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 |
|---|---|---|---|---|---|---|
2020AandA...635A.154M__Hummels_et_al._(2017)_Instance_1 | This paper presents a new 3D RT code, RAdiation SCattering in Astrophysical Simulations (RASCAS), which was designed to construct accurate multi-wavelength mock observations (spectra, images, or datacubes) from high-resolution simulations. RASCAS deploys a general two-step methodology (e.g. Hummels et al. 2017; Barrow ... | [
"Hummels et al. 2017"
] | [
"RASCAS deploys a general two-step methodology (e.g."
] | [
"Uses"
] | [
[
292,
311
]
] | [
[
240,
291
]
] |
2022AandA...663A.172M___2012_Instance_2 | We note that Pavesi et al. (2019) derived a lower κs parameter log(κs) ≈ −1 for HZ10, by observing the CO(2-1) line, which implies a low star formation efficiency for this source. The conflict between the two results can be explained by the fact that Pavesi et al. (2019) estimated the gas mass by adopting a large CO-to... | [
"Narayanan et al.",
"2012"
] | [
"On the other hand, high values of temperature, surface density, and velocity dispersion in a turbulent ISM of starbursts and merging systems will shift αCO towards lower values"
] | [
"Compare/Contrast"
] | [
[
1728,
1744
],
[
1751,
1755
]
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[
1550,
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]
] |
2022MNRAS.511.4946N__Myers_et_al._2015_Instance_1 | We validated our results against different selection effects due to redshift, luminosity, incompleteness of the FIRST survey, and incomplete radio counter-part identifications. However, we have not explicitly checked for any bias due to incomplete target selection in the DR16Q catalogue. As quasars are chosen for spect... | [
"Myers et al. 2015"
] | [
"To our rescue, eBOSS also targets all SDSS point sources that are within 1 arcsec of a radio detection in the FIRST point source catalogue"
] | [
"Uses"
] | [
[
1187,
1204
]
] | [
[
1047,
1185
]
] |
2021MNRAS.503.6170B__Santos-Santos,_Domínguez-Tenreiro_&_Pawlowski_2020_Instance_1 | Flattened distributions of very likely co-orbiting satellite galaxies around the MW (Lynden-Bell 1976, 1982; Kroupa, Theis & Boily 2005; Pawlowski, Pflamm-Altenburg & Kroupa 2012) and M31 (Metz, Kroupa & Jerjen 2007; Ibata et al. 2013) have long posed a challenge to our understanding of galaxy formation in the ΛCDM con... | [
"Santos-Santos, Domínguez-Tenreiro & Pawlowski 2020"
] | [
"Recent proper motion data confirm that most of the classical MW satellites do indeed have a common orbital plane",
"aligned with the plane normal defined by the satellite positions alone"
] | [
"Background",
"Background"
] | [
[
570,
620
]
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[
326,
438
],
[
498,
568
]
] |
2016MNRAS.463..512D__Sutter_et_al._2014_Instance_1 | The cosmic web, consisting of haloes, voids, filaments, and walls in large-scale structure is predicted by the cold dark matter model (Bond, Kofman & Pogosyan 1996; Pogosyan et al. 1998) and confirmed by large galaxy surveys (e.g. de Lapparent, Geller & Huchra 1986; Colless et al. 2003; Alam et al. 2015). Among these l... | [
"Sutter et al. 2014"
] | [
"Among these large-scale structures, the underdensities of the universe, i.e. cosmic voids, have been shown to have great potential for constraining dark energy and testing theories of gravity via several measurements. These measurements include: distance measurement via the Alcock–Paczyński test"
] | [
"Motivation"
] | [
[
640,
658
]
] | [
[
307,
603
]
] |
2020MNRAS.492.5152Z__Samarasinha_&_Mueller_2013_Instance_1 | Scheeres (2007) and Nesvornỳ & Vokrouhlickỳ (2007) established averaging methods for YORP effects experienced by small bodies (mostly asteroids) taking real-time insolation and shape into account. However, unlike thermal radiation, as Fig. 2 shows, the CO (or H2O) production rate variation versus solar distance is too ... | [
"Samarasinha & Mueller 2013"
] | [
"There are further analytical approaches described in the literature",
", although these models predicted a change in the spin state of the nucleus without taking into consideration the exact 3D shape model and its variation induced by mass loss."
] | [
"Background",
"Differences"
] | [
[
768,
794
]
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[
699,
766
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[
852,
1026
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2022MNRAS.515.1568W__Weinberg_et_al._2003_Instance_1 | The temperature of the IGM can be measured using the effect of Doppler broadening on the forest of Ly α absorption line seen in the spectra of high-redshift quasars and galaxies (Rauch 1998; Savaglio, Panagia & Padovani 2002). Traditionally, the absorbing clouds were treated as being distinct and fitting Voigt profiles... | [
"Weinberg et al. 2003"
] | [
"However, since the identification of the Ly α forest in hydrodynamic simulations",
"it was realized that in the context of cosmological models for structure formation, the Ly α forest is due to a fluctuating, continuous IGM (e.g."
] | [
"Background",
"Background"
] | [
[
824,
844
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[
516,
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[
669,
814
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2020ApJ...899..118C__Wang_et_al._2019_Instance_1 | The origin of giant pulses has been remaining a mystery since the discovery of giant pulses from Crab pulsar (Staelin & Reifenstein 1968). The generation of giant pulse activity was pointed to be an intrinsic phenomenon within the pulsar (Hankins 1971). The giant pulses are supposed to be the product of induced Compton... | [
"Wang et al. 2019"
] | [
"Alternatively, the origination of giant pulses is proposed from the coherent instability of plasma near the magnetic equator of light cylinder"
] | [
"Background"
] | [
[
719,
735
]
] | [
[
575,
717
]
] |
2015MNRAS.452.2837M__Mendigutía_2013_Instance_1 | We constructed a sample of artificial stars representing the TT and HAeBe regime by using synthetic models of stellar atmospheres (Kurucz 1993). The properties of each object are provided in Table 1. Columns two and three show the stellar luminosity and effective temperature. From these, the stellar radii was derived, ... | [
"Mendigutía 2013"
] | [
"Magnetospheric accretion (MA) shock modelling was carried out for each star by adding (blackbody) accretion contributions to the photospheric (Kurucz) spectra (see e.g. the reviews in"
] | [
"Uses"
] | [
[
670,
685
]
] | [
[
455,
638
]
] |
2019MNRAS.490.5567Z__Aschwanden_et_al._1999_Instance_1 | Coronal loops are curvilinear structures in the outer layer of the solar atmosphere, and they are formed by thermal plasmas confined by magnetic fields and well reflect the coronal magnetic field configurations. Because a number of active phenomena in the solar atmosphere, such as flares, the solar wind, coronal mass e... | [
"Aschwanden et al. 1999"
] | [
"Therefore, on the basis of the oscillation of coronal loops, especially their oscillation characteristics in frequency, phase and attenuation coefficient, solar physicists can further understand the relationships between the coronal magnetic field, flares and CME",
"and obtain corresponding physical parameters a... | [
"Motivation",
"Motivation"
] | [
[
1099,
1121
]
] | [
[
834,
1097
],
[
1152,
1238
]
] |
2021MNRAS.501.2897G__Pribulla_&_Rucinski_2006_Instance_1 | EE Cet (ADS 2163 B) is the southern (slightly fainter) component of the visual binary WDS 02499+0856 (Mason et al. 2001). It was discovered by the HIPPARCOS mission (Perryman et al. 1997), by noticing the variability of the combined light of both visual components. Lampens et al. (2001) performed photometric measuremen... | [
"Pribulla & Rucinski (2006)"
] | [
"lists the orbital parameters (orientation and separation) of WDS 02499+0856 and gave θ = 194°, ρ = 5.66 arcsec and magnitude difference ΔV = 0.07 mag (the magnitude difference can be as large as ΔV = 0.36 mag, due to photometric variability of the eclipsing binary)"
] | [
"Background"
] | [
[
434,
460
]
] | [
[
461,
726
]
] |
2021MNRAS.503.3279S__Magrini_et_al._2017_Instance_2 | Among the several features, the distribution of chemical elements across the Galactic disc historically constitutes the most important constraint to chemo-dynamical models of our Milky Way. A number of studies (e.g. Tosi 1988; Hayden et al. 2014, 2015; Anders et al. 2017) have shown the spatial distributions of chemica... | [
"Magrini et al. 2017"
] | [
"Complementary to the study of the overall metallicity distribution, the abundance ratios of several other elements, such as α-elements, iron peak, odd-z, and neutron capture, can provide deep insight into the variety of nucleosynthesis processes, with their production sites and time-scales (e.g."
] | [
"Background"
] | [
[
2068,
2087
]
] | [
[
1677,
1973
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2018ApJ...854..167G__Meece_et_al._2017_Instance_1 | In the turbulent gaseous halos of clusters, groups, and galaxies (particularly massive ones), extended filaments and clouds condense out of the hot plasma in a top-down nonlinear23
23
This nonlinear condensation process has properties significantly different from those of classic linear thermal instability (TI); the l... | [
"Meece et al. 2017"
] | [
"The thermal state and kinematics of the progenitor hot plasma halo drive the formation and evolution of all the condensed structures, which inherit some of the parent properties. Part of the inner condensed gas eventually accretes onto the central supermassive black hole (SMBH), igniting the feedback response and ... | [
"Background"
] | [
[
1094,
1111
]
] | [
[
586,
980
]
] |
2020AandA...642A.170V__Engelbrecht_&_Burger_2010_Instance_1 | Jovian electrons were used as test particles to model the charged-particle transport computationally (see e.g. Chenette et al. 1977; Conlon 1978; Fichtner et al. 2000; Zhang et al. 2007, and references therein) to ascertain the diffusion coefficients parallel and perpendicular to the Heliospheric Magnetic Field (HMF). ... | [
"Engelbrecht & Burger 2010"
] | [
"Furthermore, given the demonstrated sensitivity of computed low-energy galactic electron intensities to various turbulence quantities (see",
", it may be possible to draw conclusions from Jovian electrons to better understand the behaviour of those quantities in regions of the heliosphere where spacecraft observ... | [
"Uses",
"Uses"
] | [
[
598,
623
]
] | [
[
459,
597
],
[
648,
856
]
] |
2015ApJ...815....7V__Bale_et_al._2005_Instance_1 | Turbulence in plasmas is a complex phenomenon that is characterized by different regimes in different ranges of spatial and temporal scales. Turbulence in the solar wind has been extensively studied, both by detailed analyses of in situ measurements and from a theoretical point of view; see Bruno & Carbone (2005) for a... | [
"Bale et al. 2005"
] | [
"As motivation, we note that a variety of observations in the solar wind",
"have suggested that fluctuations near the end of the magnetohydrodynamic (MHD) inertial cascade range, and approaching the kinetic plasma range, may consist primarily of kinetic Alfvén waves (KAWs)."
] | [
"Motivation",
"Motivation"
] | [
[
986,
1002
]
] | [
[
913,
984
],
[
1026,
1224
]
] |
2018AandA...616A..11G__Forbes_et_al._2012_Instance_1 | In addition to secular evolutionary processes, a disc galaxy like ours is expected to have experienced several accretion events in its recent and early past (Bullock & Johnston 2005; De Lucia & Helmi 2008; Stewart et al. 2008; Cooper et al. 2010; Font et al. 2011; Brook et al. 2012; Martig et al. 2012; Pillepich et al.... | [
"Forbes et al. 2012"
] | [
"Events that took place in the far past are expected to have induced a thickening of the early Galactic disc,",
"and second by agitating the gaseous disc from which new stars are born, generating early stellar populations with higher initial velocity dispersions than those currently being formed"
] | [
"Background",
"Background"
] | [
[
1373,
1391
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[
746,
854
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[
1163,
1346
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2017AandA...608A..75C__Osten_et_al._2005_Instance_1 | The spectral energy distribution of the flare determines the altitude range in the planet’s atmosphere that is affected by the flare. Intense flares on AU Mic display a strong continuum emission enhancement in the XUV (see Fig. 2c) which results in increased ionisation over a broad altitude range in the thermosphere. L... | [
"Osten et al. 2005"
] | [
"There have not been many simultaneous multi-wavelength studies of flaring stars",
"There is a particular dearth of simultaneous data in the EUV which is critical for studies of exoplanetary upper atmospheres, but where measurements are difficult due to ISM absorption. More observations are needed, but if young, ... | [
"Motivation",
"Motivation"
] | [
[
805,
822
]
] | [
[
704,
783
],
[
825,
1237
]
] |
2017MNRAS.469.3108C__Schweizer_&_Seitzer_1992_Instance_1 | Having intermediate colours between the blue cloud and the red sequence, galaxies populating the so-called green-valley (e.g. Salim 2014; Schawinski et al. 2014) are generally considered as the transiting objects par excellence (Martin et al. 2007; Mendel et al. 2013; Salim 2014; Schawinski et al. 2014). Among these, t... | [
"Schweizer & Seitzer 1992"
] | [
"Although hampered by the short duration of the quenching process, the search for galaxies in this critical phase of evolution has been carried on by several authors in the past decades. Galaxies characterized by both a tidally disturbed morphology and intermediate colours (e.g",
"have been considered as valid 'r... | [
"Background",
"Background"
] | [
[
731,
755
]
] | [
[
452,
729
],
[
1055,
1120
]
] |
2022ApJ...929...32S__Singh_et_al._2017_Instance_1 | The 21 cm global spectrum experiments aim to measure the sky-averaged spectrum with high precision so as to probe the early epochs of the universe. There are a number of such ground-based experiments, including the Experiment to Detect the Global Epoch-of-Reionization Signature (EDGES; Bowman et al. 2008; Bowman & Roge... | [
"Singh et al. 2017"
] | [
"There are a number of such ground-based experiments, including",
"the Shaped Antenna measurement of the background RAdio Spectrum (SARAS;"
] | [
"Background",
"Background"
] | [
[
624,
641
]
] | [
[
148,
210
],
[
533,
604
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] |
2022MNRAS.512.1629F__Fioroni,_Savage_&_DeYonker_2019_Instance_1 | The ORCA software (version 4.0.2) (Neese 2012) was used for all geometry minimizations, potential energy surface (PES), and vibrational frequency analyses using the global hybrid functional PW6B95 (Zhao & Truhlar 2005) coupled to the split valence triple-ζ def2-TZVPP basis set with two sets of polarization functions (W... | [
"Fioroni, Savage & DeYonker 2019"
] | [
"The reliability of the used method is also underlined by the good qualitative agreement between the Density Functional Theory (DFT) and MP2-F12 calculations as found in previous works"
] | [
"Similarities"
] | [
[
968,
999
]
] | [
[
737,
920
]
] |
2016MNRAS.461.1719C__Clements,_Dunne_&_Eales_2010_Instance_1 | The early history of galaxy clusters is a poorly constrained aspect of galaxy and large-scale structure formation. Hierarchical clustering models predict that massive elliptical galaxies will form in the cores of what will become the most massive galaxy clusters today, but the epoch of the bulk of star formation for th... | [
"Clements, Dunne & Eales 2010"
] | [
"Theoretical models by Granato et al. (2004) suggest that forming clusters will go through a phase in which multiple members will undergo near-simultaneous massive bursts of star formation. The spectral energy distribution of these objects would be dominated by the far-IR, as is the case for local massive starburst... | [
"Background"
] | [
[
1027,
1055
]
] | [
[
704,
1026
]
] |
2020ApJ...898L..33P__Delrez_et_al._2018_Instance_2 | For the TRAPPIST-1 system, data obtained by HST provide initial constraints on the extent and composition of the planet’s atmospheres, suggesting that the four innermost planets do not have a cloud/haze-free H2-dominated atmosphere (de Wit et al. 2016, 2018). However, follow-up work by Moran et al. (2018) have shown th... | [
"Delrez et al. 2018"
] | [
"While the K2 optical data set detected a 3.3 day periodic 1% photometric modulation, it is not present in the Spitzer observations"
] | [
"Differences"
] | [
[
2097,
2115
]
] | [
[
1965,
2095
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] |
2019MNRAS.490..157M__Yu_&_Tremaine_2003_Instance_2 | As a class, the fastest stars in our Galaxy are expected to be hypervelocity stars (HVSs). These were first theoretically predicted by Hills (1988) as the result of a three-body interaction between a binary star and the massive black hole in the Galactic Centre (GC), Sagittarius A*. Following this close encounter, a st... | [
"Yu & Tremaine 2003"
] | [
"Other possible alternative mechanisms leading to the acceleration of HVSs are the encounter between a single star and a massive black hole binary in the GC (e.g."
] | [
"Compare/Contrast"
] | [
[
2317,
2335
]
] | [
[
2155,
2316
]
] |
2022ApJ...927..138L__Lucas_et_al._2018_Instance_1 | A color–color diagram in V − R versus B − V of the individual SSCs projected against the central spiral is shown in Figure 2 (left panel). The manner in which photometry of the individual stellar clusters was performed, including background subtraction, is described at length in Lim et al. (2020). In brief, we used the... | [
"Lucas et al. 2018"
] | [
"Conversions to magnitude are based on the standard zero-points in the Vega system as described in the ACS Data Handbook"
] | [
"Uses"
] | [
[
691,
708
]
] | [
[
570,
689
]
] |
2018MNRAS.479..615M__Shakura_&_Sunyaev_1973_Instance_1 | We also detect a Compton hump at around 15–30 keV during the 2016 NuSTAR observation. The inclusion of the 10–50 keV spectral data does not affect the spectral model parameters (disc inclination angle, spin, emissivity indices, and break radius) obtained from fitting of the 0.3–10 keV spectrum only. The best-fitting va... | [
"Shakura & Sunyaev 1973"
] | [
"At high accretion rate, the inner region of a standard α-disc"
] | [
"Uses"
] | [
[
717,
739
]
] | [
[
654,
715
]
] |
2021AandA...649A.142A__Zhang_et_al._2019_Instance_1 | An et al. (1988) and Wu et al. (1990) investigated the effects of plasma injection on the formation of the Kippenhahn-Schlüter model of prominence in optimum conditions. These authors found that for high values of the plasma-β parameter (the ratio of plasma pressure to magnetic pressure) the magnetic arcade develops a ... | [
"Zhang et al. 2019"
] | [
"Recent works suggest that the deformation of the magnetic field lines is determined by the parameter δ (the ratio of the gravity to the magnetic pressure)"
] | [
"Background"
] | [
[
825,
842
]
] | [
[
651,
805
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] |
2022MNRAS.517.4529B__Boruah,_Rozo_&_Fiedorowicz_2022_Instance_1 | The other criteria that we can use to categorize the reconstruction methods is whether the reconstruction is performed using forward-modelling or uses a direct inversion from the data. Inverting non-linear problems from partial, noisy, observations is an ill-posed inverse problem, which makes forward-modelled Bayesian ... | [
"Boruah, Rozo & Fiedorowicz 2022"
] | [
"Bayesian reconstruction methods have become increasingly popular in cosmology and have been applied in a range of different applications such as",
"weak lensing"
] | [
"Background",
"Background"
] | [
[
729,
760
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[
409,
553
],
[
661,
673
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2021ApJ...908..187W__Hayakawa_et_al._2020b_Instance_1 | Before 1500 A.D., when the magnetic latitude of China was higher than that at present, most of the observed aurorae were caused by CIRs and moderate CMEs. After 1500 A.D., the GNP moved to Canada. This caused the geomagnetic field latitude of China to decrease considerably. Meanwhile, the field intensity decreased to i... | [
"Hayakawa et al. 2020b"
] | [
"After 1500 A.D., the GNP moved to Canada. This caused the geomagnetic field latitude of China to decrease considerably. Meanwhile, the field intensity decreased to its minimum value in the last 2000 yr. Under these conditions, it would have been very rare to observe the aurora in most places in China after the 16t... | [
"Background"
] | [
[
533,
554
]
] | [
[
155,
507
]
] |
2022MNRAS.515.5416Y__Wechsler_et_al._2022_Instance_1 | There are several different methods used in the literature for creating mock catalogues and light-cones. In purely empirical methods such as the JAdes extraGalactic Ultradeep Artificial Realizations (jaguar) models used to create mock catalogues in support of the JADES survey (Williams et al. 2018), observed galaxy pro... | [
"Wechsler et al. 2022"
] | [
"In what are sometimes called ‘semi-empirical’ methods [also called subhalo abundance matching (SHAM) or halo occupation distribution (HOD) models; see Wechsler & Tinker 2018], galaxy properties are mapped on to the properties of dark matter haloes such that a set of observational quantities is reproduced"
] | [
"Background"
] | [
[
855,
875
]
] | [
[
459,
764
]
] |
2021ApJ...914...88P__Forgan_et_al._2018b_Instance_1 | Observing with instruments such as the Atacama Large Millimeter/submillimeter Array (ALMA) is crucial to our understanding of planet-formation mechanisms, as we can observe at wavelengths that trace continuum emission from the cold midplane (e.g., Testi et al. 2014), where we expect planets to be forming or have alread... | [
"Forgan et al. 2018b"
] | [
"In the case of midplane spiral structures, their origin may be linked to the presence of a companion—stellar, fly-by, or planetary"
] | [
"Background"
] | [
[
515,
534
]
] | [
[
330,
460
]
] |
2017AandA...601A..87C__Falcke_(1996)_Instance_2 | In a quasi-isothermal jet, Uj is (17)\begin{equation} \label{eq:U_j_quasi} U_{\rm j} = \zeta n_0 m_{\rm p} c^2\left(\frac{\gamma_{\rm j}\beta_{\rm j}}{\gamma_0\beta_0}\right)^{-\Gamma}\left(\frac{z}{z_0}\right)^{-2} \cdot \end{equation}Uj=ζn0mpc2γjβjγ0β0−Γzz0-2·Substituting Eqs. (17) and (13) into Eq. (10), and assumin... | [
"Falcke (1996)"
] | [
"However, it differs from Eq. (2) in"
] | [
"Differences"
] | [
[
1162,
1175
]
] | [
[
1126,
1161
]
] |
2019MNRAS.482.3288G__Orazio,_Haiman_&_MacFadyen_2013_Instance_1 | The orbital decay of BSBHs may slow down or stall at ∼pc scales (e.g. Begelman et al. 1980; Milosavljević & Merritt 2001; Zier & Biermann 2001; Yu 2002; Vasiliev, Antonini & Merritt 2014; Dvorkin & Barausse 2017; Tamburello et al. 2017), or the barrier may be overcome in gaseous environments (e.g. Gould & Rix 2000; Esc... | [
"D’Orazio, Haiman & MacFadyen 2013"
] | [
"The accretion of gas and the dynamical evolution of BSBHs are likely to be coupled",
"such that the occurrence rate of BSBHs depends on the initial conditions and gaseous environments at earlier phases"
] | [
"Background",
"Background"
] | [
[
1187,
1220
]
] | [
[
908,
990
],
[
1262,
1377
]
] |
2018ApJ...855...26A__Karim_et_al._2013_Instance_1 | The uncertainties in number counts were derived from Poisson statistics, which apply when event rates are calculated from small numbers of observed events (Gehrels 1986). Our results are given in Table 6 and plotted in Figure 7. For comparison, we also show the integral number counts from the lensing cluster surveys of... | [
"Karim et al. 2013"
] | [
"For comparison, we also show the integral number count",
"and from the high-resolution ALMA follow-up of LESS"
] | [
"Uses",
"Uses"
] | [
[
565,
582
]
] | [
[
229,
283
],
[
512,
563
]
] |
2022ApJ...936...16M__Dubrulle_et_al._1995_Instance_1 | Our assumption of a constant f
dg does not account for vertical settling and depletion of dust in the disk atmosphere, which could in principle reduce the height of the different τ = 1 surfaces shown in Figure 6. Even though the Stokes number remains smaller than 1 for all considered particle sizes well above the τ = 1... | [
"Dubrulle et al. 1995"
] | [
"The dust distribution away from the midplane is better captured by hydrodynamical simulations than by simple prescriptions relying on a parameterization of the turbulence strength (see, e.g.,",
"since it depends on the particular source of turbulence."
] | [
"Background",
"Background"
] | [
[
659,
679
]
] | [
[
467,
658
],
[
709,
765
]
] |
2015ApJ...806...20B__Bartoli_et_al._2012a_Instance_1 | The ARGO-YBJ detector, hosted in a building at the YangBaJing Cosmic Ray Observatory (Tibet, China, 90°31′50″E, 30°06′38″N), 4300 m above sea level, has been designed for very high-energy (VHE) gamma-ray astronomy and cosmic-ray observations. It is made up of a single layer of resistive plate chambers (RPCs) operated i... | [
"Bartoli et al. 2012a"
] | [
"These pads provide the digital readout of the detector up to 22 particles m−2, allowing the count of the air shower charged particles without any significant saturation up to primary cosmic-ray energies of about 200 TeV"
] | [
"Background"
] | [
[
1077,
1097
]
] | [
[
856,
1075
]
] |
2021AandA...650A.164M__Davies_et_al._2012_Instance_3 | The GMC associated with G305 is one of the most massive and luminous clouds in the Milky Way (Fig. 1). It is located in the Galactic plane at l ~ 305°, b ~ 0° and at a kinematic distance of 4 kpc (derived from a combinationof radio and Hα observationsby Clark & Porter (2004); Davies et al. (2012) measured its spectroph... | [
"Davies et al. 2012"
] | [
"Analysis of the stellar clusters in the complex reveals them to have ages of 1.5 Myr for Danks 1 and 3 Myr for Danks 2,with the former possibly being triggered by the latter"
] | [
"Background"
] | [
[
2062,
2080
]
] | [
[
1887,
2060
]
] |
2022MNRAS.513.5377F__Fulle_et_al._2020b_Instance_1 | Cometary activity is driven by the gas pressure P(s), which does not depend on the ice abundance, but only on the gas temperature: also minor species can drive cometary activity, provided that heat transfer inside a pebble is faster than ice depletion. This condition fixes an upper limit for the refractory-to-ice mass ... | [
"Fulle et al. 2020b"
] | [
"In order to fulfil equation (2) during the whole inbound orbit, cometary activity is driven by at least the five ices listed in Table 2, reporting the nucleus and gas coma parameters computed by means of the activity model"
] | [
"Uses"
] | [
[
745,
763
]
] | [
[
521,
743
]
] |
2016MNRAS.457.3191D__Martin_et_al._2005_Instance_1 | TYC 9486-927-1 was observed by Torres et al. (2006) as part of the Search for Associations Containing Young stars (SACY) programme (Torres et al. 2008). They assigned a spectral type of M1 and measured a radial velocity of vrad = 8.7 ± 4.6 km s−1 from 10 observations. The large uncertainty is likely due to the star's h... | [
"Martin et al. 2005"
] | [
"using GALEX data from",
"we find log FFUV/FJ = −2.49, log FNUV/FJ = −2.11"
] | [
"Uses",
"Uses"
] | [
[
610,
628
]
] | [
[
588,
609
],
[
629,
677
]
] |
2015AandA...584A.103S__Potekhin_et_al._2013_Instance_2 | Douchin & Haensel (2001; DH) formulated a unified EoS for NS on the basis of the SLy4 Skyrme nuclear effective force (Chabanat et al. 1998), where some parameters of the Skyrme interaction were adjusted to reproduce the Wiringa et al. calculation of neutron matter (Wiringa et al. 1988) above saturation density. Hence, ... | [
"Potekhin et al. 2013"
] | [
"Analytical fits of these neutron-star EoSs have been constructed in order to facilitate their inclusion in astrophysical simulations"
] | [
"Background"
] | [
[
1209,
1229
]
] | [
[
1075,
1207
]
] |
2017AandA...600A.123D__Coupeaud_et_al._(2011)_Instance_1 | Despite the differences of the dust analogues retained in previous studies (Mennella et al. 1998; Boudet et al. 2005; Coupeaud et al. 2011) and in the present one, the spectroscopic properties and temperature dependent behavior of all these analogues remain qualitatively similar: the MAC value is correlated with the du... | [
"Coupeaud et al. (2011)"
] | [
"whereas in",
"and Mennella et al. (1998) and in the present study this correction was not applied"
] | [
"Similarities",
"Similarities"
] | [
[
965,
987
]
] | [
[
954,
964
],
[
988,
1071
]
] |
2020ApJ...905..111Z__Jirička_et_al._2001_Instance_3 | Surveys of radio bursts in decimetric wavelengths is presented in papers by Isliker & Benz (1994) and Jirička et al. (2001), within 1–3 GHz and 0.8–2.0 GHz frequency ranges, respectively. Some of these bursts are still not well understood. This is a case of the slowly positively drifting bursts (SPDBs). They appear in ... | [
"Jirička et al. 2001"
] | [
"The majority of observed SPDBs are connected to solar flares"
] | [
"Background"
] | [
[
677,
696
]
] | [
[
615,
675
]
] |
2020ApJ...896...12X__Rosenberg_&_Coleman_1969_Instance_1 | The QBOs are also found in the local wavelet power spectra of the Bx, By, and Bz that are displayed in the left panel of Figure 2. As this figure shows, the significant regions of above 95% confidence level in the range of 256–512 days (peak at 1.01 yr) for Bx intermittently appear during 1975–2000, and those in the ra... | [
"Rosenberg & Coleman 1969"
] | [
"On the other hand, the annual variation in the IMF polarity in the band of 256–512 days, which is referred to the Rosenberg–Coleman effect",
"The authors indicated that such a result should be attributed to a more stable and flat heliospheric current sheet that only appears in the ascending phase of solar cycles... | [
"Uses",
"Compare/Contrast"
] | [
[
1161,
1185
]
] | [
[
1021,
1159
],
[
1360,
1755
]
] |
2022MNRAS.509..314F__Spitkovsky,_Levin_&_Ushomirsky_2002_Instance_1 | Magnetohydrodynamic (MHD) shallow water equations are an alternative to complete system of MHD equations for plasma. In this approximation, a thin layer of plasma with a free boundary in a gravity field is studied (Gilman 2000). Shallow water flows with rotation are usually considered in case of large-scale flows in pl... | [
"Spitkovsky, Levin & Ushomirsky 2002"
] | [
"Such a model is used to study",
"flows of accreting matter in neutron stars"
] | [
"Background",
"Background"
] | [
[
731,
766
]
] | [
[
430,
459
],
[
656,
698
]
] |
2020ApJ...904..119F__Raaijmakers_et_al._2019_Instance_1 | In this work, the parameter ranges are for 68% credibility interval unless specifically mentioned. With Equation (1), the amount of the post-merger gravitational radiation can be reasonably/qualitatively evaluated as long as
(i.e., the EoS) is known. However, various EoS models have been proposed in the literatu... | [
"Raaijmakers et al. 2019"
] | [
"This can be done either in the EoS parameterizing methods",
"or the nonparametric approach",
"and the results are well consistent with each other."
] | [
"Similarities",
"Similarities",
"Similarities"
] | [
[
1620,
1643
]
] | [
[
1561,
1618
],
[
1664,
1693
],
[
1736,
1788
]
] |
2017MNRAS.470.4075L__Janev_&_Reiter_2004_Instance_1 | In order to determine the unknown rate constant that will be used in the network, we used a methodology developed in previous articles (Loison et al. 2014a,b, 2015) and summarized in Appendix A. This methodology includes an extensive literature review, various Density Functional Theory (DFT) and ab initio calculations ... | [
"Janev & Reiter 2004"
] | [
"Moreover, in DR processes, the H ejection is in general favoured more than H2 ejection"
] | [
"Compare/Contrast"
] | [
[
1481,
1500
]
] | [
[
1366,
1452
]
] |
2016ApJ...831...63X__Bergh_2009_Instance_1 | The formation and evolution of S0 galaxies are very important for understanding the formation and evolution of galaxies, but they are still an open question (e.g., the recent review by D’Onofrio et al. 2015). Currently, there are two possible scenarios on the origin of S0 galaxies. One is that S0 galaxies are transform... | [
"van den Bergh 2009"
] | [
"Currently, there are two possible scenarios on the origin of S0 galaxies.",
"The other is that S0 galaxies are intrinsically different from spiral galaxies since their formation"
] | [
"Background",
"Background"
] | [
[
563,
581
]
] | [
[
209,
282
],
[
414,
514
]
] |
2016MNRAS.456..512C__Kronberg_et_al._2004_Instance_1 | Extended radio emission in galaxies is associated with both radio jets and lobes and with outflows, seen often as aligned radio sources in the opposite directions with respect to the central compact radio core. Giant radio galaxies (GRG) are extreme cases of this phenomenology with jets and lobes extending on ∼ Mpc sca... | [
"Kronberg et al. 2004"
] | [
"In this respect, GRGs have a crucial role in the acceleration of cosmic rays over large cosmic scales (e.g."
] | [
"Motivation"
] | [
[
522,
542
]
] | [
[
414,
521
]
] |
2018ApJ...852..112K__Neronov_&_Aharonian_2007_Instance_1 | The Virgo Cluster radio galaxy M87 (NGC 4486), located at a distance of
Mpc (Mei et al. 2007) and believed to harbour a BH of mass
, was the first extragalactic source detected at VHE energies (Aharonian et al. 2003). Given its proximity, M87 has been a prime target to probe scenarios for the formation of ... | [
"Neronov & Aharonian 2007"
] | [
"Gap-type emission models offer a promising alternative and different realizations have been proposed in the literature (e.g.,"
] | [
"Motivation"
] | [
[
1526,
1550
]
] | [
[
1400,
1525
]
] |
2020MNRAS.494.2969T__Catelan_et_al._2001_Instance_1 | In the tidal torque model used in this work, the alignment of spiral galaxies is purely due to their orientation, which in turn is related to the angular momentum correlation of neighbouring galaxies relative to the line of sight (Croft & Metzler 2000; Crittenden et al. 2001). Angular momentum correlations are mainly b... | [
"Catelan et al. 2001"
] | [
"The correlated angular momenta result into correlated inclination angles of neighbouring galaxies and thus ultimately into correlated ellipticities"
] | [
"Uses"
] | [
[
1419,
1438
]
] | [
[
1270,
1417
]
] |
2020MNRAS.498.6069P__Casertano_&_Hut_1985_Instance_1 | Galaxy colour is known to be sensitive to local density. Generally, sheets are denser than fields and filaments are denser than sheets. So the dependence of red and blue fractions on the geometry of large-scale environment shown in Fig. 5 may partly arise due to dependence of galaxy colour on local density. We need to ... | [
"Casertano & Hut 1985"
] | [
"We address this issue by calculating local number density of galaxies using kth nearest neighbour method"
] | [
"Uses"
] | [
[
537,
557
]
] | [
[
431,
535
]
] |
2020ApJ...898L..56L__Abdo_et_al._2010_Instance_1 | The 3 month γ-ray light curve of 4FGL J1510.1+5702 reveals that it is at a high flux state in an epoch of several tens of days in 2018; meanwhile, optical flux densities of GB 1508+5714 in two bands rise in the same epoch. To further investigate the relationship between these two domains of emissions, a 3 day time bin ... | [
"Abdo et al. 2010"
] | [
"It is supported by correlated optical/γ-ray flares in FSRQs (e.g.,"
] | [
"Similarities"
] | [
[
1508,
1524
]
] | [
[
1441,
1507
]
] |
2022MNRAS.510.3039K__Gunell_et_al._2018_Instance_1 | Finally, our models assume the absence of planetary magnetic fields. The early paradigm considering the evolution of terrestrial planets has implied that the planetary magnetic field is necessary to protect planetary atmospheres and reduce the atmospheric mass loss (see e.g. Dehant et al. 2007, and references therein).... | [
"Gunell et al. 2018"
] | [
"Thus, for planets in the Solar System, it was shown both in the observations",
"that the presence of a weak magnetic field can intensify atmospheric escape."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
960,
978
]
] | [
[
882,
958
],
[
1060,
1136
]
] |
2018ApJ...857...98R__Ferraz-Mello_et_al._2008_Instance_1 | Numerous investigations of tidal activity on extrasolar planets have been conducted, with a range of topics from the behavior of gas giants (e.g., Běhounková et al. 2010, 2011; Remus et al. 2012a, 2012b; Storch & Lai 2014), to tidal alterations of system dynamics (e.g., Lecoanet et al. 2009; Matsumura et al. 2010; Cébr... | [
"Ferraz-Mello et al. 2008"
] | [
"Numerous investigations of tidal activity on extrasolar planets have been conducted, with a range of topics",
"issues of spin dynamics"
] | [
"Background",
"Background"
] | [
[
566,
590
]
] | [
[
0,
107
],
[
520,
543
]
] |
2019ApJ...874L..32C__Ogle_et_al._1997_Instance_1 | Cygnus A, at z = 0.0562, is 10 times closer than the next radio galaxy of similar radio luminosity.4
4
Radio luminosity >1045 erg s−1.
The nuclear regions in Cygnus A have been observed extensively at radio through X-ray wavelengths (Carilli & Barthel 1996). The inner few arcseconds is a complex mix of optically obsc... | [
"Ogle et al. 1997"
] | [
"The inner few arcseconds is a complex mix of",
"polarized, broad optical emission lines due to scattering by dust"
] | [
"Background",
"Background"
] | [
[
779,
795
]
] | [
[
261,
305
],
[
689,
754
]
] |
2016ApJ...833...76B__Klimchuk_et_al._2008_Instance_1 | A significant limitation of the model is that it ignores the well-established hydrodynamic evolution of the loop during the cooling process, involving the substantial transfer of mass between the chromosphere and the corona. For large downward heat fluxes, the transition region is unable to radiate the supplied energy,... | [
"Klimchuk et al. 2008"
] | [
"It has been suggested",
"that the enthalpy fluxes associated with both evaporating and condensing plasma are at all times in approximate balance with the excess or deficit of the heat flux relative to the transition region radiation loss rate."
] | [
"Background",
"Background"
] | [
[
796,
816
]
] | [
[
773,
794
],
[
818,
1036
]
] |
2018MNRAS.474..838D__and_2016_Instance_1 | The first step in searching for dynamically correlated minor bodies, particularly those resulting from break-ups, is to get a clear characterization of what the expectations may be. The outcome of cometary disruption is well documented through two well-studied examples, those of the comets 73P/Schwassmann-Wachmann 3 an... | [
"Kadota et al. 2017"
] | [
"Some of these fragments have been recovered",
"and 2016–2017"
] | [
"Background",
"Background"
] | [
[
718,
736
]
] | [
[
595,
638
],
[
698,
711
]
] |
2021ApJ...912..163B__Brennecka_et_al._2020_Instance_2 | Braukmuller et al. (2018) proposed that all elements fall into one of four categories based on their condensation temperature: refractory elements (50% condensation temperature, Tc,50 > 1400 K), which exhibit approximately uniform enrichments in their Si-normalized concentrations in CC chondrites compared to CI chondri... | [
"Brennecka et al. 2020"
] | [
"For the purposes of this study, we adopt the composition of type I CAIs as the representative value of refractory objects because they are seemingly the most abundant type and lack the characteristic elemental depletions of other CAI groups (e.g.,"
] | [
"Uses"
] | [
[
3452,
3473
]
] | [
[
3183,
3430
]
] |
2019AandA...627A..53H__Villar-Martín_et_al._1999_Instance_1 | A spatial coincidence of the radio jet morphology and velocity dispersion of the ionised gas has already been reported for spatially-resolved spectroscopy of more luminous radio-quiet AGN (e.g. Husemann et al. 2013; Villar-Martín et al. 2017) and powerful compact radio sources (e.g. Roche et al. 2016), but it has been ... | [
"Villar-Martín et al. 1999"
] | [
"Hence, we think that the radio jet is transferring its energy and momentum to the ambient medium through an extended shock front, which creates turbulence in a dense clumpy ISM. Such a great impact of the radio jet has been observationally shown in many cases (e.g."
] | [
"Similarities"
] | [
[
969,
994
]
] | [
[
703,
968
]
] |
2018ApJ...854...73I__Bowler_et_al._2014_Instance_1 | The best-fit parameters are shown in Table 3. We find that the uncertainties in M* and
are considerably large due to a degeneracy between the two parameters when all parameters are variable. Plotted in Figure 1 is the faint-end slope α as a function of redshift. Our results indicate that the best-fit values of α... | [
"Bowler et al. 2014"
] | [
"We also plot the results of previous blank-field surveys"
] | [
"Uses"
] | [
[
856,
874
]
] | [
[
697,
753
]
] |
2019MNRAS.484..712D__Moriarty_et_al._2014_Instance_1 | The Gibbs free energy of the system, and thus the composition of the solids formed depends on the pressure and temperature at which condensation occurs. In order to consider reasonable pressures and temperatures for the inner regions of the PPD, and in order to convert these temperatures and pressures into radial locat... | [
"Moriarty et al. 2014"
] | [
"This model has been previously used for the modelling of planetesimal formation in PPDs"
] | [
"Background"
] | [
[
641,
661
]
] | [
[
552,
639
]
] |
2017MNRAS.469S..39F__Johansen_et_al._2015_Instance_1 | This conclusion can be quantified by the number of catastrophic collisions per comet (Rickman et al. 2015)
(6)
\begin{equation}
N_{{\rm coll}} = N_{\rm p} A_{\rm p} u T / V,
\end{equation}
where Np is the number of comets in the disc, Ap and u are the collision cross-section and speed, respectively, T ≈ 0.4 Gyr is ... | [
"Johansen et al. 2015"
] | [
"The size distribution is probably shallower"
] | [
"Compare/Contrast"
] | [
[
666,
686
]
] | [
[
621,
664
]
] |
2021MNRAS.503.1734I__McKinney_et_al._2019_Instance_1 | We show in Fig. 6 the dependence of some Ly α characteristics on absolute FUV magnitude. Our galaxies with detected LyC emission are shown by red filled circles and those with upper limits of LyC emission are represented by red open circles. All our low-mass galaxies are characterized by moderate Ly α luminosities in a... | [
"McKinney et al. 2019"
] | [
"All our low-mass galaxies are characterized by moderate Ly α luminosities in a narrow range between 1042.19 and 1042.74 erg s−1 (Fig. 6a), that are slightly below the values for confirmed LyC leakers (blue filled circles) by Izotov et al. (2016a,b, 2018a,b) and high-redshift galaxies (grey open circles) by Ouchi e... | [
"Compare/Contrast"
] | [
[
836,
856
]
] | [
[
242,
758
]
] |
2018MNRAS.476.2421G__Gallego_et_al._2018_Instance_1 | An alternative approach is to map the CGM through direct imaging of the Ly α line. Theoretical models suggest that three main mechanisms should be able to generate circumgalactic Ly α emission: cooling radiation of gravitationally heated gas (e.g. Haiman, Spaans & Quataert 2000; Yang et al. 2006; Dijkstra & Loeb 2009),... | [
"Gallego et al. 2018"
] | [
"While the fluorescent signal powered by the diffuse metagalactic UV background",
"with an expected surface brightness (SB) of $\\rm SB_{Ly\\alpha }\\sim 10^{-20} \\,erg \\,s^{-1} \\,cm^{-2} \\,arcsec^{-2}$",
"is still out of reach for current optical instrumentation (but see",
"Ly α fluorescence is predicted... | [
"Background",
"Background",
"Background",
"Background"
] | [
[
1009,
1028
]
] | [
[
613,
691
],
[
781,
897
],
[
942,
1008
],
[
1031,
1169
]
] |
2022ApJ...927..149L__Cicone_et_al._2017_Instance_1 | These trends make physical sense and agree with the limited previous measurements. Physically, elevated SFR/M
⋆ may trace more intense radiation fields and stronger heating of the gas, suggesting higher temperatures. The anticorrelation with M
⋆ may reflect the impact of dust shielding. Based on the existence of the ma... | [
"Cicone et al. 2017"
] | [
"In literature studies, CO line ratios do appear enhanced in low-metallicity regions or galaxies (e.g.,"
] | [
"Background"
] | [
[
772,
790
]
] | [
[
587,
689
]
] |
2022MNRAS.512.4280P__Umetsu_et_al._2016_Instance_1 | 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"
] | [
"The NFW profile has been shown to provide an overall good agreement with observations and simulations over a broad range of scales in GR"
] | [
"Similarities"
] | [
[
2078,
2096
]
] | [
[
1914,
2050
]
] |
2018AandA...615A..77L__XIII_2016_Instance_1 | The last decade and a half has seen a revolution in the study of overdensities in the early Universe. While the study and careful characterization of large associations of galaxies in the local Universe has been possible for nearly a century, and in the intermediate redshift Universe for a significant fraction of that ... | [
"Planck Collaboration XIII 2016"
] | [
"While some phenomena exist in the early Universe, such as quasars or radio galaxies, which are so powerful and intrinsically bright that they have been able to serve as beacons to early searches near the epoch of H I reionization (z ~ 5.5–10,",
"the bulk of the galaxy population residing in the early Universe do... | [
"Background",
"Background"
] | [
[
985,
1015
]
] | [
[
716,
958
],
[
1018,
1114
]
] |
2019MNRAS.489..855C__Husemann_et_al._2013_Instance_2 | 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"
] | [
"Common definitions include",
"or the $\\rm [O\\, III]$ flux weighted radius"
] | [
"Uses",
"Uses"
] | [
[
1315,
1335
]
] | [
[
1148,
1174
],
[
1270,
1313
]
] |
2019ApJ...871...58T__Charbonnel_&_Lagarde_2010_Instance_1 | We derived stellar parameters, [C/M], and [N/M] using SLAM. To avoid bad fits at the edges of the parameter space, we exclude stars with spectral S/N in the g band less than 50, and metallicity less than −1.4. The derived C and N abundances are shown in Figure 8. Clearly, in the top panel, the CH-strong, CH-normal, and... | [
"Charbonnel & Lagarde 2010"
] | [
"As evolved stars ascend the RGB, C and N abundances may be changed by first dredge-up",
"and extra mixing"
] | [
"Background",
"Background"
] | [
[
710,
735
]
] | [
[
567,
652
],
[
671,
687
]
] |
2021AandA...655A..99D__Hernández_et_al._2010_Instance_1 | The giant planet metallicity correlation supports the core-accretion scenario for the formation of planets (Pollack et al. 1996; Ida & Lin 2004; Mordasini et al. 2009), in which it is assumed that planetesimals are formed by the condensation of heavy elements. The discovery of this correlation has led to an increased i... | [
"González Hernández et al. 2010"
] | [
"The discovery of this correlation has led to an increased interest on the abundances of other elements in planet hosts(e.g."
] | [
"Motivation"
] | [
[
605,
635
]
] | [
[
261,
384
]
] |
2022MNRAS.509.1959S__Nordlander_et_al._2019_Instance_1 | However, the transition between the two extremes of modern (metal-rich) and primordial (metal-poor) star formation, and in particular the role of dust coupling and stellar radiation feedback at low metallicity, has thus far received limited exploration. Krumholz (2011) present analytical models for radiation feedback a... | [
"Nordlander et al. 2019"
] | [
"However, these studies do not explore lower metallicities, despite available evidence for the existence of a low-metallicity ISM in the past through the discovery of stars",
"as well as several others with $\\rm {[Fe/H]} \\lt -5$"
] | [
"Motivation",
"Motivation"
] | [
[
1046,
1068
]
] | [
[
602,
773
],
[
879,
931
]
] |
2022ApJ...939..117Z__Blandford_et_al._2019_Instance_1 | Blazars are a subclass of active galactic nuclei (AGNs) with relativistic jets of high-energy particles pointing near our line of sight (e.g., Urry & Padovani 1995). Their nonthermal emission is generally detected across the entire electromagnetic spectrum from radio to γ-ray bands. Blazars are subclassified into flat-... | [
"Blandford et al. 2019"
] | [
"while BL Lacs are powered by an advection-dominated, low radiative efficiency accretion flow"
] | [
"Background"
] | [
[
894,
915
]
] | [
[
777,
869
]
] |
2022AandA...659L...1L__Lellouch_et_al._2013_Instance_2 | Without knowledge of nucleus shape and spin parameters (pole orientation and shape), a thermophysical model is pointless, and we instead adopted a NEATM (Near Earth Asteroid Thermal Model) model, used extensively for asteroids (Harris 1998) and TNOs (Müller et al. 2020, and references therein). NEATM is based on the as... | [
"Lellouch et al. 2013"
] | [
"Given the rh = 20 au distance of our measurements (and the expected large size of 2014 UN271), we adopted a beaming factor η = 1.175 ± 0.42, based on measurements of 85 Centaurs and TNOs"
] | [
"Uses"
] | [
[
1003,
1023
]
] | [
[
815,
1001
]
] |
2020MNRAS.492.4727C__Rees_1976_Instance_1 | A strong property of the isothermal gas that defines the interstellar medium (ISM) is the absence of a characteristic mass scale owing to the scale-free nature of gravity. From the collapse condition of an isothermal sphere, one can derive the Jeans mass as
(2)$$\begin{eqnarray*}
M_{\mathrm{J}} = \frac{4 \pi}{3} \rho ... | [
"Rees 1976"
] | [
"At very large densities, though, owing to the increased dust absorption coefficient, the gas becomes opaque to its own radiation. This is sometimes referred to as the opacity limit",
"At this point, the fragmentation is halted, setting a scale below which no fragments form."
] | [
"Background",
"Background"
] | [
[
1135,
1144
]
] | [
[
929,
1109
],
[
1147,
1237
]
] |
2016AandA...591A..13V__Giovannini_et_al._2013_Instance_1 | The first direct proof of the existence of magnetic fields in large-scale extragalactic environments, i.e., galaxy clusters, dates back to the 1970s with the discovery of extended, diffuse, central synchrotron sources called radio halos (see, e.g., Feretti et al. 2012 for a review). Later, indirect evidence of the exis... | [
"Giovannini et al. 2013"
] | [
"On scales up to a few Mpc from the nearest galaxy cluster, possibly along filaments, only a few diffuse synchrotron sources have been reported"
] | [
"Background"
] | [
[
866,
888
]
] | [
[
660,
802
]
] |
2021ApJ...915L...8D__Chen_et_al._2020_Instance_1 | Magnetic field fluctuations in the solar wind are highly turbulent. The measured power spectral density (PSD) of the fluctuating magnetic field always exhibits power laws k−α, where k is the wavenumber, and α is the spectral index. A single spacecraft measures the PSD as a function of f−α in the frequency domain, which... | [
"Chen et al. 2020"
] | [
"The inertial range, which is dominated by magnetohydrodynamic (MHD) turbulence, follows the cascade models with spectral indices αi from around 3/2 to 5/3"
] | [
"Background"
] | [
[
726,
742
]
] | [
[
548,
702
]
] |
2015ApJ...811L..32H__Liewer_et_al._2001_Instance_1 | In this Letter, we directly test the relationship between proton kinetic instabilities and plasma turbulence in the solar wind using a hybrid expanding box model that allows us to study self-consistently physical processes at ion scales. In the hybrid expanding box model, a constant solar wind radial velocity vsw is as... | [
"Liewer et al. 2001"
] | [
"The expanding box uses these comoving coordinates, approximating the spherical coordinates by the Cartesian ones"
] | [
"Uses"
] | [
[
728,
746
]
] | [
[
614,
726
]
] |
2021AandA...654A.132B__Davies_et_al._2014b_Instance_1 | We can use the equivalent width of Hα (EWHα, see Table 4) to put additional constraints on the recent star formation history of the AGNs. To do so, we first need to estimate the largest fraction of the Hα luminosity that could arise from star formation, and for this we use the group of AGNs with the highest EWHα. There... | [
"Davies et al. 2014b"
] | [
"To assess the star formation contribution to the Hα flux, we consider lines from the most extreme AGN photoionisation models of Groves et al. (2004), to the location of solar metallicity star-forming galaxies (see also"
] | [
"Uses"
] | [
[
978,
997
]
] | [
[
759,
977
]
] |
2022AandA...662A...8M__Shu_et_al._1987_Instance_1 | Even before studying the relationship between the IMF and the CMF, it is important to realize that how the IMF originates from the observed CMF depends directly on the definition of the cores, assumed to be the gas mass reservoir used for the formation of each star or binary system. As shown by Louvet et al. (2021), de... | [
"Shu et al. 1987"
] | [
"In addition, the theoretical definition of cores also depends on whether the star-formation scenario is quasi-static or dynamic. In the former scenario, cores are gas condensations sufficiently dense to be on the verge of gravitational collapse, and they convert the core gas into stars"
] | [
"Background"
] | [
[
787,
802
]
] | [
[
499,
785
]
] |
2021AandA...654A.126B__Hotta_(2017)_Instance_1 | Analytical and semianalytical approaches have been developed to describe this process and estimate the width of the overshooting layer (e.g., Schmitt et al. 1984; Zahn 1991; Rempel 2004). With the improvement of computational methods and resources, an increasing number of studies have been devoted to numerical simulati... | [
"Hotta (2017)",
"Hotta 2017",
"Hotta (2017)"
] | [
"A commonly used tactic to increase the efficiency and improve the stability of these simulations is to artificially increase the luminosity (or nuclear energy for convective cores or burning shells) and to modify the thermal diffusivity of the reference stellar model. This tactic is common and has been used, for e... | [
"Background",
"Background"
] | [
[
895,
907
],
[
1763,
1773
],
[
2039,
2051
]
] | [
[
471,
796
],
[
978,
1381
]
] |
2019ApJ...882...97P__Warmuth_&_Mann_2016_Instance_1 | The RADYN code (Carlsson & Stein 1992, 1995, 1997; Allred et al. 2015) is a one-dimensional radiative hydrodynamic code that can be used to study the interaction of particle beams with the solar atmosphere. It uses the Fokker–Planck formalism (McTiernan & Petrosian 1990), which takes into account the beam energy losses... | [
"Warmuth & Mann 2016"
] | [
"The beam fluxes used had values of 3 × 109, 1 × 1010, and 3 × 1010 erg cm−2 s−1, while the low-energy cutoff EC covered the parameter space where flare values are usually found (20–120 keV;"
] | [
"Uses"
] | [
[
874,
893
]
] | [
[
684,
873
]
] |
2017ApJ...835..101H__Vanderbeke_et_al._2014_Instance_1 | In the present survey of GCSs in BCGs, we use the color index
(from here on we drop the accents on the SDSS indices). In the following discussion it will be useful to have a calibration of this index versus cluster metallicity [Fe/H]. To do this, we would ideally need to have GC photometry of the same clusters i... | [
"Vanderbeke et al. 2014"
] | [
"Galaxies satisfying all three of these criteria are rare; in principle the Milky Way GC databases could be used, but cluster-to-cluster foreground reddenings differ strongly, the published SDSS indices",
"show considerable scatter versus metallicity, and the variety of studies from which the UBVRI indices were d... | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
688,
710
]
] | [
[
485,
686
],
[
712,
923
]
] |
2020ApJ...904...81G__Nariyuki_&_Hada_2007_Instance_1 | Alfvén waves of arbitrary amplitude with constant total pressure are known to provide an exact solution to the compressible magnetohydrodynamic (MHD) system in a homogeneous plasma, in that nonlinearities are turned off and there no couplings with compressible modes. However, such a dynamical system is linearly unstabl... | [
"Nariyuki & Hada 2007"
] | [
"However, such a dynamical system is linearly unstable to parametric instabilities and large-amplitude Alfvén waves are known to decay into compressible and secondary Alfvénic modes through three- or four-wave resonances that lead to a variety of parametric instabilities, depending on the plasma beta and dispersive... | [
"Background"
] | [
[
777,
797
]
] | [
[
268,
629
]
] |
2020MNRAS.498.1801K__Gundlach_et_al._2011_Instance_1 | Water ice is ubiquitous in the cold regions of the Universe, owing to the fact that hydrogen and oxygen are the two most abundant elements to form a solid such as icy dust particles and comets. It is, therefore, commonly accepted that the essential component of dust particles and planetesimals in protoplanetary discs i... | [
"Gundlach et al. 2011"
] | [
"Recent works on laboratory measurements of cohesion between crystalline water-ice particles at vacuum conditions provided encouraging results that dust particles composed of water ice might be much more cohesive than previously believed"
] | [
"Background"
] | [
[
1296,
1316
]
] | [
[
1058,
1294
]
] |
2016MNRAS.463.3204R__Trautman_1967_Instance_1 | Since the perturbation in equation (22) is not conservative, we shall focus on the extension of Noether's theorem to non-conservative systems by Djukic & Vujanovic (1975). It must be $F_i-q^\prime _if\ne 0$ for the conservation law to hold (Vujanovic, Strauss & Jones 1986). For the case of non-conservative systems the ... | [
"Trautman 1967"
] | [
"This equation and the condition $F_i-q^\\prime _if\\ne 0$ furnish the generalized NBH equations"
] | [
"Uses"
] | [
[
938,
951
]
] | [
[
843,
936
]
] |
2017MNRAS.469.2662D__Morales_et_al._2012_Instance_1 | A well-studied way to look at antenna spectral requirements is from the perspective of foreground avoidance in power spectrum space. In the avoidance scheme, smooth-spectrum foregrounds should, in the ideal case, occupy a wedge–shaped region of the two–dimensional power spectrum space (where the wavenumber k can be dec... | [
"Morales et al. 2012"
] | [
"In the avoidance scheme, smooth-spectrum foregrounds should, in the ideal case, occupy a wedge–shaped region of the two–dimensional power spectrum space (where the wavenumber k can be decomposed into k⊥ and $k_\\Vert$ that are the transverse and line-of-sight wave numbers, respectively) whereas the remaining area ... | [
"Background"
] | [
[
542,
561
]
] | [
[
133,
510
]
] |
2019ApJ...875...90L__Velli_et_al._2015_Instance_3 | 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... | [
"Velli et al. 2015"
] | [
"Maybe we do not need to intentionally take to heart such the classical dichotomy, because waves and reconnections may interact with each other"
] | [
"Motivation"
] | [
[
2208,
2225
]
] | [
[
2036,
2178
]
] |
2015MNRAS.452.2731S__Stroe_et_al._2013_Instance_1 | The H α studies of Umeda et al. (2004) and Stroe et al. (2014a, 2015) are tracing instantaneous (averaged over 10 Myr) SF and little is known about SF on longer time-scales and the reservoir of gas that would enable future SF. An excellent test case for studying the gas content of galaxies within merging clusters with ... | [
"Stroe et al. 2013"
] | [
"The cluster merger induced relatively strong shocks, which travelled through the ICM, accelerated particles to produce relics towards the north and south of the cluster"
] | [
"Background"
] | [
[
1251,
1268
]
] | [
[
1057,
1225
]
] |
2020AandA...644A..97C__Leroy_et_al._2013_Instance_2 | Major nearby galaxy cold gas mapping surveys (Regan et al. 2001; Wilson et al. 2009; Rahman et al. 2011; Leroy et al. 2009; Donovan Meyer et al. 2013; Bolatto et al. 2017; Sorai et al. 2019; Sun et al. 2018) have focused on observations of the molecular gas (through CO lines). Despite a few notable exceptions (e.g. Ala... | [
"Leroy et al. 2013"
] | [
"On kpc scales and in the discs of nearby star-forming galaxies, τdep is approximately constant around 1–2 Gyr"
] | [
"Background"
] | [
[
1327,
1344
]
] | [
[
1176,
1285
]
] |
2022ApJ...930...70H__Vogl_et_al._2020_Instance_1 | There are some existing studies applying machine learning to transient studies. For example, the spectral types of the SNe can be classified based on their light-curve data (Möller et al. 2016; Muthukrishna et al. 2019a; Takahashi et al. 2020; Villar et al. 2020), and transients can be identified from the astronomical ... | [
"Vogl et al. 2020"
] | [
"Several other works",
"applied a Gaussian process, principal component analysis (PCA), and deep learning neural networks to radiative transfer models of SNe."
] | [
"Background",
"Background"
] | [
[
965,
981
]
] | [
[
926,
945
],
[
1007,
1141
]
] |
2021AandA...650A.203G__Chiosi_1980_Instance_1 | In the past, as well as in the more recent literature, there have been many attempts to explain the different chemical evolutionary paths of different MW components, particular those of the thin and thick discs. The outcome of these studies is that the observed different chemical evolutionary paths are related to diffe... | [
"Chiosi 1980"
] | [
"A good agreement between observations and theoretical predictions for the Galaxy is obtained by models that are based on the assumption that the disc formed via the infalling of gas"
] | [
"Background"
] | [
[
1045,
1056
]
] | [
[
862,
1043
]
] |
2022AandA...659A..54E__Kendall_et_al._1992_Instance_1 | Exploration of the stationary points of the [H, P, S, O] molecular system was initially carried out using Møller–Plesset second order Perturbation Theory (MP2) (Møller & Plesset 1934; Frisch et al. 1990a,b; Head-Gordon & Head-Gordon 1994; Head-Gordon et al. 1988; Sæbø & Almlöf 1989) with the 6-311++G(d, p) basis set (M... | [
"Kendall et al. 1992"
] | [
"Following this, higher level calculations on the electronic structure, rotational constants, and harmonic vibrational frequencies of each isomer were performed using CCSD(T) together with the Dunning basis sets aug-cc-pV(X+d)Z (X = T, Q, 5)"
] | [
"Uses"
] | [
[
1271,
1290
]
] | [
[
994,
1234
]
] |
2019MNRAS.484.1359Y__Melrose_&_Yuen_2014_Instance_1 | The discrete change in spin-down rate between the on and off states suggests a switching behaviour in the pulsar magnetosphere. While explanation for the phenomenon remains inconclusive, conventional treatments typically involve referring each emission state to different condition in the magnetosphere in such a way tha... | [
"Melrose & Yuen 2014"
] | [
"Our investigation is based on a magnetospheric model that synthesizes the corotating magnetosphere model and the vacuum model",
", in which multiple quasi-stable magnetospheric states are described by the parameter y such that the charge filling fraction of a state corresponds to a y value and a change in the ch... | [
"Uses",
"Uses"
] | [
[
1489,
1508
]
] | [
[
1362,
1487
],
[
1515,
1790
]
] |
2018MNRAS.474.2277D__Oliveira,_Dottori_&_Bica_1998_Instance_2 | There are three possible explanations for the origin of these systems: (1) they formed from the fragmentation of the same molecular cloud (Elmegreen & Elmegreen 1983), (2) they were generated in distinct molecular clouds and then became bound systems after a close encounter leading to a tidal capture (Vallenari, Betton... | [
"de Oliveira, Dottori & Bica 1998"
] | [
"In some cases, the stellar system resulting from the merger event may show significant internal rotation (in fact, for many years this has been the preferred dynamical route to form rotating star clusters; see"
] | [
"Background"
] | [
[
1591,
1623
]
] | [
[
1290,
1499
]
] |
2016ApJ...817...12P__Chamandy_et_al._2014_Instance_1 | Large-scale magnetic fields with strength of the order of 1–10 μG have been observed in disk galaxies (e.g., Beck et al. 1996; Fletcher 2010; Beck 2012; Beck & Wielebinski 2013; Van Eck et al. 2015). The origin of these fields can be explained through mean-field dynamo theory (Ruzmaikin et al. 1988; Beck et al. 1996; B... | [
"Chamandy et al. 2014"
] | [
"Mechanisms suggested to produce these small-scale magnetic helicity fluxes are: advection of magnetic fields by an outflow from the disk through the galactic fountain or wind"
] | [
"Background"
] | [
[
1184,
1204
]
] | [
[
969,
1143
]
] |
2021ApJ...921...18K__Kushwaha_et_al._2018a_Instance_3 | 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"
] | [
"For example, in Mrk 501 the shift in both peaks strongly implies the same particle distribution for the overall emission, while for OJ 287 the shift of only the high-energy peak can be reproduced by either inverse Compton scattering of the broad-line region photon field"
] | [
"Compare/Contrast"
] | [
[
1883,
1904
]
] | [
[
1611,
1881
]
] |
2018MNRAS.478.2541F__Smith_&_Tombleson_2015_Instance_2 | Utilizing the full range of peak absolute magnitudes observed in LBV stars [M ≃ (−13)–(−9) mag; e.g. Smith et al. 2011b] provides a range of peak apparent magnitudes of m ≃ 16.5–20.5 mag, for a distance of D ≃ 8 Mpc (Table 1). Hence, if the transient source (m ≈ 21.0 mag; Section 2.1.2) is an LBV star, it must have b... | [
"Smith & Tombleson 2015"
] | [
"Secondly, although a fraction of LBV stars are isolated (e.g."
] | [
"Compare/Contrast"
] | [
[
1303,
1325
]
] | [
[
1241,
1302
]
] |
2018AandA...619A..13V__Saviane_et_al._2012_Instance_4 | The EWs were measured with the methods described in Vásquez et al. (2015). As in Paper I, we used the sum of the EWs of the two strongest CaT lines (λ8542, λ8662) as a metallicity estimator, following the Ca II triplet method of Armandroff & Da Costa (1991). Different functions have been tested in the literature to mea... | [
"Saviane et al. (2012)"
] | [
"For internal consistency, all EWs in this work have been adjusted to the measurement scale of",
"by using this relation."
] | [
"Uses",
"Uses"
] | [
[
2136,
2157
]
] | [
[
2042,
2135
],
[
2158,
2181
]
] |
2020ApJ...895...82V__Fryer_et_al._2018_Instance_1 | The shock is then revived by adding an energy injection following the parameterized method of Fryer et al. (2018). In this model, roughly
was deposited into the inner
in the first
. Some of this energy is lost through neutrino emission and the total explosion energy at late times for this model is
... | [
"Fryer et al. (2018)"
] | [
"The shock is then revived by adding an energy injection following the parameterized method of"
] | [
"Uses"
] | [
[
94,
113
]
] | [
[
0,
93
]
] |
2017ApJ...844...14L__Martell_et_al._2008_Instance_1 | Figure 2 shows the measured spectral indices of stars as functions of K magnitude, obtained from the 2MASS catalog. The CN, HK′, and CH indices increase with decreasing magnitude because the brighter RGB stars have lower temperatures and the strengths of these molecular bands generally increase with decreasing temperat... | [
"Martell et al. 2008"
] | [
"In particular, the CN index distribution shows the largest spread. Note that a bimodality or a large spread in CN distribution is generally observed in most GCs"
] | [
"Similarities"
] | [
[
918,
937
]
] | [
[
662,
822
]
] |
2019MNRAS.487..475C__Ward-Thompson_et_al._2009_Instance_1 | We attempted to find a correlation between the mean magnetic field and the outflow and minor axis of the cloud CB 17. Relative orientations between various quantities of CB 17 are presented in the first row of Table 6, along with a comparative study of the same for some dark clouds. The first column gives the cloud ID ... | [
"Ward-Thompson et al. 2009"
] | [
"A similar feature has also been observed",
"CB 3 and CB 246"
] | [
"Similarities",
"Similarities"
] | [
[
1097,
1122
]
] | [
[
937,
977
],
[
1080,
1095
]
] |
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