechanisms ... | [
"Granato et al. 2004"
] | [
"as well as strong AGN/QSO and Supernova feedback that will heat and expel the gas (e.g."
] | [
"Background"
] | [
[
675,
694
]
] | [
[
587,
674
]
] |
2016AandA...595A..72M__Vergani_et_al._2015_Instance_1 | On the other hand, the Australia Telescope Compact Array (ATCA) 21 cm line survey of GRB host galaxies revealed high levels of atomic hydrogen (H i), suggesting that the connection between atomic gas and star formation is stronger than previously thought (Michałowski et al. 2015). Star formation may be directly fuelled... | [
"Vergani et al. 2015"
] | [
"Indeed, large atomic gas reservoirs, together with low molecular gas masses",
"and stellar masses",
"indicate that GRB hosts are preferentially galaxies that have very recently started a star formation episode."
] | [
"Compare/Contrast",
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1052,
1071
]
] | [
[
884,
959
],
[
1006,
1024
],
[
1074,
1183
]
] |
2015AandA...582A..22L__Todorov_et_al._2014_Instance_2 | Dust distribution:We employed the standard flared disk model with well-mixed gas and dust, which has been successfully used to explain the observed SEDs of a large sample of young stellar objects and BDs (e.g., Wolf et al. 2003; Sauter et al. 2009; Harvey et al. 2012a; Joergens et al. 2013; Liu et al. 2015). The struct... | [
"Todorov et al. 2014"
] | [
"J04414489+2301513 (a~15 AU,"
] | [
"Uses"
] | [
[
1210,
1229
]
] | [
[
1182,
1209
]
] |
2019ApJ...882..144K__Berk_et_al._2001_Instance_2 | The FOCAS and NIRSPEC spectra of PSO J006+39 were obtained at two different epochs separated by 1 yr and 9 months (by slightly less than 3 months in the quasar rest frame). Previously, we found that the PS1 y-band light curve of PSO J006+39 shows brightness variations with a peak-to-peak amplitude of ∼0.7 mag over ∼4 y... | [
"Vanden Berk et al. 2001"
] | [
"The spectral windows adopted for the analysis of the FOCAS and NIRSPEC spectra were taken to be similar to the rest-frame wavelength intervals commonly used to fit the continua of quasars"
] | [
"Uses"
] | [
[
1465,
1488
]
] | [
[
1276,
1463
]
] |
2017ApJ...835..246Y__Yoon_&_Seough_2014_Instance_1 | The present analysis builds upon the macroscopic-kinetic model of the solar wind, originally formulated by Yoon & Seough (2014) for the proton temperatures. The same model was recently generalized to include collisional dissipation (Yoon 2016a, 2016b). The basic methodology is similar to that of Marsch & Tu (2001) and ... | [
"Yoon & Seough (2014)",
"Yoon & Seough 2014"
] | [
"and Yoon (2016a, 2016b) discuss the wave generation in a self-consistent manner by solving the adiabatic dispersion relation and wave kinetic equation for each spatial location.",
"We now extend the original formalism",
"in another direction."
] | [
"Motivation",
"Extends",
"Extends"
] | [
[
514,
534
],
[
751,
769
]
] | [
[
535,
712
],
[
713,
749
],
[
771,
792
]
] |
2021MNRAS.503.1319G__Chae_&_Mao_2003_Instance_2 | In the first scenario, we assume that neither the characteristic velocity dispersion (σ*) nor the number density (n*) of galaxies evolves with redshifts (νn = νv = 0). Given the redshift coverage of the lensing galaxies in the lens sample (0.06 zl 1.0), if we constrain a non-evolving VDF using the lens data, then, as... | [
"Chae & Mao 2003"
] | [
"Consequently, the image separation distribution is consistent with the SDSS measured stellar VDF",
"and the Second Southern Sky Redshift Survey (SSRS2) inferred stellar VDF",
"although the two stellar VDFs are significantly different from each other concerning their corresponding parameter values."
] | [
"Similarities",
"Similarities",
"Compare/Contrast"
] | [
[
1564,
1579
]
] | [
[
1373,
1469
],
[
1490,
1562
],
[
1582,
1704
]
] |
2020AandA...639A.107S__Helling_et_al._2019a_Instance_1 | Micro-porosity is the porosity arising from the organisation of the condensate monomers (e.g. Mg2 SiO4 in Mg2 SiO4[s]) within a cloud particle during growth. This is different from the porosity that can be used to characterise aggregates that originate from particle-particle collision processes (coagulation, e.g. Domin... | [
"Helling et al. 2019a"
] | [
"Earth-like exoplanets, mini-Neptunes, and T-type brown dwarfs may form water clouds, composed of liquid or solid particles, but warmer planets and brown dwarfs of L-type and later have been shown to form cloud particles made of a mix of materials that is dominated by Mg, Si, Fe, and O and to a lesser extent by Ti,... | [
"Background"
] | [
[
1134,
1154
]
] | [
[
751,
1091
]
] |
2018ApJ...852...45W__Ghisellini_et_al._2013_Instance_1 | Similarly to former works (e.g., Zhang et al. 2010, 2012; Kang et al. 2014, 2016; Yan et al. 2016), we neglect the low-frequency radio data and consider the data with
(or
) in our SED fitting with the one-zone model due to the fact that radio emission should come from the large-scale jet and cannot be acco... | [
"Ghisellini et al. 2013"
] | [
"In four LSP blazars (0333 + 321, 0430 + 052, 2145 + 067, 2230 + 114), the putative UV excesses are not included in our SED fitting, as they should come from the cold accretion disk"
] | [
"Uses"
] | [
[
829,
851
]
] | [
[
623,
803
]
] |
2015AandA...575A.111D__Drimmel_&_Spergel_2001_Instance_1 | Using our stellar parameters, we derived an estimate of the spectroscopic distances of XO-2N and XO-2S by means of the following procedure. We generated Monte Carlo (MC) normal distributions for each spectroscopic parameter Teff, [Fe/H], and log g, composed of 10 000 random values and centred on the best estimates (Ta... | [
"Drimmel & Spergel 2001"
] | [
"We derived AV(s) by adopting a simplified model of the local distribution of the interstellar dust density",
"expressed by the relation ρ = ρ0·sech2(z/hs), where z is the height of the star above the Galactic plane and hs is the scale-height of the dust, for which we adopted the value of 190 pc."
] | [
"Uses",
"Uses"
] | [
[
1262,
1284
]
] | [
[
1154,
1260
],
[
1287,
1473
]
] |
2019ApJ...875...90L__Pontieu_et_al._2011_Instance_1 | When energy flows from the interior of the Sun outward into the solar atmosphere, why is the Sun’s outer atmosphere, the corona, much hotter than the inner atmosphere, the underlying chromosphere and photosphere? This is the long-standing problem of the coronal heating, which is one of the eight key mysteries in modern... | [
"De Pontieu et al. 2011"
] | [
"Especially during recent decades, high-resolution observations of solar super-fine structures indicate that small spicules, minor hot jets along small-scale magnetic channels from the low atmosphere upwards to the corona, petty tornados and cyclones, and small explosive phenomena such as mini-filament eruptions an... | [
"Background"
] | [
[
1248,
1270
]
] | [
[
824,
1246
]
] |
2016ApJ...825..150C__Bermúdez_et_al._2013_Instance_1 | The rotational spectrum of NaCl has been obtained using two different FTMW spectrometers constructed at the University of Valladolid. A solid rod was prepared by pressing the NaCl fine powder mixed with a small amount of commercial binder and was placed in the ablation nozzle (Alonso et al. 2009; Mata et al. 2012). A p... | [
"Bermúdez et al. 2013"
] | [
"NaCl was first investigated using a chirped-pulse Fourier transform microwave (CP-FTMW) spectrometer with a laser ablation source",
"operating between 6.0 and 12.0 GHz to sample swiftly the rotational spectra of the different species present in the supersonic expansion."
] | [
"Background",
"Background"
] | [
[
719,
739
]
] | [
[
570,
699
],
[
741,
878
]
] |
2019MNRAS.489..855C__Husemann_et_al._2013_Instance_1 | The size of ENLRs have been defined in different ways in the literature. Bennert et al. (2002) and Schmitt et al. (2003b) used the Hubble Space Telescope (HST) to obtain narrow band images of $\rm [O\, III]$, and adopted the maximum 3σ detected radius as the radius of the ENLR. This method is subject to the instrumenta... | [
"Husemann et al. 2013"
] | [
"The long-slit based observations also have drawbacks: the morphology of ENLR is sometimes irregular so that the derived size depends on the orientation of slits"
] | [
"Motivation"
] | [
[
830,
850
]
] | [
[
648,
808
]
] |
2021AandA...656A.122D__Triana_et_al._2015_Instance_1 | Understanding how angular momentum and chemicals are transported in the interiors of stars (and planets) along their evolution is one of the key challenges of modern stellar (and planetary) astrophysics. Indeed, rotation modifies their structure, their chemical stratification, their internal flows and magnetism, and th... | [
"Triana et al. 2015"
] | [
"Then, observations of oscillation modes in",
"and in B-type stars",
"provided us new Rosetta stones to constrain the transport of angular momentum in the whole Hertzsprung-Russell diagram."
] | [
"Background",
"Background",
"Background"
] | [
[
1586,
1604
]
] | [
[
1196,
1238
],
[
1539,
1558
],
[
1760,
1879
]
] |
2018AandA...613A..15S__Becker_et_al._2016_Instance_1 | In this study, we have outlined and successfully tested a refined technique to measure in contemporary lensing surveys the scale-dependent galaxy bias down to non-linear scales of k ~ 10 h−1 Mpc for lens galaxies at z ≲ 0.6. To test our reconstruction technique, we employ a fiducial survey with a sky coverage of ~ 1000... | [
"Becker et al. 2016"
] | [
"Despite some variations in survey depth and area, these survey parameters are similar to the ongoing Kilo-Degree Survey (KiDS), Dark Energy Survey (DES), or the survey with the Hyper Suprime-Cam"
] | [
"Similarities"
] | [
[
755,
773
]
] | [
[
538,
732
]
] |
2016ApJ...817..156W__Yan_et_al._2014a_Instance_1 | Recently, one of the hot topics in solar physics is the understanding of solar filaments in the corona, including their distribution, formation, eruption, and stability (Yang et al. 2008; Kong et al. 2015; Su et al. 2015; Yan et al. 2015). Martin (1998) and Gaizauskas (2002) have shown that convergence and cancellation... | [
"Yan et al. 2014a"
] | [
"Many reports on the eruption of filaments are concerned with torus instability or/and kink instability"
] | [
"Background"
] | [
[
807,
823
]
] | [
[
644,
746
]
] |
2021MNRAS.507..175S___2008_Instance_1 | Momentum and kinetic energy can be directly transferred to the gas, suppressing inflows. The fast-moving jets can also shock heat the surrounding gas. Many models have invoked kinetic jets to suppress cooling flows and SFRs in massive haloes (e.g. Dubois et al. 2010; Gaspari et al. 2012a; Li & Bryan 2014a; Prasad et al... | [
"Hopkins et al.",
"2008"
] | [
"Many models in the literature also invoke the idea that AGN can effectively drive strong pressure-driven outflows and offset cooling if a large fraction of the accretion energy is thermalized"
] | [
"Background"
] | [
[
636,
650
],
[
667,
671
]
] | [
[
352,
543
]
] |
2022AandA...663A..70F___2017_Instance_1 | Out of these sites (a) might provide the conditions for a very weak r-process and νp-process, whether only up to Sr, Y, Zr or up to (but not beyond) the A = 130 peak is still debated (Wanajo et al. 2018; Curtis et al. 2019; Fischer et al. 2020a; Ghosh et al. 2022). (b) is a class of supernovae whose existence is put in... | [
"Nishimura et al.",
"2017"
] | [
"Dependent on the initial fields, varying weak (probably dominating) to strong r-process conditions can be obtained, the latter, however, only for precollapse fields beyond 1012 G"
] | [
"Uses"
] | [
[
1022,
1038
],
[
1045,
1049
]
] | [
[
768,
946
]
] |
2021ApJ...921...18K__Kushwaha_et_al._2018a_Instance_1 | The most unique and characteristic observational feature of blazars’ highly variable broadband emission is the broad bimodal SED extending from the lowest accessible EM band, i.e., the radio, to the highest accessible, i.e., GeV-TeV γ-rays. The broadband SED of all blazars can be categorized into three different spectr... | [
"Kushwaha et al. 2018a"
] | [
"Only in a few rare instances has an appreciable shift in the location of the peaks been observed, e.g., the 1997 outburst of Mrk 501",
"and the activity of OJ 287 from the end of 2015 to the middle of 2017"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
919,
940
]
] | [
[
677,
809
],
[
848,
917
]
] |
2017MNRAS.472..772M__Cassata_et_al._2015_Instance_1 | Fig. 7 also shows that there is little evidence for a relation between the Ly α luminosity and M1500 for Ly α-selected sources at z = 5.7 in our UV and Ly α luminosity range. As both M1500 and LLy α are, to first order, related to the SFR, we would have expected a correlation. To illustrate this, we show lines at const... | [
"Cassata et al. 2015"
] | [
"More recently, other surveys also revealed that the fraction of high-EW Ly α emitters increases towards fainter UV magnitudes"
] | [
"Background"
] | [
[
831,
850
]
] | [
[
638,
763
]
] |
2022ApJ...934..126K__Lotekar_et_al._2016_Instance_1 | We considered a homogeneous, collisionless two species plasma consisting of electrons and ions (H+ ions) in the simulation model. The ambient plasma parameters for ions and electrons are given in Table 2. The ions and electrons are considered to be fluid and their dynamic is incorporated into the simulation model using... | [
"Lotekar et al. 2016"
] | [
"We used a compensated filter to eliminate the small wavelength modes linked with such numerical noise"
] | [
"Uses"
] | [
[
1560,
1579
]
] | [
[
1457,
1558
]
] |
2017AandA...607A..71G__Hansen_&_Oh_(2006)_Instance_2 | 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{$Z/Z_\odot = 0.63\left(\tau_{\rm d}/10^{-4}\right)\left(10^... | [
"Hansen & Oh (2006)"
] | [
"The behavior for the low- and high-dust contents is quite different.",
"On the one hand, the escape fractions versus NHI,cl scales for τd,cl = 1 (filled symbols in Fig. 12) as predicted by",
"in their “surface scatter” approximation",
"On the other hand, however, this is not the case for the low-dust scenari... | [
"Differences",
"Similarities",
"Similarities",
"Differences"
] | [
[
1384,
1402
]
] | [
[
1198,
1266
],
[
1267,
1383
],
[
1403,
1443
],
[
1594,
1766
]
] |
2016MNRAS.457.2433P__Nolan_et_al._2012_Instance_1 | From the result of the χ2 minimization, we found that the minimized χ2 values agree with the expected values, i.e. the computed χ2 are typically in the range of ($\mathrm{d.o.f.}-\sqrt{2 \mathrm{d.o.f.}}$, $\mathrm{d.o.f.}+\sqrt{2 \mathrm{d.o.f.}}$), where d.o.f. is the number of degrees of freedom. This means that the... | [
"Nolan et al. (2012)"
] | [
"Mrk 421 is a very hard spectrum γ-ray source with a photon index of ≈1.77 and its semiminor and semimajor axes at 68 per cent confidence are of 0$_{.}^{\\circ}$0067 as derived in"
] | [
"Uses"
] | [
[
809,
828
]
] | [
[
631,
808
]
] |
2016AandA...586A..89C__Lo_2005_Instance_1 | The knowledge of physical properties, the structure, and the kinematics of the matter in the vicinity of supermassive black holes (SMBH) is essential to build detailed models of the clumpy outflow and to test the disc-wind scenario. While X-ray variability studies can provide accurate information on the atomic and ioni... | [
"Lo 2005"
] | [
"While X-ray variability studies can provide accurate information on the atomic and ionized matter on scales of the BLR, the radio emission from luminous H2O masers (the so-called “megamasers”) constitutes a fundamental instrument to study the geometry and kinematics of the molecular gas at sub-parsec distance from... | [
"Motivation"
] | [
[
746,
753
]
] | [
[
233,
725
]
] |
2021MNRAS.501.2522J__Mukherjee_&_Paul_2004_Instance_1 | GX 301-2 is an HMXB consisting of a highly magnetized (B ∼ 4 × 1012 G, or even larger Doroshenko et al. 2010) pulsar and a B-type hyper-giant star Wray 977 (Vidal 1973; Kaper et al. 1995; Staubert et al. 2019). According to modelling of high-resolution optical spectra, Wray 977 has a mass of 43 ± 10 $\, \mathrm{M}_{\od... | [
"Mukherjee & Paul 2004"
] | [
"The broad-band X-ray spectrum is orbital phase-dependent and can be approximately described as a power law with a high-energy cutoff and a cyclotron resonant scattering feature around 40 keV"
] | [
"Background"
] | [
[
1142,
1163
]
] | [
[
925,
1115
]
] |
2019MNRAS.486.3741H__Susa_et_al._2015_Instance_1 | As the initial state of star-forming clouds, a critical Bonnor–Ebert (B.E.) density profile (Ebert 1955; Bonnor 1956) is adopted for each model. Note that the B.E. density profile or B.E. sphere is usually used as the initial condition of star-forming clouds (e.g. Matsumoto & Tomisaka 2004; Banerjee & Pudritz 2006; Mac... | [
"Susa et al. 2015"
] | [
"The temperature Tcl of each cloud is determined as the result of a one-zone calculation (for details, see"
] | [
"Uses"
] | [
[
672,
688
]
] | [
[
566,
671
]
] |
2019AandA...629A..54U__Marinucci_et_al._2015_Instance_4 | NGC 2110. NGC 2110 is another nearby (z = 0.00779, Gallimore et al. 1999), X-ray bright Seyfert galaxy. Diniz et al. (2015) report a black hole mass of
2
.
7
−
2.1
+
3.5
×
10
8
M
⊙
$ 2.7^{+ 3.5}_{- 2.1} \times 10^{8}\,{{M}_{\odot}} $
, from the relation with the stellar velocity dispersion. From Bepp... | [
"Marinucci et al. 2015"
] | [
"Indeed, only lower limits to the high-energy cut-off have been found with NuSTAR (210 keV"
] | [
"Compare/Contrast"
] | [
[
1910,
1931
]
] | [
[
1819,
1908
]
] |
2018ApJ...864..158L__Pino_&_Lazarian_2005_Instance_1 | Inspection of Equation (25) reveals that for pitch angles satisfying
,
so that curvature drift energization is more efficient than generalized betatron energy loss during incompressible contraction/merging of small-scale flux ropes. When μ2 1/3, betatron energy loss dominates curvature drift energization.... | [
"de Gouveia dal Pino & Lazarian 2005"
] | [
"Consider the following three possibilities: (1) If energetic particles maintain a highly beamed pitch-angle distribution (which requires negligible pitch-angle scattering), curvature drift energy gain strongly dominates generalized betatron energy loss, and for all practical purposes we have a first-order Fermi ac... | [
"Uses"
] | [
[
966,
1001
]
] | [
[
535,
964
]
] |
2021MNRAS.506..813D__Fabricius_et_al._2014_Instance_1 | Traditionally, GCs have been considered as relatively simple spherical, non-rotating, and almost completely relaxed systems. However, observational results obtained in the past few years are demonstrating that they are much more complex than previously thought. In particular, the classical simplified approach of neglec... | [
"Fabricius et al. 2014"
] | [
"In particular, the classical simplified approach of neglecting rotation in GCs has become untenable from the observational point of view. In fact, there is an increasing wealth of observational results suggesting that, when properly surveyed, the majority of GCs rotate at some level. As of today, more than $50{{\\... | [
"Background"
] | [
[
708,
729
]
] | [
[
262,
661
]
] |
2017MNRAS.469..521K__Redfield_2007_Instance_1 | Molecular CO gas is observed in the sub-mm with both single-dish telescopes (JCMT, APEX) and interferometers such as ALMA, the SMA or NOEMA. For the brightest targets, ALMA's high-resolution and unprecedented sensitivity allow us to obtain CO maps for different lines and isotopes showing the location of CO belts and gi... | [
"Redfield 2007"
] | [
"Also, metals have been detected, using UV/optical absorption lines, around",
"and HD 32297 (Na i,"
] | [
"Background",
"Background"
] | [
[
915,
928
]
] | [
[
718,
792
],
[
895,
914
]
] |
2018MNRAS.475.1104B__Leonard_et_al._2001_Instance_1 | Observational evidence suggests that SNe IIn are aspherical and may have high polarization signals. An ∼ 20 per cent level of SN asphericity may result in a detectable 1 per cent linear polarization signal (Höflich 1991; Leonard & Filippenko 2005). While a number of efforts have been made to explain core-collapse SNe i... | [
"Leonard et al. 2001"
] | [
"The initially low polarization levels often rise during the plateau phase",
"with a polarization angle that typically remains nearly fixed throughout (e.g."
] | [
"Background",
"Background"
] | [
[
1036,
1055
]
] | [
[
855,
928
],
[
957,
1035
]
] |
2020MNRAS.499.5230F__Tripp,_Savage_&_Jenkins_2000_Instance_1 | Different methods have been proposed to detect the hot, highly ionized WHIM gas: detection in galaxy groups with Sunyaev–Zeldovich effect (Hill et al. 2016; de Graaff et al. 2019; Lim et al. 2020; Tanimura et al. 2020) using autocorrelation function measurements (Galeazzi et al. 2010), with absorption lines in quasar s... | [
"Tripp, Savage & Jenkins 2000"
] | [
"Nevertheless, the UV lines have so far mostly been used to detect absorbing gas with temperature range $10^5\\, \\mathrm{K} \\lt T \\lt 10^6\\, \\mathrm{K}$ from either O vi"
] | [
"Background"
] | [
[
848,
876
]
] | [
[
679,
846
]
] |
2017AandA...602A..29B__Shepherd_1997_Instance_1 | The MOJAVE survey provides access to excellent Very Long Baseline Array (VLBA) data taken at 15 GHz. This is of great value for investigating AGN properties on a statistical basis (e.g., Lister et al. 2016; Homan et al. 2015). Whereas the MOJAVE team is providing a statistical analysis of the complete sample, our appro... | [
"Shepherd 1997"
] | [
"We re-modeled fifty VLBA observations of 1308+326 obtained at 15 GHz (taken from the online MOJAVE archive webpage) between 1995.05 and 2014.07 with Gaussian components within the difmap-modelfit program",
"The modelfit program fits image-plane model components to the visibilities in the uv plane.",
"We did no... | [
"Uses",
"Background",
"Compare/Contrast"
] | [
[
894,
907
]
] | [
[
689,
892
],
[
910,
1001
],
[
1002,
1726
]
] |
2016AandA...586A.156K__Osorio_et_al._(2011)_Instance_1 | In this study, we use a model atom of Li i which was originally developed and tested by Cayrel et al. (2007) and Sbordone et al. (2010). For the purposes of the current work, the model atom was updated and now consists of 26 levels and 123 (96 of which are radiative) bound-bound transitions of Li i and the ground level... | [
"Osorio et al. (2011)"
] | [
"We used electron collisional excitation and ionization rates from the quantum mechanical computations of",
"for the energy levels of up to 5s (2S)."
] | [
"Uses",
"Uses"
] | [
[
1073,
1093
]
] | [
[
968,
1072
],
[
1094,
1133
]
] |
2016MNRAS.462.2275K__Porubcan,_Kornos_&_Williams_2004_Instance_1 | Currently, the concept of the existence of genetic relations between comets and meteoroid streams as well as near-Earth asteroids (NEAs) is generally accepted. As a consequence, a new definition, the ‘comet–asteroid–meteoroid complex’, was introduced for the indication of the families of objects with a common origin. T... | [
"Porubcan, Kornos & Williams 2004"
] | [
"A cometary nature of these NEAs was suggested and a conclusion was made that they are either extinct fragments of comet Encke or represent (together with comet Encke) the remnants of a larger comet-progenitor of the stream"
] | [
"Background"
] | [
[
1049,
1081
]
] | [
[
779,
1001
]
] |
2016ApJ...822...22O__Orlando_et_al._2015_Instance_1 | We used the FLASH code (Fryxell et al. 2000) to perform the calculations. In particular we solved the equations for compressible gas dynamics with the FLASH implementation of the piecewise-parabolic method (Colella & Woodward 1984). The radiative losses Λ in Equation (2) are calculated through a table lookup/interpolat... | [
"Orlando et al. 2015"
] | [
"For the former, we calculated the ion and electron temperatures in each cell of the post-shock medium, taking into account the effects of Coulomb collisions (see",
"for the details of the implementation)."
] | [
"Uses",
"Uses"
] | [
[
708,
727
]
] | [
[
546,
707
],
[
728,
767
]
] |
2022AandA...660A.135V__Spina_et_al._2016_Instance_1 | The first study, to our knowledge, to notice the net increase in the abundance of slow (s) neutron capture elements in young stellar populations is D’Orazi et al. (2009), in which the abundance of barium in young star clusters was seen to be higher than in the older ones. Maiorca et al. (2011, 2012) added a few more el... | [
"Spina et al. 2016"
] | [
"Once the existence of a relationship between age and chemical clocks was established (see, e.g.,"
] | [
"Background"
] | [
[
1222,
1239
]
] | [
[
1125,
1221
]
] |
2021MNRAS.505.5833F__Lesgourgues_2011_Instance_1 | Besides the Patchy and the LN mocks, we also model the multipoles of the BOSS CMASS two-point correlation function using an analytic approach, which is required to run the Monte Carlo analysis (see Section 5). The 2PCF can be obtained from the Fourier transform of the matter power spectrum, P(k), for which we assume th... | [
"Lesgourgues 2011"
] | [
"In the equation above, Plin(k) is the linear matter power spectrum computed using the Boltzmann code CLASS",
"assuming the Planck 2015 (Ade et al. 2016) fiducial cosmology."
] | [
"Uses",
"Uses"
] | [
[
614,
630
]
] | [
[
506,
612
],
[
633,
695
]
] |
2019ApJ...875...63M__Stern_et_al._2019_Instance_1 | The technique of weak lensing offers direct measurement of the total matter distribution of a galaxy cluster (baryonic and dark matter), and can thus provide an unbiased mass calibration. Weak lensing manifests itself as small but coherent distortions of distant galaxies that result from the gravitational deflection of... | [
"Stern et al. 2019"
] | [
"Numerous attempts to calibrate SZ masses have been made in the literature using",
"SPT clusters"
] | [
"Background",
"Background"
] | [
[
708,
725
]
] | [
[
474,
553
],
[
631,
643
]
] |
2019AandA...625A.148D__Li_et_al._2011_Instance_1 | With a stellar mass of 5 × 1010 M⊙ (Viaene et al. 2014), Andromeda belongs to the transition regime between the active blue-sequence galaxies and passive red-sequence galaxies (e.g. Bower et al. 2017; Baldry et al. 2006), which happens around the stellar mass of 3 × 1010 M⊙ (e.g. Kauffmann et al. 2003). This galaxy is ... | [
"Li et al. 2011"
] | [
"Andromeda hosts both very little gas and very little star formation, while the black hole is basically quiet and has some murmurs"
] | [
"Background"
] | [
[
555,
569
]
] | [
[
424,
553
]
] |
2021MNRAS.502..915C__Cisneros-Parra_1970_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 ... | [
"Cisneros-Parra 1970"
] | [
"while if we assume that redback companions are akin to the companions in CV systems whose outer envelopes have also been stripped through accretion, then we may expect a smaller value k2 ∼ 10−3"
] | [
"Uses"
] | [
[
1077,
1096
]
] | [
[
882,
1075
]
] |
2018MNRAS.478...69A__Borucki_2016_Instance_1 | The complexity of non-adiabatic pulsations and their coupling to the convection has posed many problems since the field’s inception and still does. The main problem lies in our, so far, limited understanding of the interaction between convection and pulsations. However, several important steps forward have already been... | [
"Borucki 2016"
] | [
"The case of solar pulsational stability has been studied in detail",
"while the space missions",
"and Kepler",
"have provided high-quality seismic data for stars of different flavours against which we can test models and further our understanding of stellar pulsations."
] | [
"Background",
"Background",
"Background",
"Background"
] | [
[
700,
712
]
] | [
[
445,
511
],
[
615,
639
],
[
667,
677
],
[
714,
871
]
] |
2020AandA...635A.121M__Stolker_et_al._2016_Instance_1 | As scattered light imaging is sensitive to the stellar irradiation, it allows one to search for misalignments between various disk regions. While studying the morphology of the innermost disk region is challenging due to its very small radial extent, often marginally resolvable by optical interferometry (Lazareff et al... | [
"Stolker et al. 2016"
] | [
"In this scenario, depending on the misalignment angle, the outer disk image will show narrow shadow lanes (e.g.,"
] | [
"Background"
] | [
[
568,
587
]
] | [
[
434,
546
]
] |
2020ApJ...897...73M__Dugair_et_al._2013_Instance_1 | Many Be-binary systems were observed during their outbursts, which offered interesting results (Bildsten et al. 1997; Reig 2011). Bright X-ray outbursts are observed in Be binaries, most likely during the periastron passage of its neutron star through the circumstellar disk of its companion. Depending on the amount of ... | [
"Dugair et al. 2013"
] | [
"Quasi-periodic oscillations (QPOs) have been detected from many Be binaries, such as",
"4U 0115+63"
] | [
"Background",
"Background"
] | [
[
1507,
1525
]
] | [
[
1288,
1372
],
[
1455,
1465
]
] |
2021ApJ...921...25C__Way_et_al._2017_Instance_1 | Only a few GCM studies have previously considered isolated examples of higher-order spin–orbit resonance effects on climate (Wordsworth et al. 2010; Yang et al. 2013, 2020; Turbet et al. 2016; Boutle et al. 2017; Del Genio et al. 2019b). To our knowledge, no previous work has incorporated geothermal heating into a 3D G... | [
"Way et al. 2017"
] | [
"Yang et al. (2013) showed that at 2:1 and 6:1 resonances with a static/slab ocean (see Section 2.2.2 of",
"), Bond albedo is lower than it is for synchronous rotation and decreases rather than increases with incident stellar flux, thus destabilizing the climate as the planet approaches the IHZ."
] | [
"Background",
"Background"
] | [
[
752,
767
]
] | [
[
648,
751
],
[
767,
955
]
] |
2021MNRAS.503..354G__Cantat-Gaudin_et_al._2020_Instance_1 | The spatial distribution of OB stars and associations, young long-period Cepheids and open clusters, star-forming regions, H ii regions, interstellar dust, and giant molecular and neutral gas clouds in the solar vicinity that have been in existence generally τ ≲ 108 yr is known to correlate with the location of the inn... | [
"Cantat-Gaudin et al. 2020"
] | [
"The Sun is situated at the inner edge of the Orion arm"
] | [
"Background"
] | [
[
738,
763
]
] | [
[
538,
592
]
] |
2018MNRAS.476.4510P__Hobbs,_Edwards_&_Manchester_2006_Instance_1 | The modulation of an extra-solar signal can, if working in terms of signal phase, be expressed as a time modulation, e.g. for a phase evolution given by
(1)
\begin{eqnarray}
\phi (t) = \phi _0 + 2\pi f_0\left( t - t_0 + \Delta \tau (t) \right),
\end{eqnarray}
where t is the time of arrival of the signal at the obse... | [
"Hobbs, Edwards & Manchester 2006"
] | [
"Here, for each of the terms we use the sign conventions given in the source code for the pulsar timing software tempo21"
] | [
"Uses"
] | [
[
1355,
1387
]
] | [
[
1234,
1353
]
] |
2022ApJ...937...76W__Verdini_et_al._2015_Instance_1 | Direct measures of cascade rates in turbulent systems often employ theoretical formulations related to Kolmogorov’s “4/5” law (Kolmogorov 1941b; Frisch 1995) and its variants, in which the inertial range cascade rate is related to a signed third-order structure function. This so-called exact law is derived from the flu... | [
"Verdini et al. 2015"
] | [
"Frequently a major issue in these applications is the use of formulations derived assuming isotropy in turbulence that is actually anisotropic",
", this being the typical case for solar wind and magnetosheath turbulence."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1276,
1295
]
] | [
[
1132,
1274
],
[
1296,
1370
]
] |
2017MNRAS.470.3882T__Breen_et_al._2015_Instance_1 | A sample of 17 starless clump candidates has been selected from the Traficante et al. (2015a) as objects with Σ ≥ 0.05 g cm−2, mass ${{{M}}}\ge 300$ M⊙, bolometric luminosity over envelope mass ratio L/M ≤ 0.3 and very low dust temperature (T 15 K), indicative of very young stage of evolution (see Section 4), no (or f... | [
"Breen et al. 2015"
] | [
"and found no Class II CH3OH masers in the sources of our sample"
] | [
"Uses"
] | [
[
776,
793
]
] | [
[
711,
774
]
] |
2022MNRAS.515.2633P__Blandford_&_Königl_1979_Instance_1 | Active galactic nuclei (AGN) have been discovered a century ago and still remain a hot topic of research. The theoretical predictions and the observational results suggest that the AGN have three main components namely, a central supermassive black hole (SMBH), an accretion disc around the SMBH, bipolar high relativist... | [
"Blandford & Königl 1979"
] | [
"Simulations and theory together suggest that the magnetic field plays an important role in collimating the particles and giving them a jet like shape"
] | [
"Background"
] | [
[
860,
883
]
] | [
[
709,
858
]
] |
2022MNRAS.516.5874W__Haasteren_2017_Instance_1 | An outlier is defined to be an anomalous event or observation that arises from a process that differs from the majority of the data generation. Outlier detection has always been an indispensable part of data analysis; contaminated data sets without proper outlier treatment can increase modelling uncertainties and produ... | [
"Vallisneri & van Haasteren 2017"
] | [
"A common mitigation strategy is to model the data as a Gaussian mixture of inlier and outlier distributions with differing variance"
] | [
"Uses"
] | [
[
500,
531
]
] | [
[
343,
474
]
] |
2020AandA...639A..88C__Chatzistergos_et_al._2019b_Instance_2 | To overcome these limitations, in our previous paper (Chatzistergos et al. 2018b, Paper I, hereafter) we introduced a novel approach to process the historical and modern Ca II K observations, to perform their photometric calibration, to compensate for the intensity centre-to-limb variation (CLV, hereafter), and to acco... | [
"Paper II"
] | [
"In",
", we applied our method to 85 972 images from 9 Ca II K archives to derive plage areas and produce the first composite of plage areas over the entire 20th century. In particular, we analysed the Ca II K archives from the Arcetri, Kodaikanal (8-bit digitisation), McMath-Hulbert, Meudon, Mitaka, Mt Wilson, R... | [
"Background",
"Background"
] | [
[
960,
968
]
] | [
[
957,
959
],
[
968,
1476
]
] |
2018AandA...616A..96R__Haardt_&_Madau_(2012)_Instance_1 | As expected, the final luminosity (LV) of our model dwarfs strongly correlates with the shape of their formation histories. We divide our models into three categories dependent on their LV range. In the following, we will refer to them as sustained, extended and quenched. A few representative cases of each of these thr... | [
"Haardt & Madau (2012)"
] | [
"The strength of the UV-background heating is indicated by the dotted black curve. It represents the hydrogen photo-heating rate due to the UV-background photons following the model of"
] | [
"Uses"
] | [
[
539,
560
]
] | [
[
355,
538
]
] |
2020AandA...638A..16T__Barnes_(2017)_Instance_2 | Figure 12 shows the results of our tidal evolution calculations. The left panel of Fig. 12 shows the planetary rotational evolution of GJ 1148 b due to star–planet tides. After ~850 Myr, GJ 1148 b reaches a rotation period that is 2∕3 of the orbital period, and remains there with Prot = 27.5 d. During the integration t... | [
"Barnes (2017)"
] | [
"The latter is longer by roughly the mass ratio of Mars to Titan, which can be understood from Eq. (2) of"
] | [
"Uses"
] | [
[
1697,
1710
]
] | [
[
1592,
1696
]
] |
2015MNRAS.454.2691M__Leitherer_et_al._1999_Instance_1 | In order for simulations to play a role in improving our understanding of the formation and dynamics of the CGM, particularly given the complex, multiphase picture emerging from the latest observations (Tumlinson et al. 2011; Werk et al. 2014), the level of detail and sophistication in stellar feedback models must impr... | [
"Leitherer et al. 1999"
] | [
"Unlike the subgrid recipes which involve kinetically prescribed decoupled winds and cooling-suppressed blastwaves, the FIRE simulations solve the ‘overcooling’ problem by explicitly modelling the radiation pressure, stellar winds, and ionizing feedback from young stars as taken directly from the population synthes... | [
"Uses"
] | [
[
855,
876
]
] | [
[
519,
853
]
] |
2021AandA...653A..36M__Goulding_&_Alexander_(2009)_Instance_4 | The SFG sample was constructed using the Great Observatories All-Sky LIRG Survey (GOALS sample, Armus et al. 2009), from which we extracted 158 galaxies, with data from Inami et al. (2013), who report the fine-structure lines at high resolution in the 10 − 36 μm interval, and Stierwalt et al. (2014), who include the de... | [
"Goulding & Alexander (2009)"
] | [
"The galaxies presented by Bernard-Salas et al. (2009) have instead an average redshift of 0.0074, while the sample by",
"has an average redshift of 0.0044."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
2507,
2534
]
] | [
[
2389,
2506
],
[
2535,
2569
]
] |
2019MNRAS.486.1781R__Bonning_et_al._2012_Instance_1 | To check for any spectral variation in the optical/IR bands, we looked for variation in the V − J band colour against the V-band brightness. This colour variation was analysed for the epochs A, B, D, and E. During epochs A and B, the source showed a ‘redder when brighter’ (RWB) behaviour. During epoch E, a bluer when b... | [
"Bonning et al. 2012"
] | [
"From studies on the optical–IR colour–magnitude diagram, it is known that FSRQs in general show an RWB trend, which is attributed to them having a luminous accretion disc"
] | [
"Compare/Contrast"
] | [
[
922,
941
]
] | [
[
734,
904
]
] |
2020ApJ...898L..25K__Townsley_&_Bildsten_2003_Instance_1 | Once He core burning finishes the core contracts and hydrogen burning starts, the radius of the hot subdwarf expands beyond its Roche radius, and mass transfer starts at an orbital period close to the observed orbital period. Mass transfer will continue for ≈1 Myr at a rate exceeding 10−9 M⊙ yr−1 until hydrogen shell b... | [
"Townsley & Bildsten 2003"
] | [
"Mass transfer will continue for ≈1 Myr at a rate exceeding 10−9 M⊙ yr−1 until hydrogen shell burning is finished and the star contracts to become a carbon–oxygen WD with a thick helium layer and a small residual layer of hydrogen. The high accretion rate will heat the accreting WD significantly"
] | [
"Background"
] | [
[
523,
547
]
] | [
[
226,
521
]
] |
2018ApJ...866L...1S__Pecharromán_et_al._1999_Instance_1 | 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)"
] | [
"It was found that the complex dielectric function from",
"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."
] | [
"Uses",
"Uses"
] | [
[
55,
80
]
] | [
[
0,
54
],
[
81,
307
]
] |
2018MNRAS.479.3254V__Schneider_et_al._2018_Instance_1 | 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; ... | [
"Schneider et al. 2018"
] | [
"For example, studies of young clusters embedded in moderate-mass MCs (∼104M⊙)",
"have shown that their age histograms contain a large majority of young (1–2 Myr) objects, but also a tail of older (up to several Myr) ones suggesting an accelerating star formation activity, sometimes followed by a subsequent decli... | [
"Background",
"Background"
] | [
[
990,
1011
]
] | [
[
593,
670
],
[
725,
969
]
] |
2019MNRAS.483..971V__al_2002_Instance_1 | We have also considered early radio emission from gamma-ray bursts (GRBs), which can have higher brightness temperatures at early times than blazars, owing to their ultrarelativistic velocities. They can therefore be brighter and easier to measure while still at small angular sizes, and are consequently observed to sho... | [
"Granot et al 2002"
] | [
"The Blandford–McKee blast wave of the ultrarelativistic shock moving into a medium of uniform external density ρ0 has radius R ≃ 2cT Γ2/(1 + $z$) and explosion energy per unit solid angle E/Ω ≃ ρ0R3Γ2c2, which gives Γ ≃ 9(Eiso, 53/n0)1/8(T/[(1 + $z$)day])−3/8, where $E=10^{53}\\, \\mbox{erg}(\\Omega /4\\pi)E_{iso,... | [
"Uses"
] | [
[
1115,
1132
]
] | [
[
759,
1113
]
] |
2016MNRAS.463L..26B__Ackermann_et_al._2014_Instance_1 | We calculate the corresponding γ-ray spectrum constructed from the photons arriving at the observer within the observation time of MAGIC and plot it in the bottom panel of Fig. 5. Although it is possible to explain the very fast variability of the emission even with a moderate Lorentz factor of the blob, strong constra... | [
"Ackermann et al. 2014"
] | [
"Note that such large values of the Lorentz factor of the emission region in the jet have been already postulated in terms of other models in order to explain extremely short flares observed in this source"
] | [
"Similarities"
] | [
[
861,
882
]
] | [
[
655,
859
]
] |
2015ApJ...799...55G__Klassen_et_al._2000_Instance_1 | While the angular extent of IP shocks can be directly investigated using multi-point in situ measurements, the size of coronal shocks can only be indirectly inferred via remote-sensing observations of the electromagnetic emissions associated with them. According to Nelson & Robinson (1975), the average angle subtended ... | [
"Klassen et al. 2000"
] | [
"Type II radio sources often show non-radial propagation trajectories (see Mann et al. 2003, and references therein). Wave-like large-scale disturbances propagating over the solar disk in extreme ultraviolet observations (usually referred to as âEIT wavesâ or âEUV wavesâ) are in close empirical correlation ... | [
"Background"
] | [
[
876,
895
]
] | [
[
534,
874
]
] |
2015AandA...582A.104R__Stix_2002_Instance_1 | Thermal motions of atoms produce a Doppler broadening of spectral lines with a Gaussian profile. Other unresolved velocities of a random nature are usually described as a turbulence broadening with a Gaussian or Lorentzian profile (see Rutten 2003, for a detailed description). The instrumental broadening encompasses th... | [
"Stix 2002"
] | [
"In other words, the velocity equivalent of the observed line width, Wobs = c × Δλ/λ, at 1/e of the peak intensity results from instrumental, Doppler, and turbulence (non-thermal) broadenings by (1)\\begin{equation} W_{\\rm{obs}}^2 = \\left(c\\times \\frac{\\Delta\\lambda}{\\lambda}\\right)^2 = W_{\\rm{instrumental... | [
"Uses"
] | [
[
1190,
1199
]
] | [
[
678,
1188
]
] |
2017AandA...605A..20C__Lattanzi_et_al._(2015)_Instance_1 | As mentioned above, molecular oxygen was used to calibrate the magnetic field applied. A total of 155 Zeeman components (for the three transitions considered) was measured, with the magnetic field varied from B = 2.3 G (Itot = 0.2 Amp) to B = 113.5 G (Itot = 10 Amp). Figure 5 shows the Zeeman spectrum for the N,J = 3, ... | [
"Lattanzi et al. (2015)"
] | [
"In the fitting procedure the spectroscopic parameters (i.e., the rotational, centrifugal distortion, and fine structure constants) were kept fixed at the values derived by"
] | [
"Uses"
] | [
[
1333,
1355
]
] | [
[
1161,
1332
]
] |
2021ApJ...915...93L__Magdziarz_&_Zdziarski_1995_Instance_1 | Table 3 shows the best-fit model parameters for the baseline fit for the three observations. We note that we did not find any statistically significant neutral or ionized absorption intrinsic to the source. On the addition of an ionized absorption model generated using the latest atomic data with the photoionization mo... | [
"Magdziarz & Zdziarski 1995"
] | [
"The pexrav model assumes an exponentially cutoff power-law spectrum reflected from neutral material"
] | [
"Uses"
] | [
[
1066,
1092
]
] | [
[
965,
1064
]
] |
2015MNRAS.448..629G__Cenko_et_al._2011_Instance_1 | The remaining six parameters are less constrained. They are ϵe, ϵB, n0, L (where L = ηL0), κ and Ek. We apply constraints to the range of allowed values for these parameters. ϵB has been found to be as low as 10−8 (Barniol Duran 2014; Santana, Barniol Duran & Kumar 2014) and as a fraction can be as high as 1. In practi... | [
"Cenko et al. 2011"
] | [
"n0 is limited between 10−5 and 100 cm−3, in line with what has been found in these sources"
] | [
"Uses"
] | [
[
674,
691
]
] | [
[
582,
672
]
] |
2016ApJ...827..151Y__Couvidat_et_al._2015_Instance_1 | The data produced by the HMI instrument are of high quality; however, there are known uncertainties, limitations and systematic errors present that affect the measurement of magnetic flux. These include a sinusoidal variation in the total magnetic flux with a periodicity of 12 and 24 hr, due to a Doppler shift present ... | [
"Couvidat et al. 2015"
] | [
"This affects weak and strong magnetic fields in the LoS magnetograms differently, with the daily variation remaining less than 30 G for field strengths below 1000 G and less than 75 G for field strengths below 2250 G. On average during a day this is roughly ±35 G",
"Nevertheless, the strength of these instrument... | [
"Uses",
"Compare/Contrast"
] | [
[
827,
847
]
] | [
[
562,
825
],
[
850,
1016
]
] |
2020AandA...644A..59K__Heays_et_al._2017_Instance_3 | Analyzing optical emission lines, emanating from within the northern lobe, Tylenda et al. (2019) found a reddening with EB − V ≈ 0.9 mag or AV ≈ 2.8 mag, which we assume is mainly circumstellar in origin. Hajduk et al. (2013) observed two stars shining through the southern lobe and found AV = 3.3 − 4.4 mag with unknown... | [
"Heays et al."
] | [
"The presence of ISM grains makes it possible for the observed molecules to survive for a very long time, longer than 350 yr. The lifetimes in the presence of the large grains considered by",
"are typically a few times shorter than the age of the remnant."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1164,
1176
]
] | [
[
975,
1163
],
[
1177,
1239
]
] |
2016MNRAS.457..212S__Ijjas,_Steinhardt_&_Loeb_2013_Instance_1 | One of the first and simplest proposed Friedmann–Robertson–Walker (FRW) cosmological model is the Λ cold dark matter (ΛCDM) universe, which involves Einstein's cosmological constant Λ. This standard model of cosmology, which is also referred to as the concordance model, assumes that the total energy density ρ of the un... | [
"Ijjas, Steinhardt & Loeb 2013"
] | [
"However, the latest observations by Planck",
"indicate that there may be some problems with such an inflationary scenario"
] | [
"Motivation",
"Motivation"
] | [
[
2332,
2361
]
] | [
[
2178,
2220
],
[
2255,
2330
]
] |
2022ApJ...936..102A__Williams_et_al._2006_Instance_3 | As regards the modeling of BGK modes, there are two main theoretical approaches: the integral solution or BGK methodology and the differential (or Schamel) technique. In the former method (BGK), one assumes that the initial particle distribution function and the electrostatic potential profiles are known, so these are ... | [
"Williams et al. (2006)"
] | [
"Their simulation results also reveal that the bipolar pulses reported in the Enceladus plume by",
"and Pickett et al. (2015) could most probably be ion holes."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
3115,
3137
]
] | [
[
3019,
3114
],
[
3138,
3197
]
] |
2022MNRAS.509.3488I__Terzić_&_Graham_2005_Instance_1 | The values rinf, ρinf, and σinf of equations (9) and (10) were computed assuming a bulge mass profile. Unlike other works that use isothermal sphere or Dehnen profiles (see e.g Volonteri, Haardt & Madau 2003; Sesana 2010; Sesana & Khan 2015; Bonetti et al. 2018b; Volonteri et al. 2020), here we decided to use a Sérsic ... | [
"Terzić & Graham 2005"
] | [
"The analytical expressions for the Sérsic model are taken from Prugniel & Simien (1997) (see also"
] | [
"Uses"
] | [
[
638,
658
]
] | [
[
540,
637
]
] |
2022MNRAS.515...71S___2017_Instance_1 |
Steady and smooth decline: Since falling from the peak of the 2012b event, SN 2009ip has only continued to fade and is now the faintest it has ever been in the optical. Immediately after the 2012 event (around day 200), it was declining somewhat slower than the rate of 56Co decay for a 56Ni mass of 0.04 $\, {\rm M}_{\... | [
"Smith et al.",
"2017"
] | [
"SNe IIn span a wide diversity of late-time decay rates, ranging from some SNe IIn that have essentially flat light curves for many years, like SN 2005ip",
"down to those that have only weak CSM interaction and faster decline rates that are difficult to distinguish from radioactive decay or light echoes."
] | [
"Background",
"Background"
] | [
[
1807,
1819
],
[
1826,
1830
]
] | [
[
1653,
1805
],
[
1875,
2023
]
] |
2019AandA...627A.130D__Broadhurst_et_al._2019_Instance_2 | Gravitational-wave astronomy has recently become a reality with the first detection of gravitational waves (GW hereafter) by the Laser Interferometer Gravitational-Wave Observatory (LIGO) and Virgo ground-based interferemeters. To date, eleven events have been reported by the LIGO and Virgo detectors (Abbott 2018), and... | [
"Broadhurst et al. 2019"
] | [
"Recent works have studied lensing effects in the existing LIGO/Virgo O1 and O2 events"
] | [
"Background"
] | [
[
741,
763
]
] | [
[
630,
715
]
] |
2019MNRAS.482..194B__Mallmann_et_al._2018_Instance_1 | Observationally, it is a big challenge to conclude whether AGN’s feedback could regulate star formation or not, and how it regulates star formation. On one hand, if strong outflows emerge, they could clear out the star-forming gas to suppress star formation (Alexander & Hickox 2012; García-Burillo et al. 2014; Alatalo ... | [
"Mallmann et al. 2018"
] | [
"In fact observations show either no or positive relationships between star formation rates and SMBH accretion rates but no negative trends are seen"
] | [
"Motivation"
] | [
[
970,
990
]
] | [
[
745,
892
]
] |
2019MNRAS.487..845B__Acero_et_al._2015_Instance_1 |
Fermi–LAT (Atwood et al. 2009) is a pair conversion telescope, with a field of view (FoV) of above 2 sr, operating in the energy range from 20 MeV to 300 GeV. It is the most sensitive instrument available in this energy range (Ackermann et al. 2012). A few months after the launch in 2008 June, Fermi–LAT started to ope... | [
"Acero et al. 2015"
] | [
"The third Fermi–LAT catalogue (3FGL catalogue:",
"has been used to include the contributions of sources inside the ROI."
] | [
"Uses",
"Uses"
] | [
[
1331,
1348
]
] | [
[
1284,
1330
],
[
1350,
1419
]
] |
2020ApJ...903L..22T__Vuitton_et_al._2007_Instance_2 | While the Loison et al. (2015) CH3C3N model corroborates the upper atmospheric abundance of C4H3N inferred by Vuitton et al. (2007) from the T5 INMS measurements (a factor of 2 higher than those derived from T40 in Vuitton et al. 2019), a large disparity between the photochemical models (and within the ensemble of mode... | [
"Vuitton et al. 2007"
] | [
"Aside from electron dissociative recombination of C4H3NH+",
"neutral production of CH3C3N can occur in a few ways"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
568,
587
]
] | [
[
509,
566
],
[
590,
642
]
] |
2020MNRAS.493L..98S__Sourie,_Oertel_&_Novak_2016_Instance_1 | To solve equations (9)−(11), the pulsar rotation rate Ω0, the long-term spin-down rate $\dot{\Omega }_\infty$, the initial lag δΩ0, the mutual-friction coefficients $\mathcal {B}_{\operatorname{\text{f}}}$ and $\mathcal {B}_{\operatorname{\text{pin}}}$, and the ratios $I_{\operatorname{\text{n}}}^{\operatorname{\text{f... | [
"Sourie, Oertel & Novak 2016"
] | [
"Typical values for the underlying parameters are: $\\varepsilon _{\\operatorname{\\text{p}}}^{\\operatorname{\\text{pin}}}\\simeq 0.05-0.2$, $\\varepsilon _{\\operatorname{\\text{p}}}^{\\operatorname{\\text{f}}}\\simeq 0.1-0.5$ (see e.g."
] | [
"Uses"
] | [
[
1076,
1103
]
] | [
[
827,
1052
]
] |
2021MNRAS.505.2111L__Xu_et_al._2018_Instance_1 | Recently, quasars observed with multiple measurements, another potential cosmological probe with a higher redshift range that reaches to z ∼ 5, is becoming popular to constrain cosmological models in the largely unexplored portion of redshift range from z ∼ 2 to z ∼ 5. A sample that contains 120 angular size measuremen... | [
"Xu et al. 2018"
] | [
"Recently, quasars observed with multiple measurements, another potential cosmological probe with a higher redshift range that reaches to z ∼ 5, is becoming popular to constrain cosmological models in the largely unexplored portion of redshift range from z ∼ 2 to z ∼ 5. A sample that contains 120 angular size measu... | [
"Background",
"Background"
] | [
[
617,
631
]
] | [
[
0,
420
],
[
442,
545
]
] |
2022AandA...666A..67P__Gall_et_al._2017_Instance_1 | The KN coincident with GW170817 showed a rapidly fading EM transient in the optical and infrared bands. The term kilonova was historically coined from the perception of its brightness being a thousand times larger than a nova (Li & Paczyński 1998; Rosswog 2005; Metzger et al. 2010). We discuss in this work that, even i... | [
"Gall et al. 2017"
] | [
"An alternative scenario, such as dust formation in the KN that could also explain such a blue-red evolution, has been ruled out"
] | [
"Background"
] | [
[
925,
941
]
] | [
[
796,
923
]
] |
2019ApJ...881...42J__Kelson_et_al._2000_Instance_1 | Stellar population evolution studies beyond z ≈ 1 have primarily focused on ages through studies of luminosity changes. Beifiori et al. (2017) used new data for 19 galaxies in z = 1.3–1.6 clusters obtained with the Very Large Telescope/KMOS to extend the redshift coverage of the results regarding the evolution of the m... | [
"Kelson et al. 2000"
] | [
"The authors used their new results together with the available literature results covering up to z = 1.3",
"to further solidify the evidence supporting passive evolution and a formation redshift zform ≈ 2."
] | [
"Uses",
"Compare/Contrast"
] | [
[
549,
567
]
] | [
[
383,
487
],
[
806,
903
]
] |
2022ApJ...928...38T__Tiwari_&_Nusser_2016_Instance_1 | The LoTSS survey, homogeneously covering the whole northern sky complete down to the sub mJy limit will overcome statistical limitations due to shot noise. The large galaxy number density and large sky coverage will substantially reduce cosmic variance in cosmological analysis. The radio galaxies, tracing the backgroun... | [
"Tiwari & Nusser 2016"
] | [
"The upcoming LoTSS catalogs, covering a large sky area, will help us to explore further regarding",
"and the current puzzling dipole signal observed with radio catalogs"
] | [
"Future Work",
"Future Work"
] | [
[
949,
969
]
] | [
[
545,
642
],
[
760,
827
]
] |
2022MNRAS.510.4723P__Henri_&_Petrucci_1997_Instance_1 | A new result brought by our work is the role of incident polarization on the reflected spectral outcome. Although some X-ray polarization of the primary radiation is expected to be due to Comptonization of thermal radiation inside the corona, general estimates for the polarization degree of the primary source are rathe... | [
"Henri & Petrucci 1997"
] | [
"In case of lamp-post models",
"general-relativistic effects will rotate the polarization position angle along null geodesics from the corona towards the disc",
"and the situation becomes more general for incident disc irradiation, i.e. any incident state of polarization is possible. Our computations, apart fro... | [
"Compare/Contrast",
"Compare/Contrast",
"Compare/Contrast"
] | [
[
810,
831
]
] | [
[
731,
758
],
[
919,
1045
],
[
1068,
1498
]
] |
2021MNRAS.501.3781R__Nisini_et_al._2005_Instance_1 | While spatially extended optical jets and bipolar CO molecular outflows have been observed in numerous Class 0/I protostars (e.g. Reipurth & Bally 2001; Bally 2016, and references therein), near-infrared high-resolution spectroscopy and spectroimaging observations in the past two decades have made it possible to study ... | [
"Nisini et al. 2005"
] | [
"While spatially extended optical jets and bipolar CO molecular outflows have been observed in numerous Class 0/I protostars",
"near-infrared high-resolution spectroscopy and spectroimaging observations in the past two decades have made it possible to study the kinematics of the outflowing gas and physical proper... | [
"Background",
"Background"
] | [
[
511,
529
]
] | [
[
0,
123
],
[
190,
479
]
] |
2018ApJ...866L...1S__Pecharromán_et_al._1999_Instance_7 | 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"
] | [
"XRD of their sample obtained from heating boehmite to 1173 K",
"suggests δ-alumina to be present, though some amounts of θ-alumina and α-alumina are present, as they deduce from XRD and infrared and NMR spectroscopy."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1837,
1860
]
] | [
[
1775,
1835
],
[
1862,
2014
]
] |
2019MNRAS.487.1210T__McNamara_&_Nulsen_2007_Instance_2 | 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"
] | [
"AGNs can release copious amounts of energy into the intracluster medium (ICM) through many ways, including: jetted outflows that inflate cavities, weak shocks, sound waves, or turbulence in the ICM (e.g."
] | [
"Background"
] | [
[
1637,
1659
]
] | [
[
1404,
1607
]
] |
2021MNRAS.506.5935R__Ellison_et_al._2011_Instance_1 | The discovery of a correlation between the mass of supermassive black holes (SMBHs) and several properties of their host galaxies (e.g. Magorrian et al. 1998; Ferrarese & Merritt 2000; Gebhardt et al. 2000; Kormendy & Ho 2013) has suggested that the growth of SMBHs and their host galaxies are tightly connected. Mergers... | [
"Ellison et al. 2011"
] | [
"It has been shown that the fraction of AGN in mergers tends to increase as the separation between the two galaxies decreases"
] | [
"Background"
] | [
[
1418,
1437
]
] | [
[
1292,
1416
]
] |
2021ApJ...911...79P___2007_Instance_1 | Now we turn to the question of whether there are any general trends or strong correlations between the degree of HSP compliance, the average Fidx, and the average Φ derived from the AR samples contained in the defined HRs. As shown in the scatter plot of the average Fidx versus the HSP (Figure 5(a)), we find a weak ten... | [
"Leka & Barnes",
"2007"
] | [
"On the other hand, a positive correlation exists between the average Φ and the average Fidx with the linear PCC = 0.65 (refer to Figure 5(b)). Such correlation of Φ with flaring activity in individual ARs has been reported in many previous studies (e.g.,"
] | [
"Similarities"
] | [
[
1012,
1025
],
[
1032,
1036
]
] | [
[
757,
1011
]
] |
2016MNRAS.463.3783B__Reid_&_White_2011_Instance_2 | It is well known that a per cent level understanding of the anisotropy of the redshift-space galaxy clustering is needed to accurately recover cosmological information from the RSD signal in order to shed light on the issue of dark energy versus modified gravity. From a statistical point of view, the source of the anis... | [
"Reid & White 2011"
] | [
"We have compared to N-body simulations the well-known GSM",
"We have concluded that, among the three, QGQ is the only model capable of providing a precise redshift-space correlation function on scales down to ∼5 h−1 Mpc over the range of redshifts covered by future surveys."
] | [
"Compare/Contrast",
"Differences"
] | [
[
2333,
2350
]
] | [
[
2274,
2331
],
[
2628,
2841
]
] |
2018ApJ...856..140H__Leary_et_al._2009_Instance_1 | The number of BHs, their mass distribution, and the number density are poorly known in NSCs. Theoretically, a single-mass distribution of objects forms a power-law density cusp around a massive object with n(r) ∝ r−1.75 (Bahcall & Wolf 1976), where n(r) is the number density, and r is the distance from the MBH. For mul... | [
"O’Leary et al. 2009"
] | [
"As BHs are heavier than typical stars, they are expected to relax into the steeper cusps. The relaxation time of BH populations is much shorter: 0.1–1 Gyr"
] | [
"Compare/Contrast"
] | [
[
985,
1004
]
] | [
[
829,
983
]
] |
2017ApJ...845...86E__Soler_&_Terradas_2015_Instance_2 | Among the suggestedmechanisms responsible for the strong damping of the coronal loop oscillations (e.g., Ruderman & Roberts 2002; Ofman 2005, 2009; Morton & Erdélyi 2009) resonant absorption of the MHD waves, which was established first by Ionson (1978), is a strong candidate. Several works developed this theory (e.g.,... | [
"Soler & Terradas 2015"
] | [
"The background Alfvén or slow continuum can be due to the variation of the plasma density"
] | [
"Background"
] | [
[
1430,
1451
]
] | [
[
1254,
1343
]
] |
2017ApJ...850L..40A__Yang_et_al._2017_Instance_1 | Aided by the tight localization constraints of the three-detector network and the proximity of the GW source, multiple independent surveys across the EM spectrum were launched in search of a counterpart beyond the sGRB (Abbott et al. 2017c). Such a counterpart, SSS17a (later IAU-designated AT 2017gfo), was first discov... | [
"Yang et al. 2017"
] | [
"Five other teams made independent detections of the same optical transient and host galaxy all within about one hour and reported their results within about five hours of one another"
] | [
"Background"
] | [
[
756,
772
]
] | [
[
489,
671
]
] |
2018ApJ...856..136P__Burkhart_et_al._2010_Instance_1 | Depending on the specific driver, the characteristics of turbulence will then be imprinted within the ISM mainly as three-dimensional density and velocity fluctuations, and these fluctuations have been traditionally studied via correlation functions such as the spatial power spectrum (SPS) (e.g., Crovisier & Dickey 198... | [
"Burkhart et al. 2010"
] | [
"In particular, the SPS approach has been applied to observations of various Galactic and extragalactic environments (e.g.,"
] | [
"Background"
] | [
[
623,
643
]
] | [
[
438,
560
]
] |
2015ApJ...806...15Z___2015_Instance_1 | Since the launch of Swift (Gehrels et al. 2004) in 2004, the nature of jet breaks in gamma-ray burst (GRB) afterglows has become increasingly puzzling. There is strong evidence that the ejecta from the GRB central engine must be jet-like (Zhang & Mészáros 2004). Thus a collimation correction factor,
, where
... | [
"Guiriec et al.",
"2015"
] | [
"Internally, the ejecta release their energy through",
"or photospheric dissipation (e.g.,",
"and produce the prompt gamma-ray emission of GRBs."
] | [
"Background",
"Background",
"Background"
] | [
[
915,
929
],
[
942,
946
]
] | [
[
661,
712
],
[
880,
914
],
[
1016,
1066
]
] |
2018ApJ...864..160R__Bhat_et_al._2013_Instance_1 | Figure 9 shows the components required for such a time-domain survey, with the PC beamformer as specified above. The required components are shown in four different colors. Visibilities computed in the uGMRT backend (GWB; marked in blue) at 1 ms time resolution are transferred to the the PC beamformer nodes (marked in ... | [
"Bhat et al. 2013"
] | [
"The multi-DM search for single pulses (colored in yellow) on each of these visibility beams would need to be executed on a separate FRB cluster, followed by coincidence filtering to remove spurious events"
] | [
"Future Work"
] | [
[
1187,
1203
]
] | [
[
981,
1185
]
] |
2017AandA...601A..72I__Kobayashi_&_Tanaka_2010_Instance_3 | Small grains, which contribute most to infrared emission, are removed by collisional fragmentation and blown out by radiation pressure. The removal timescale is much shorter than the ages of host stars. Disruptive collisions among underlying large bodies, which are called planetesimals, produce smaller bodies and colli... | [
"Kobayashi & Tanaka 2010"
] | [
"In the obtained size distribution, erosive collisions are more important than catastrophic collisions (see Fig. 10 of",
"Taking into account the size distribution and erosive collisions, we derive t0 according to the collisional cascade (see Appendix E for derivation), (3)\\begin{eqnarray} t_0&\\sim& 1.3... | [
"Uses",
"Uses"
] | [
[
1275,
1298
]
] | [
[
1157,
1274
],
[
1301,
1890
]
] |
2020ApJ...897...94G__Stanway_&_Eldridge_2019_Instance_1 | It is interesting that the sources with suspected or confirmed Lyman continuum radiation at high redshifts are peculiar and rare, bright SFGs with rather hard ionizing spectra marked by high-ionization emission lines (e.g., N v, C iv, He ii, O iii, C iii). Their presence at high redshift can be hardly explained by pure... | [
"Stanway & Eldridge 2019"
] | [
"Their presence at high redshift can be hardly explained by pure SFGs, even requiring uncommon assumptions (e.g., large stellar rotation, binary stellar population, top-heavy initial mass function, extremely low metallicity) as discussed by a number of recent works (see"
] | [
"Compare/Contrast"
] | [
[
833,
856
]
] | [
[
257,
526
]
] |
2017AandA...599A..55B__Shakura_1972_Instance_1 | When the characteristic time of variability of the mass flux along the accretion disk is longer than the relaxation time of the local disk equilibrium, it is possible to use the approximation of local equilibrium Shakura (1972), see also Bisnovatyi-Kogan (2011), to calculate the transient disk structure. The equilibriu... | [
"Shakura (1972)"
] | [
"When the characteristic time of variability of the mass flux along the accretion disk is longer than the relaxation time of the local disk equilibrium, it is possible to use the approximation of local equilibrium",
"see also Bisnovatyi-Kogan (2011), to calculate the transient disk structure."
] | [
"Uses",
"Uses"
] | [
[
213,
227
]
] | [
[
0,
212
],
[
229,
305
]
] |
2019MNRAS.482..194B__Choi_et_al._2015_Instance_1 | Observationally, it is a big challenge to conclude whether AGN’s feedback could regulate star formation or not, and how it regulates star formation. On one hand, if strong outflows emerge, they could clear out the star-forming gas to suppress star formation (Alexander & Hickox 2012; García-Burillo et al. 2014; Alatalo ... | [
"Choi et al. 2015"
] | [
"The heating by jets propagating through the galaxies could prevent gas from cooling and cut-off the gas supply for further star formation"
] | [
"Background"
] | [
[
543,
559
]
] | [
[
382,
519
]
] |
2019MNRAS.490.1870L__Guo_et_al._2015_Instance_2 | In principle, we could measure the multipole moments in a given simulation by directly populating dark matter haloes in the simulation with galaxies. However, this is computationally very expensive and comes with realization noise due to the random number and phase-space positions of galaxies. Instead, we use a tabulat... | [
"Guo et al. 2015"
] | [
"With such a bin width of ∼0.03 dex, any biases in ξ are less than $5{{\\ \\rm per\\ cent}}$ of the observational uncertainty for a BOSS CMASS-like sample (see"
] | [
"Uses"
] | [
[
2541,
2556
]
] | [
[
2385,
2540
]
] |
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