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 |
|---|---|---|---|---|---|---|
2022MNRAS.510.5302I__Fields_et_al._2014_Instance_1 | Lithium is the only metal element produced during the Big Bang nucleosynthesis (BBN) due to the lack of stable nuclei with mass number eight (Fields, Molaro & Sarkar 2014). The element abundances predicted by the standard BBN theory for the baryonic density coming from the Planck mission agree well with those observed,... | [
"Fields et al. 2014"
] | [
"This problem is also known as the Cosmological Lithium problem"
] | [
"Background"
] | [
[
984,
1002
]
] | [
[
920,
982
]
] |
2016ApJ...824...92H__Douglas_&_Ballai_2007_Instance_1 | A couple of years after the closure of the solar flare myth debate, Dere et al. (1997) and Thompson et al. (1998) reported on the presence of wavefronts observed on the solar disk that propagated away from the site of the flare. They were originally termed “EIT waves” (Thompson et al. 1999) after the instrument that fi... | [
"Douglas & Ballai 2007"
] | [
"Over that time they have been assigned different terms, such as",
"coronal waves (e.g.,"
] | [
"Background",
"Background"
] | [
[
708,
729
]
] | [
[
481,
544
],
[
687,
707
]
] |
2015ApJ...815..129S__Shen_et_al._2011_Instance_1 | The mass accretion onto the black hole is important for a better understanding of AGN evolution. The Eddington ratio, the ratio between the AGN bolometric luminosity and the Eddington luminosity (Lbol/LEdd), provides insight into the black hole growth because the bolometric luminosity reflects the mass accretion rate. ... | [
"Shen et al. 2011"
] | [
"For comparison, we show published observations in the same redshift range from the literature in the right panel of Figure 5"
] | [
"Uses"
] | [
[
1003,
1019
]
] | [
[
833,
957
]
] |
2018AandA...615A.148D__Weidner_et_al._(2010)_Instance_3 | The last column in Table 1 reports the number of OB stars minus the “diffuse” population estimated from their density in the Reference field (22.5 stars per square degree): as is immediately seen, the M-star statistics is much larger than the OB star statistics. This can hardly be considered surprising, if an ordinary ... | [
"Weidner et al. (2010)"
] | [
"We estimated using the",
"IMF the expected range for the observed M/OB number ratio."
] | [
"Uses",
"Uses"
] | [
[
2409,
2430
]
] | [
[
2386,
2408
],
[
2431,
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]
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2021MNRAS.503..815V__Schmalzing,_Buchert_&_Kerscher_1995_Instance_1 | Level crossing statistics is a pioneering approach for characterizing stochastic processes introduced by S. O. Rice (Rice 1944, 1945). Up-, down-, and conditional crossing statistics are modifications to the primary definition of level crossing (Bardeen et al. 1986; Bond & Efstathiou 1987; Ryden 1988; Ryden et al. 1989... | [
"Schmalzing, Buchert & Kerscher 1995"
] | [
"Minkowski functionals, which are also closely related to the crossing statistics",
"and have been utilized for cosmological random fields"
] | [
"Background",
"Background"
] | [
[
692,
727
]
] | [
[
440,
520
],
[
607,
660
]
] |
2017AandA...602A..75R__Kaneko_&_Yokoyama_(2015)_Instance_2 | We can see how this is consistent with the development of small scales via phase mixing by introducing local wavenumbers for the variation with α and β, (3)\begin{eqnarray} \xi \propto \exp {\rm i}\left[ \int \kappa_\alpha {\rm d}\alpha + \int \kappa_\beta {\rm d}\beta \right]\!. \label{number3} \end{eqnarray}ξ∝expi∫κα... | [
"Kaneko & Yokoyama (2015)"
] | [
"This phase motion has been seen in magnetospheric data of Alfvén waves",
"and the simulations of coronal oscillations by",
"These studies note that the direction of motion is related to the spatial variation of ωc."
] | [
"Uses",
"Uses",
"Uses"
] | [
[
3614,
3638
]
] | [
[
3457,
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[
3567,
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[
3640,
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2021AandA...646A.142R__Nelson_&_Melrose_1985_Instance_1 | CME-driven shocks accelerate not just protons, but also the electrons in the solar corona (Holman & Pesses 1983; Schlickeiser 1984; Kirk 1994; Mann et al. 1995, 2001; Mann & Klassen 2005). These accelerated electron beams can be observed as type II bursts in the solar radio radiation in the metric wave range (Wild & Mc... | [
"Nelson & Melrose 1985"
] | [
"Energetic electrons are unstable to Langmuir waves, thus they are converted into radio emission at the local plasma frequency and its harmonic (see"
] | [
"Background"
] | [
[
792,
813
]
] | [
[
644,
791
]
] |
2019AandA...626A..49P__Springel_et_al._(2005)_Instance_1 | To provide enough galaxies to adequately train a neural network, EAGLE galaxies from the simulation snapshots with a redshift of less than 1.0 were used. Objects with M⋆ greater than 1010 M⊙ were selected while the merging partner of the merging systems must be larger than 109 M⊙. The merging partner must also be more ... | [
"Springel et al. (2005)"
] | [
"have shown that the effects of a merger are visible for approximately 0.25 Gyr after the merger event while the pre-merger stage is much longer. However, we chose to have the pre and post merger period approximately equal as tests conducted with longer pre-merger times showed no improvement, see discussion in Sect... | [
"Compare/Contrast"
] | [
[
1068,
1090
]
] | [
[
1091,
1412
]
] |
2017MNRAS.469.4620B___2017_Instance_1 | In Table 3, we present a detail comparison of our theoretical energy values from the layer n = 7. For this purpose, we have taken four data sets available in the literature. First, we compare with the ab initio values of Fritzsche (1995) because they have used a larger configuration space than previous ab initio comput... | [
"NIST Atomic Spectra Database (ver. 5.3) 2017"
] | [
"Fourthly, with the NIST data base",
"which is considered as the most critically analysed data base.",
"Comparison with observed energies",
"and with the NIST values shows that the present ab initio values are not fully converged to experimental values."
] | [
"Uses",
"Uses",
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[
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[
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2022MNRAS.516.2500C__Lin_et_al._2009_Instance_1 | Neutron star X-ray binaries are an important class of low-mass X-ray binaries to understand the radiative and dynamical configuration of the inner region of an accretion disc. Though from previous studies especially based on RXTE (Rossi X-ray Timing Explorer) data of Z sources, it was known that there must exist a coro... | [
"Lin et al. 2009"
] | [
"The hybrid source XTE J1701–462 occupies a special place among NS LMXBs and is considered to be a remarkable source, as it displays all the characteristics exhibited by both Z and atoll sources"
] | [
"Motivation"
] | [
[
1492,
1507
]
] | [
[
1272,
1465
]
] |
2021MNRAS.504.3316B__than_2000_Instance_3 | WASP-43b is the most heavily scrutinized phase curve, with four analyses of this data set already published (Stevenson et al. 2017; Mendonça et al. 2018; Morello et al. 2019; May & Stevenson 2020). Our phase curve semi-amplitude, eclipse depth, and radius are consistent with all of these works. The more contentious iss... | [
"Stevenson et al. (2017)"
] | [
"As for the planet’s phase offset,",
"and May & Stevenson (2020) favour a larger phase offset (21 ± 2 °E) than Mendonça et al. (2018) and Morello et al. (2019) (12 ± 3 °E and 11 ± 2 °E)."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
646,
669
]
] | [
[
612,
645
],
[
670,
818
]
] |
2015MNRAS.446.1140T__Murray_et_al._2010_Instance_3 | Recently, forms of feedback that are fundamentally different from SNe have been shown to be essential to galaxy formation. Murray, Quataert & Thompson (2010) analysed the dynamical effects of several forms of stellar feedback on parent molecular clouds. In their models they include momentum input from ionized gas in H ... | [
"Murray et al. 2010"
] | [
"There are at least three reasons why radiative feedback is an essential ingredient of the galaxy formation process.",
"Thirdly, it is difficult to explain the large gas turbulence values observed in star-forming regions without including the momentum input by radiation"
] | [
"Background",
"Background"
] | [
[
2072,
2090
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[
1353,
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[
1920,
2070
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2018MNRAS.473.4279D__Markevitch_et_al._2002_Instance_1 | The Hubble Frontier Fields program1 (or HFF hereafter, Lotz et al. 2017) provides the most remarkably detailed examples of gravitational lensing by galaxy clusters, registering hundreds of multiply lensed galaxies for charting galaxy formation to unprecedented depths (see e.g. Jauzac et al. 2014, 2015a,b; Lam et al. 20... | [
"Markevitch et al. 2002"
] | [
"Furthermore, most of these HFF clusters are in a state of collision, enhancing their value for assessing the collisionality of dark matter (DM), a basic assumption of the standard particle interpretation of DM"
] | [
"Motivation"
] | [
[
648,
670
]
] | [
[
437,
646
]
] |
2021ApJ...916...61F__Hutsemékers_et_al._2019_Instance_1 | There are several popular scenarios employed to explain the observational features of CL AGNs. One scenario is that the broad emission lines are obscured by the torus or moving clouds over the observer’s line of sight (Goodrich & Miller 1989), while only several CL AGNs can be explained by this scenario (Wang et al. 20... | [
"Hutsemékers et al. 2019"
] | [
"The features observed in most CL AGNs, e.g., the complex multiband spectral variabilities, and strong changes seen in the infrared or low level of polarization, strongly argue against the scattering (or obscuration) scenario (e.g.,"
] | [
"Compare/Contrast"
] | [
[
665,
688
]
] | [
[
375,
606
]
] |
2018ApJ...866L...1S__Pecharromán_et_al._1999_Instance_5 | 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)"
] | [
"noted that heating bayerite at 500°C eliminates the XRD pattern of bayerite, and they note that at 700°C, the infrared reflectance spectrum of the boehmite sample no longer shows OH− stretching bands."
] | [
"Compare/Contrast"
] | [
[
1209,
1234
]
] | [
[
1235,
1435
]
] |
2017AandA...605A..88L__Bernstein_et_al._2002_Instance_1 | Altogether, the approximately thirty molecules recently detected have confirmed the chemical complexity in the nebula, and generated our interest for the present study. Of these species, we will focus our attention on the seventeen species listed by molecular families in Table 1. As can be seen in this table, the WHISP... | [
"Bernstein et al. 2002"
] | [
"As can be seen in this table, the WHISPER survey allowed the detection of some organic molecules in the Horsehead nebula, such as formaldehyde (H2CO) and methanol (CH3OH), which constitute key species in the likely synthesis of more complex organic molecules such as some prebiotic molecules"
] | [
"Uses"
] | [
[
574,
595
]
] | [
[
281,
572
]
] |
2015AandA...579A.102B__Boselli_et_al._2009_Instance_2 | Once corrected for dust attenuation, Hα luminosities can be transformed into star formation rates (SFR, in M⊙ yr-1) using a factor that depends on the assumed IMF and stellar model7: (10)\begin{equation} {SFR = k({\rm H}\alpha) \times L({\rm H}\alpha)_{\rm cor}} . \end{equation}SFR=k(Hα)×L(Hα)cor.We recall that this re... | [
"Boselli et al. 2009"
] | [
"In these objects, the total number of OB associations is significantly larger than the number of HII regions under formation and of OB stars reaching the final stage of their evolution, thus their total Hα luminosity is fairly constant with time. This might not be the case in strongly perturbed systems or in dwarf... | [
"Compare/Contrast"
] | [
[
1271,
1290
]
] | [
[
855,
1269
]
] |
2020ApJ...888...46C__Singh_et_al._1995_Instance_1 | The theoretical models mentioned above have made assumptions. The validity of these assumptions needs to be examined. Besides, all these models involve parameters to be determined. These problems could be better understood through numerical simulations. Hurlburt et al. (1994) performed a two-dimensional numerical simul... | [
"Singh et al. (1995"
] | [
"Early attempts of low-resolution three-dimensional numerical simulations on overshooting were made by",
"(downward overshooting)"
] | [
"Background",
"Background"
] | [
[
1080,
1098
]
] | [
[
936,
1037
],
[
1132,
1155
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2019AandA...622A.106M__Lanz_et_al._(2010)_Instance_2 | The standard single-frequency detection methods for point sources in the CMB and far IR are based on wavelet techniques (Vielva et al. 2003; Barnard et al. 2004; González-Nuevo et al. 2006) or on the matched filter (or MF hereafter, Tegmark & de Oliveira-Costa 1998; Herranz et al. 2002; Barreiro et al. 2003; López-Cani... | [
"Lanz et al. (2010)"
] | [
"also showed that the MMF can be generalized for the case where the SED of the sources is not known.",
"This generalization outperforms the single-frequency MF in terms of S/N and can be used to infer the spectral index of synchrotron-dominated radio sources, as shown in Lanz et al. (2013)."
] | [
"Background",
"Compare/Contrast"
] | [
[
2277,
2295
]
] | [
[
2296,
2395
],
[
2396,
2583
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] |
2015ApJ...808...56M__Deming_et_al._2015_Instance_1 | We have tested the pixel-ICA algorithm, i.e., a non-parametric method proposed by Morello et al. (2014, 2015) to detrend Spitzer/IRAC primary transit observations, on simulated data sets. Systematics similar to the ones present in Spitzer/IRAC data sets are obtained by combining instrumental jitter with inter- or intra... | [
"Deming et al. 2015"
] | [
"The detrending performances of pixel-ICA method have been compared with division by a polynomial function of the centroid, in this paper PCD method, and PLD method"
] | [
"Compare/Contrast"
] | [
[
748,
766
]
] | [
[
583,
746
]
] |
2022MNRAS.516.5289M__Thompson_et_al._2015_Instance_2 | Given the number densities within the mass-dissociation index plane of Fig. 8, we now ask ourselves whether known dissociated clusters, such as the Bullet cluster, are expected in L210N1024NR? The Bullet Cluster has a mass of $\sim 1.5 \times 10^{15} \, {\rm M}_{\odot }$ (e.g. Clowe et al. 2004; Bradač et al. 2006; Clo... | [
"Thompson et al. (2015)"
] | [
"This result is inline with the number density estimate of the order of ∼10−10 Mpc−3 by"
] | [
"Similarities"
] | [
[
1881,
1903
]
] | [
[
1794,
1880
]
] |
2022ApJ...935..135B__Mathur_1990_Instance_1 | All responses calculated in this paper only account for the direct response to a perturbing potential. In general, though, the response also has an indirect component that arises from the fact that neighboring regions in the disk interact with each other gravitationally. This self-gravity of the response, which we have... | [
"Mathur 1990"
] | [
"Our preliminary analysis shows that the self-gravitating response is a linear superposition of two terms: (i) a continuum of modes given in Equation (12), dressed by self-gravity, that undergo phase mixing and give rise to the phase spiral; and (ii) a discrete set of modes called point modes or normal modes (see",... | [
"Uses",
"Uses"
] | [
[
1145,
1156
]
] | [
[
831,
1144
],
[
1173,
1207
]
] |
2018AandA...620A..80M__observations,_Gerin_et_al._2017_Instance_1 | Methyl formate is the species for which the largest number of transitions were identified. In total 24 transitions from both A and E species were observed (18 unblended), with energy levels between 100 and 500 K, allowing to constrain the properties of the emitting region from the LTE model. We ran a set of models usin... | [
"Gerin et al. 2017"
] | [
"One warm and compact component at 200 K and a size of 0.35″ (that of the continuum compact emission obtained by ALMA Band 7 observations,"
] | [
"Uses"
] | [
[
1387,
1404
]
] | [
[
1249,
1386
]
] |
2021MNRAS.504..146V__Vink_&_Gräfener_2012_Instance_1 | The direct detection of the first gravitational waves from the merger of two heavy black holes (BHs) in GW 150914 confirmed one of the toughest predictions of Einstein’s theory of general relativity. But while satisfying the world of physics in general, for astrophysics this was only the beginning: many were surprised ... | [
"Vink & Gräfener 2012"
] | [
"this mass is significantly diminished via stellar winds already during core hydrogen (H) burning"
] | [
"Background"
] | [
[
955,
975
]
] | [
[
857,
953
]
] |
2021AandA...648A..14R__Gürkan_et_al._(2018)_Instance_1 | To obtain a more complete picture of the physical processes that shape star formation in the early Universe, very deep radio surveys overwide areas of sky are required to complement deep submillimetre surveys. Previous work has used high-resolution radio observations, typically at 1.4 GHz, as a method of pinpointing th... | [
"Gürkan et al. (2018)"
] | [
"The Low Frequency Array",
"has opened up new ways of studying galaxies in the radio, and a number of studies have used LOFAR’s capabilities to investigate this relationship between star formation and radio luminosity in the low-frequency regime – for example",
"Read et al. (2018), Smith et al. (2021), and Wang... | [
"Background",
"Background",
"Background"
] | [
[
1157,
1177
]
] | [
[
868,
891
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[
925,
1156
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[
1179,
1244
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] |
2022MNRAS.516.4833J__Boffin_&_Jorissen_1988_Instance_1 | It is now clear that binary stars hold the key to understanding the formation of many planetary nebulae (PNe; Jones & Boffin 2017a). However, with much of the recent focus being placed on common envelope evolution (Boffin & Jones 2019), the role of wider binaries remains almost completely unconstrained (Tyndall et al. ... | [
"Boffin & Jorissen 1988"
] | [
"The chemical contamination of barium stars is believed to be due to accretion of chemically enriched material from an evolved binary companion, likely through wind"
] | [
"Background"
] | [
[
1319,
1341
]
] | [
[
1154,
1317
]
] |
2015ApJ...803...96S__Török_et_al._2004_Instance_1 | Since their initial discovery with AIA on board the Solar Dynamics Observatory (SDO), HCs have been generally regarded as proxies for magnetic flux ropes (MFRs; volumetric plasma structures with magnetic field lines that wrap around a central axis). This is supported by the following observational studies: (1) Cheng et... | [
"Török et al. 2004"
] | [
"Then a separation of the HC top from that of the prominence was observed during the eruption initiated by the ideal kink instability",
"Therefore, this observation offered further important support for the idea that an HC is an MFR"
] | [
"Differences",
"Similarities"
] | [
[
1291,
1308
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[
1157,
1289
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[
1417,
1512
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2020AandA...637A..44N__Kraus_(2018)_Instance_2 | Among the existing IACT systems, HESS has the largest FoV and hence provides the highest sensitivity for the diffuse γ-ray flux. Its electron spectrum analysis technique could be directly used to obtain a measurement of the diffuse Galactic γ-ray flux above energies of several TeV in the Galactic Ridge (|l| 30°, |b| ... | [
"Kraus 2018"
] | [
"The overall excesses within 805 and 1186 h of HESS exposures"
] | [
"Uses"
] | [
[
1272,
1282
]
] | [
[
1210,
1270
]
] |
2018AandA...612A..34D__Dexter_et_al._2010_Instance_1 | Sagittarius A* (Sgr A*) is a supermassive black hole system that allows one to observationally test the aforementioned GRMHD models of accretion flows (Goddi et al. 2017). Millimeter-Very Long Baseline Interferometry (mm-VLBI) is capable of resolving the shadow of the event horizon (Falcke et al. 2000), making this an ... | [
"Dexter et al. 2010"
] | [
"Most of the radiative models for Sgr A*, which are based on post-processing GRMHD simulations, assume that electrons have a thermal, relativistic (Maxwell–Jüttner) distribution function, and that the proton-to-electron temperature ratio is constant across the simulation domain"
] | [
"Background"
] | [
[
825,
843
]
] | [
[
479,
756
]
] |
2019ApJ...882..131M__Clements_et_al._2018_Instance_1 | The ice layer covering refractory grains in dense MCs consists mainly of amorphous water ice (Tielens & Allamandola 1987). A key property of the icy mantle is its porosity, which determines its ability to adsorb, desorb, and trap atoms and molecules. The actual degree of porosity of interstellar ices is still debated. ... | [
"Clements et al. 2018"
] | [
"There are indeed indications that the buildup of the ice in cold environments results in the formation of pores as shown b",
"and simulations",
"These two studies, based on Monte Carlo simulations, suggest a significant level of porosity at the surface/subsurface, in particular in cold and dense environments."... | [
"Background",
"Background",
"Background"
] | [
[
555,
575
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] | [
[
320,
442
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[
516,
531
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[
578,
743
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] |
2022MNRAS.514.1169A__Fisher_et_al._1995_Instance_1 | SHT has some inherent geometrical advantages, especially for large-angle and deep surveys. A significant advantage is that the spherical coordinates apply to wide-angle surveys like BOSS without any flat-sky approximation. A traditional P(k) analysis relies on the flat-sky approximation to distinguish between transvers... | [
"Fisher et al. 1995"
] | [
"This geometric advantage is shared with the related analysis technique of spherical Fourier-Bessel (SFB) decomposition",
"which, in addtion to spherical harmonic decomposition, involves a further Fourier-Bessel transform and data-compression along the line-of-sight.",
"However, SFB does not share another impor... | [
"Similarities",
"Background",
"Differences"
] | [
[
671,
689
]
] | [
[
551,
669
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[
865,
1009
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[
1010,
1169
]
] |
2022MNRAS.516.3900A__Cazaux_et_al._2022_Instance_1 | Sudden outbursts of NH3 simultaneously with H2S detected with the ROSINA-DFMS instrument on the Rosetta S/C point to the presence of abundant ammonium hydrosulphide in or on carbonaceous grains from comet 67P/Churyumov-Gerasimenko. There seems to be a clear distinction between the nucleus ice, where H2S and NH3 exist i... | [
"Cazaux et al. 2022"
] | [
"While Sn can also be formed from pure H2S ice by photo processing",
"the fact that S3 is clearly related to dust and is not found in the normal nucleus ice, where H2S is quite abundant, indicates that S3 is a product of radiolysis of the ammonium salt."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1018,
1036
]
] | [
[
951,
1016
],
[
1039,
1222
]
] |
2018AandA...620A..31M__Palla_&_Stahler_1992_Instance_1 | Any massive stellar source from ~8 M⊙ can burn hot enough to completely ionise the surrounding molecular material to form an H II region (Wood & Churchwell 1989; Churchwell 1990; Kurtz 2005) and destroy any complex chemical tracers that are traditionally used to understand the kinematics of their natal environments and... | [
"Palla & Stahler 1992"
] | [
"However, for heavily accreting massive YSOs the onset of the H II region could be delayed via stellar bloating",
"where the effective temperature of the star is much cooler than it would be considering a main sequence star of the same luminosity. In these models, a halt or considerable reduction in accretion (≪1... | [
"Background",
"Background"
] | [
[
641,
661
]
] | [
[
529,
639
],
[
730,
1105
]
] |
2019AandA...625A.121M__Beaugé_&_Nesvorný_2012_Instance_2 | The final location of close-in giant planets in our models reflects the strength of the tides that we include in our modeling, which play a very important role in the decay of planetary orbits. These are dynamical tides (e.g., Lai 1997; Ivanov & Papaloizou 2004, 2007, 2011) and in our simulations we used a formulation ... | [
"Beaugé & Nesvorný 2012"
] | [
"When we change the magnitude of two tides, the final location of the planets can be adjusted"
] | [
"Uses"
] | [
[
1239,
1261
]
] | [
[
1145,
1237
]
] |
2020MNRAS.491.5073P__Sutherland_&_Saunders_1992_Instance_1 | The catalogue used in this work is based on a far-IR sample selected in the ∼2 deg2-wide COSMOS field and obtained within the Herschel-PEP survey (Lutz et al. 2011). We consider the latest released blind catalogue selected at 160-μm (DR1, 7047 sources) with >3σ flux density, corresponding to a flux limit of ∼9.8 mJy. T... | [
"Sutherland & Saunders 1992"
] | [
"Concerning the other far-IR PACS band (100 μm) and the mid-IR 24-μm band, we use the association available in the DR1 release and based on the maximum likelihood technique"
] | [
"Uses"
] | [
[
893,
919
]
] | [
[
720,
891
]
] |
2020AandA...638A..16T__Barnes_(2017)_Instance_1 | 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 time for GJ 1148 b to reach asymptotic rotation is inversely proportional to the initial Prot, as long as the initial Prot is much less than 27.5 d, and it depends on the other parameters of GJ 1148 b according to Eq. (3) of"
] | [
"Uses"
] | [
[
811,
824
]
] | [
[
582,
810
]
] |
2019ApJ...883...76R__Strateva_et_al._2005_Instance_1 | Previous observations of AGN that investigate correlations between αOX and Eddington ratio have revealed some similarities with X-ray binary outbursts at high Lbol/LEdd, but these comparisons have not been possible below the critical Lbol/LEdd ≲ 10−2, where an inversion in this correlation is predicted to occur. At hig... | [
"Strateva et al. 2005"
] | [
"At higher Eddington ratios of Lbol/LEdd ≳ 10−2, single-epoch X-ray and UV observations of large samples of AGN have previously revealed a hardening of αOX as Lbol/LEdd drops from ∼1 to ∼10−2 (e.g.,"
] | [
"Background"
] | [
[
533,
553
]
] | [
[
314,
511
]
] |
2022MNRAS.513.5245A__Done_&_Jin_2016_Instance_1 | We assume the time-scales we observe here are generated in the corona itself (and note that longer time-scale changes will be driven by the disc outside of the corona) and are made visible by a changing electron temperature and density as a result of local turbulence and coupling to mass accretion rate propagations thr... | [
"Done & Jin 2016"
] | [
"We note that we can discount variations in the seed photon population as the driver for changes in the power spectrum, as the UV emission from the disc is established to be considerably less variable than the corona in NLS1s"
] | [
"Uses"
] | [
[
661,
676
]
] | [
[
352,
576
]
] |
2018MNRAS.478...95K__Toalá_et_al._2012_Instance_1 | We subsequently considered the time evolution of a number of selected cores (based on the requirement that we have sufficient data to follow at least 200 kyr of evolution), finding a remarkably similar chemical evolution in all cores, including one that is strongly stabilized by turbulence and magnetic field and theref... | [
"Toalá et al. 2012"
] | [
"We find here that about two free-fall times (as defined for cylindrical systems, see",
"are sufficient to reach core deuteration fractions of ≳0.1."
] | [
"Uses",
"Uses"
] | [
[
977,
994
]
] | [
[
892,
976
],
[
996,
1055
]
] |
2021MNRAS.504.5074S__Maraschi,_Ghisellini_&_Celotti_1992_Instance_1 | The broad-band spectral energy distribution (SED) of blazars is characterized by two broad humps, one at optical/UV/X-ray bands and the other in the HE γ-ray band (see Padovani et al. 2017 for a recent review). It is believed that the first peak (low-energy component) is mostly due to synchrotron emission from relativi... | [
"Maraschi, Ghisellini & Celotti 1992"
] | [
"Within conventional leptonic scenarios, this component is produced when the synchrotron-emitting electrons inverse Compton up scatter the photons of internal (synchrotron self-Compton, SSC;"
] | [
"Compare/Contrast"
] | [
[
626,
661
]
] | [
[
400,
589
]
] |
2015MNRAS.446.2468E__Kauffmann_&_Haehnelt_2000_Instance_1 | In the following, all measurements and maps derived from snapshots prior to t = 800 Myr are therefore using the original simulation (R+13), with the others extracted from the simulation at 1 pc resolution (for the gaseous component). Note that star formation was turned on at t ∼ 745 Myr in the simulation as to avoid ga... | [
"Kauffmann & Haehnelt 2000"
] | [
"Adding on AGN feedback would significantly impact on the distribution, kinematics and physical status of the gas, specifically for the close environment of the black hole"
] | [
"Future Work"
] | [
[
752,
777
]
] | [
[
505,
675
]
] |
2018MNRAS.476L...6R__Cyr_et_al._2000_Instance_1 | The coronal mass ejections (CMEs) are frequent discharge of huge energy and massive magnetized plasma from the solar corona into the heliosphere. They are of paramount importance in space physics for their key role in extreme space weather and geo-effectiveness, e.g. (Gosling 1993; Low 2001; Schrijver & Siscoe 2010; Ca... | [
"St Cyr et al. 2000"
] | [
"In last few decades, the understanding of CMEs improved significantly because of space and ground-based observational data with the help of various modelling efforts. The studies are focused on the morphological and kinematic evolution of CMEs in the heliosphere, e.g."
] | [
"Background"
] | [
[
630,
648
]
] | [
[
339,
607
]
] |
2020MNRAS.499.4666F__Michałowski_2015_Instance_1 | An example of these implications is the so-called ‘dust budget crisis’ introduced in Section 4.4: the dust masses currently estimated at z > 5 are not compatible with standard dust production channels and require an overhaul in our models of the initial mass function for star formation, of supernova production rates, o... | [
"Michałowski 2015"
] | [
"The growth of dust grains through accretion in the ISM has been proposed as a solution (e.g."
] | [
"Motivation"
] | [
[
592,
608
]
] | [
[
478,
570
]
] |
2022ApJ...934..103H__Moore_et_al._2001_Instance_1 | Compared to various studies based on in situ measurements of MFR structures after eruption, the origination of CME-MFRs before and during eruptions remains elusive due to the complex environment in the solar source region and limited observations. At the present time, there are certain hypotheses on the formation proce... | [
"Moore et al. 2001"
] | [
"Other studies suggest that the presence of preeruptive MFRs is not necessary and MFRs could be built up in the corona via magnetic reconnection processes associated with flares"
] | [
"Motivation"
] | [
[
824,
841
]
] | [
[
627,
803
]
] |
2021MNRAS.508.4767S__Chiaki,_Yoshida_&_Hirano_2016_Instance_1 | Although it is still unknown why the disc fragmentation for the primordial cases is well described by the simple relation such as equation (1), an important fact is that a barotropic EOS with γeff ≃ 1.1 approximately represents the gas thermal evolution during the cloud collapse for $n \lesssim 10^{19}\, \mathrm{cm}^{-... | [
"Chiaki, Yoshida & Hirano 2016"
] | [
"For instance, it is well known that adding a tiny amount of heavy elements and dust grains alters the EOS of a collapsing cloud (e.g."
] | [
"Background"
] | [
[
1089,
1118
]
] | [
[
755,
888
]
] |
2020AandA...641A.118F__Nakajima_et_al._(2018b)_Instance_1 | Comparison with z ≈ 2−4galaxies. High-ionization UV lines have been detected in the spectra of z ≳ 2 galaxies through gravitational lensing (e.g., Stark et al. 2014; Patrício et al. 2016; Vanzella et al. 2016, 2017; Berg et al. 2018), spectral stacking (e.g., Nakajima et al. 2018b; Rigby et al. 2018; Saxena et al. 2020... | [
"Nakajima et al. 2018b",
"Nakajima et al. (2018b)",
"Nakajima et al. (2018b)"
] | [
"High-ionization UV lines have been detected in the spectra of z ≳ 2 galaxies through",
"spectral stacking",
"The EWs of He II, O III]λ1666, and C III] from these works are larger than those measured in the average spectra of our LAEs, with the exception of",
"some of the stacks from",
"The EWs from",
"ar... | [
"Background",
"Background",
"Similarities",
"Similarities",
"Differences",
"Differences"
] | [
[
260,
281
],
[
720,
743
],
[
824,
847
]
] | [
[
33,
117
],
[
235,
252
],
[
449,
596
],
[
696,
719
],
[
811,
823
],
[
848,
987
]
] |
2021ApJ...908...45B__Eyink_&_Sreenivasan_2006_Instance_1 | Here we shall set the potential
and make the change of variable
; hence, the vortical parts of the footpoint equations of motion are cast into a Hamiltonian form. The Hamiltonian describing the dynamics of magnetic footpoints driven by the vortical component of the turbulence on the photosphere is
50
... | [
"Eyink & Sreenivasan 2006"
] | [
"From Figure 2 in Rincon et al. (2017), we further notice that the vortical component of the photospheric surface velocity field has a structure reminiscent of 2D Euler turbulence, which admits a vortex point representation",
"also on the sphere"
] | [
"Uses",
"Uses"
] | [
[
626,
650
]
] | [
[
402,
624
],
[
652,
670
]
] |
2016AandA...592L..11S__Vasyunin_&_Herbst_(2013)_Instance_1 | Methanol is believed to be formed on dust grains (Watanabe & Kouchi 2002) by subsequent hydrogenation of carbon monoxide, and its detection towards prestellar cores is already a challenge for current models given the absence of efficient desorption processes in these sources. Thermal desorption is out of question becau... | [
"Vasyunin & Herbst (2013)"
] | [
"An alternative route to explain the presence of methanol in the gas phase is the reactive/chemical desorption that has been theoretically proposed by Garrod et al. (2007) and",
"and experimentally studied by Dulieu et al. (2013) and Minissale et al. (2016).",
"On the other hand, c-C3H2 is mainly formed in the ... | [
"Background",
"Background",
"Background",
"Background",
"Background",
"Differences"
] | [
[
784,
808
]
] | [
[
609,
783
],
[
809,
888
],
[
889,
948
],
[
977,
1116
],
[
1117,
1215
],
[
1243,
1648
]
] |
2016MNRAS.456..512C__Kronberg_et_al._2004_Instance_3 | 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"
] | [
"To date our knowledge of GRGs (see e.g.",
"is limited by their sparse numbers and by the difficulty of detecting them over large areas of the sky. Low-frequency radio observations have an enhanced capacity to detect the extended old electron population in these objects (see e.g. the recent Low Frequency Array – ... | [
"Background",
"Background",
"Future Work",
"Future Work"
] | [
[
1070,
1090
]
] | [
[
917,
956
],
[
1159,
1588
],
[
1589,
1763
],
[
1789,
2040
]
] |
2015MNRAS.448.1847H__Kim_et_al._2003_Instance_1 | We assume that gas and dust are well mixed along each line of sight in which case the gas surface density (Σgas) is proportional to the dust surface density (Σdust) and the proportionality factor is the gas-to-dust mass ratio (rgd). The dust masses derived by SED fitting methods vary significantly and systematically (e... | [
"Kim et al. 2003"
] | [
"Within a 500 arcsec radius centred on NGC 346, we find an atomic gas mass of 2.7×106 M⊙ using the Parkes+ATCA H i map"
] | [
"Uses"
] | [
[
812,
827
]
] | [
[
693,
810
]
] |
2021MNRAS.503.5179N__Blanton_et_al._2004_Instance_2 | Here, we report on molecular gas observations of NGC 0708, the BCG in the low-mass galaxy cluster Abell 262, itself part of the Perseus–Pisces galaxy supercluster. NGC 0708 lies 58.3 ± 5.4 Mpc away (estimated using infrared surface brightness fluctuations; Jensen et al. 2003). It is a giant elliptical galaxy with a wea... | [
"Blanton et al. 2004"
] | [
"Analysis of Chandra observations revealed a hole or bubble within the ICM, cospatial with the eastern lobe of the jet"
] | [
"Background"
] | [
[
1235,
1254
]
] | [
[
1116,
1233
]
] |
2020AandA...633A.163C__Aalto_et_al._2015_Instance_1 | By using the RADEX2 dense cloud models developed by Aalto et al. (2015) to reproduce the HCN(3–2)/(1–0) line luminosity ratios in the outflow of Mrk 231, we can attempt to find a combination of XHCN, XCN, Tkin, and nH2 solutions that can also fit the CN/HCN and CN spin doublet line ratios (Table 2). We assume that the ... | [
"Aalto et al. (2015)"
] | [
"By using the RADEX2 dense cloud models developed by",
"to reproduce the HCN(3–2)/(1–0) line luminosity ratios in the outflow of Mrk 231, we can attempt to find a combination of XHCN, XCN, Tkin, and nH2 solutions that can also fit the CN/HCN and CN spin doublet line ratios (Table 2)"
] | [
"Uses",
"Uses"
] | [
[
52,
71
]
] | [
[
0,
51
],
[
72,
299
]
] |
2022MNRAS.511.1121M__Reig_&_Nespoli_2013_Instance_4 | Critical luminosity (Lcrit) is the luminosity above which a state transition from subcritical to supercritical takes place. The subcritical state (LX Lcrit) is known to be the low luminosity state whereas the supercritical state is high luminosity state (LX > Lcrit) (Becker et al. 2012). The critical luminosity is cruc... | [
"Reig & Nespoli 2013"
] | [
"The HB pattern is generally observed in the subcritical regime and the DB pattern is observed in the supercritical regime"
] | [
"Background"
] | [
[
2008,
2027
]
] | [
[
1885,
2006
]
] |
2018ApJ...864...76Z__Plunkett_et_al._2013_Instance_1 | C18O (J = 2–1) observations revealed a rotational structure in the north–south direction at the center of IRAS 4C, but whether the rotation is Keplerian is not known due to the low signal-to-noise ratio (S/N) (Tobin et al. 2015). Spitzer IRAC observations show an outflow cavity structure highlighted by scattered light ... | [
"Plunkett et al. 2013"
] | [
"Previous 12CO observations either reported no detection of outflow emission toward this source",
"or only weak compact blueshifted emission towards east of the continuum source"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
877,
897
]
] | [
[
781,
875
],
[
918,
996
]
] |
2020AandA...633A..70P__Kocevski_et_al._2011_Instance_1 | Recent studies have used the spectral indices [OII], Hδ, and Dn4000 to probe the stellar population of galaxies at intermediate redshifts (0.5 ≲ z ≲ 1.2) because they are available in the observed optical frame. All these indicators, when combined, can be used to distinguish actively star-forming, (post-) starburst, an... | [
"Kocevski et al. 2011"
] | [
"The [OII]λ3737 emission traces on-going star formation",
"but it also depends on the metallicity and can be a poor tracer for dusty galaxies (e.g."
] | [
"Background",
"Background"
] | [
[
829,
849
]
] | [
[
530,
584
],
[
703,
791
]
] |
2020AandA...638A.113C__Juneau_et_al._2013_Instance_1 | To date, large surveys focused on detecting AGN systems have been conducted at a range of different wavelengths and, in particular, for the IR and X-ray domains (Alexander et al. 2005, 2008; Ivison et al. 2004; Lutz et al. 2005; Menéndez-Delmestre et al. 2007, 2009; Valiante et al. 2007; Pope et al. 2008; Bonzini et al... | [
"Juneau et al. 2013"
] | [
"Moreover, other studies have compared AGN selected from various wavebands and find that their host galaxies tend to have different properties",
"and star-formation rates (SFR;"
] | [
"Motivation",
"Motivation"
] | [
[
1013,
1031
]
] | [
[
800,
941
],
[
982,
1012
]
] |
2016ApJ...819...59S__Castelli_&_Kurucz_2004_Instance_1 | HD 47366 (HIP 31674, BD−12 1566, HR 2437, TYC 5373-2001-1) is listed in the Hipparcos Catalogue (ESA 1997) as a K1 III star, with a visual magnitude of V = 6.11 and a color index of B − V = 0.994. The Hipparcos parallax π = 12.5 ± 0.42 mas (van Leeuwen 2007) corresponds to a distance of 80.0 ± 2.7 pc. The reddening E(B... | [
"Castelli & Kurucz 2004"
] | [
"The model atmosphere used in this work was interpolated from the line-blanketed, local thermodynamic equilibrium (LTE) ATLAS9-ODFNEW grid"
] | [
"Uses"
] | [
[
1482,
1504
]
] | [
[
1343,
1480
]
] |
2020MNRAS.491.3860S__Schlickeiser_2003_Instance_1 | The main assumption is that the statistical properties of the interaction of the charged particles with the fields are dominated by Gaussian distributions. This is in correspondence with the Central Limit Theorem (CLT), which requires that all stochastic systems evolve asymptotically towards Gaussian statistics provide... | [
"Schlickeiser 2003"
] | [
"Besides these necessary conditions for the applicability of the FP equation, also other simplifying assumption for a better tractability of the FP equation are being made, such as (1) the magnetic fluctuations are homogeneous in space, (2) the electromagnetic fields are quasi-static, (3) the interaction has a fini... | [
"Background",
"Background"
] | [
[
889,
906
]
] | [
[
515,
888
],
[
920,
1094
]
] |
2022AandA...667A..15K__Yamashiki_et_al._2019_Instance_1 | In the search for new exoplanets, M dwarfs are ideal targets due to their high abundance in the Galaxy (Bochanski et al. 2010). However, M-type stars are prone to high levels of stellar activity (Walkowicz et al. 2011; Loyd et al. 2016, 2018b) that can impact the radial velocity and/or transit signal of such systems th... | [
"Yamashiki et al. 2019"
] | [
"Aside from the observational implications, the planet’s physical and chemical state can be altered by stellar activity as well due to, for example, coronal mass ejections (CMEs) and stellar particle events (SPEs)"
] | [
"Background"
] | [
[
862,
883
]
] | [
[
648,
860
]
] |
2020ApJ...901....8B__Müller-Mellin_et_al._1995_Instance_1 | Three semiannual galactic hydrogen spectra as a function of energy between 40 and 250 MeV have been obtained in three different consecutive time periods (from 2018 August 6 to 2020 January 5) very much inside the heliosphere (1 au); the energy profiles are shown as black circles in Figure 6. Each measured energy spectr... | [
"Müller-Mellin et al. 1995"
] | [
"As a further comparison, data from the SOHO/EPHIN spacecraft (red square marker) between 40 MeV and 53 MeV are also presented",
"The agreement appears to be good in all the three examined periods, considering both statistical and systematic uncertainties."
] | [
"Uses",
"Similarities"
] | [
[
715,
740
]
] | [
[
588,
713
],
[
743,
869
]
] |
2022ApJ...937...58I__Tabatabaei_et_al._2013_Instance_1 | For JW39 and JW100 the disks’ slopes are consistent with linearity, that is the trend expected from Equation (4). This may suggests that the smoothing scale (∼10 kpc) is similar to the CRe transport scale, and, hence, the slopes resemble the standard SFR calibrators. Therefore, the spatial correlation slopes observed i... | [
"Tabatabaei et al. 2013"
] | [
"Covering these spatial scales in ≤108 yr requires a diffusion coefficient of D ≥ 9 × 1028 cm2 s−1, which is slightly higher than observed in spiral galaxies"
] | [
"Differences"
] | [
[
1414,
1436
]
] | [
[
1230,
1386
]
] |
2019MNRAS.482.5651M__Ruiz-Lapuente_et_al._2004_Instance_1 | To judge the origin of a star in an SNR, its kinetics characteristics may provide very important informations. Generally, except for being stripped-off a part of its envelope, the companion may receive a velocity kick from the supernova ejecta, but the kick velocity is usually much smaller than the orbital velocity (Ma... | [
"Ruiz-Lapuente et al. 2004"
] | [
"If the spatial velocity of a star in an SNR is very different from the others in the SNR, the star is very possible to be the surviving companion in the remnant"
] | [
"Uses"
] | [
[
849,
874
]
] | [
[
687,
847
]
] |
2022ApJ...925..123N__Frenklach_&_Feigelson_1989_Instance_1 | Benzene (C6H6), the simplest aromatic hydrocarbon, is a molecule that has raised great interest in the astrophysical community for almost four decades. This is mainly because C6H6 is one of the main precursors of polycyclic aromatic hydrocarbons (PAHs) reported to be present in interstellar dust particles (Leger & Puge... | [
"Frenklach & Feigelson 1989"
] | [
"Mechanisms involving the addition of hydrocarbons, such as acetylene onto aromatic rings as well as the attachment of other aromatic rings, or hydrocarbon pyrolysis, have been proposed to characterize the growth process of PAHs"
] | [
"Background"
] | [
[
1259,
1285
]
] | [
[
1007,
1234
]
] |
2022MNRAS.509.6091H___2020a_Instance_1 | Galactic winds have been ubiquitously observed in galaxies at both low and high redshifts, and they are critical to galaxy formation and evolution. Simulations calibrated to match these observations predict that a large amount of galactic material is ejected as a wind before reaccreting to either form stars or be eject... | [
"Huang et al. 2020a"
] | [
"Current cosmological hydrodynamic simulations of galaxy formation employ a variety of subgrid models (e.g.",
"that artificially launch galactic winds,"
] | [
"Background",
"Background"
] | [
[
731,
749
]
] | [
[
389,
495
],
[
751,
791
]
] |
2021MNRAS.503..354G__Cantat-Gaudin_et_al._2020_Instance_2 | 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"
] | [
"These three spatial features nearby to the Sun appear to form part of the global spiral structure in the Galaxy. Contrary, the objects of older population with larger random velocities, for instance, main-sequence A–K stars or the oldest Cepheids and open clusters, do not currently follow the exact location of tho... | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1110,
1135
]
] | [
[
781,
1109
],
[
1137,
1151
]
] |
2017AandA...601A..87C__Falcke_(1996)_Instance_1 | 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)"
] | [
"The above equation should reduce to the jet Lorentz factor profile used in",
"when ζ = 1."
] | [
"Similarities",
"Similarities"
] | [
[
1077,
1090
]
] | [
[
1002,
1076
],
[
1114,
1125
]
] |
2019ApJ...884..132K__Tanihata_et_al._2003_Instance_2 | First, we discuss the discrepancy of the distribution scale of the radio core positions based on the discussions of the internal shock model (Koyama et al. 2015; Niinuma et al. 2015). As is discussed there, the radio cores in Mrk 501 and Mrk 421 observed at 43 or 22 GHz can usually be considered as the internal shocked... | [
"Tanihata et al. 2003"
] | [
"The core stable within 200 μas constrained by the VERA can be explained by Lorentz factors within a factor of two variation for the slower ejecta, i.e., 8 ≤ Γs ≤ 17, by assuming",
"Γf/Γs ≤ 1.01"
] | [
"Background",
"Background"
] | [
[
1512,
1532
]
] | [
[
1273,
1450
],
[
1498,
1510
]
] |
2019ApJ...886...34F__Sahijpal_&_Goswami_1998_Instance_2 | If the variation in 10Be/9Be ratios of CAIs reflects those episodic accretion events, 10Be/9Be ratios of CH–CB CAIs observed in this study would give important constraints on the evolution of the solar protoplanetary disk. Astronomical observations suggest that FUori-type outbursts are confined to the first few hundred... | [
"Sahijpal & Goswami 1998"
] | [
"This scenario is in agreement with arguments by other authors that the 26Al-free CAIs formed prior to injection and homogenization of 26Al in the early solar system"
] | [
"Similarities"
] | [
[
1542,
1565
]
] | [
[
1376,
1540
]
] |
2021MNRAS.501.2934C__Pinte_et_al._2019_Instance_1 | Understanding how the diverse populations of protoplanetary discs in young stellar regions results in the range of exoplanet types and architectures found in the Galaxy is one of the major goals of planet-formation theory. This is an extremely challenging task due in part to the limited observational constraints availa... | [
"Pinte et al. 2019"
] | [
"When planets become massive enough, they can carve gap",
"and disturb the dynamics of the gas"
] | [
"Background",
"Background"
] | [
[
1342,
1359
]
] | [
[
1130,
1184
],
[
1262,
1297
]
] |
2016ApJ...829...29T__Haiman_et_al._2000_Instance_1 | Among various DM candidates, the most popular candidate is the weakly interacting massive particles (WIMPs; like the neutralino), which have mass in the GeV range (Jungman et al. 1996; Bertone et al. 2005; Hooper & Profumo 2007; Feng 2010). The WIMPs are non-relativistic at the epoch of decoupling from the interacting ... | [
"Haiman et al. 2000"
] | [
"Galaxies formed in these halos because of the cooling of",
"or molecular hydrogen"
] | [
"Background",
"Background"
] | [
[
693,
711
]
] | [
[
548,
604
],
[
646,
667
]
] |
2015ApJ...798...95B___2010_Instance_1 | The gravitational microlensing of lensed quasars has proven to be an effective tool for measuring the properties of quasar accretion disks, and is starting to become useful for studying the X-ray corona as well. The time-dependent microlensing magnification (or demagnification) of one or more images of a lensed quasar ... | [
"Morgan et al. 2010"
] | [
"This allows us to use the microlensing magnifications to estimate the source size, and such work has shown that in general the accretion disks are larger than would be expected from either thin disk modeling or total flux arguments"
] | [
"Background"
] | [
[
750,
769
]
] | [
[
474,
705
]
] |
2018MNRAS.473.2020L__Preibisch_et_al._1998_Instance_1 | Upper Scorpius (hereafter UpSco) is part of the nearest OB association to the Sun, Scorpius Centaurus. The region is nearby, with a distance of ∼145 pc from Hipparcos (de Bruijne et al. 1997) and a recent update from Gaia (144.2 ± 17.6 pc: Fang, Herczeg & Rizzuto 2017). UpSco is young, with different age determinations... | [
"Preibisch et al. 1998"
] | [
"The bright end of the UpSco population has been examined in X-rays"
] | [
"Background"
] | [
[
845,
866
]
] | [
[
744,
810
]
] |
2021AandA...651A..87O__Brunthaler_et_al._2021_Instance_1 | To complement our study, we also analyzed GLOSTAR continuum images toward sites with maser emission. A full description of the GLOSTAR continuum data calibration and imaging is given in Brunthaler et al. (2021), while the full analysis of continuum images of Cygnus X will be presented in a forthcoming paper. Here, we b... | [
"Brunthaler et al. (2021)"
] | [
"A full description of the GLOSTAR continuum data calibration and imaging is given in"
] | [
"Uses"
] | [
[
186,
210
]
] | [
[
101,
185
]
] |
2015ApJ...804..101Y__Hawley_et_al._1995_Instance_1 | It is interesting to note that for wind originating within
, their value of Be becomes almost constant when
. This corresponds to the slight decrease of the poloidal velocity beyond
shown in the left panel of Figure 8. The reason why Be does not change beyond
is because in this region turbulen... | [
"Hawley et al. 1995"
] | [
"More precisely, it takes 3–4 orbits for MRI to develop and ∼10 orbits to saturate"
] | [
"Uses"
] | [
[
1029,
1047
]
] | [
[
946,
1027
]
] |
2017AandA...601A.134M__Fung_&_Dong_(2015)_Instance_2 | Several predictions for planet(s) shaping the disk of SAO 206462 have been proposed (Muto et al. 2012; Garufi et al. 2013; Fung & Dong 2015; Bae et al. 2016; van der Marel et al. 2016a. Using linear equations from the spiral density wave theory, Muto et al. (2012) suggested two planets with separations beyond ~50 au by... | [
"Fung & Dong (2015)"
] | [
"presented scaling relations between the azimuthal separation of the primary and secondary arms and the planet-to-star mass ratio for a single companion on a circular orbit with a mass between Neptune mass and 16 MJ around a 1 M⊙ star. They predicted with 30% accuracy that a single putative planet responsible for b... | [
"Background"
] | [
[
676,
694
]
] | [
[
695,
1071
]
] |
2019ApJ...883...73C___2010_Instance_1 | Assuming that the force-field approach to the solution of the Parker (1965) cosmic-ray transport equation is valid, the connection between historic cosmic-ray intensities and the solar properties they encountered lies in the effective diffusion coefficient that is assumed in this approximation. Establishing such a conn... | [
"Matthaeus et al.",
"2010"
] | [
"The most likely candidates for this task, given their reasonable agreement with observations and numerical simulations of cosmic-ray diffusion coefficients, are the quasilinear theory (QLT) of Jokipii (1966), the weakly nonlinear theory (WNLT) of Shalchi et al. (2004b), and the nonlinear guiding center theory (NLG... | [
"Background"
] | [
[
804,
820
],
[
847,
851
]
] | [
[
451,
803
]
] |
2018AandA...610A..44M__Krüger_&_Dreizler_(1992)_Instance_2 | The first investigations of the rotational spectra of ethyl isocyanide were carried out in 1966 by Bolton et al. (1966). The spectra of the first vibrational and torsional excited states were measured in the centimeter wave domain (Anderson & Gwinn 1968). In this initial study, the dipole moment was determined to be μa... | [
"Krüger & Dreizler (1992)"
] | [
"Our analysis was rather easy, starting from a prediction based on",
"parameters."
] | [
"Uses",
"Uses"
] | [
[
1117,
1141
]
] | [
[
1051,
1116
],
[
1142,
1153
]
] |
2021MNRAS.500..291B__Serafinelli_et_al._2019_Instance_1 | We have presented the analysis of the current X-ray observations of the disc wind in MCG-03-58-007. Here, multiple and variable wind components with velocities ranging from $\sim \! -0.08\, c$ to $\sim \! - 0.2\, c$ (and potentially up to $0.35\, c$) are seen at different times. Multi-epoch observations of disc winds, ... | [
"Serafinelli et al. 2019"
] | [
"Other examples of AGN with at least two variable phases of the X-ray winds are",
"and PG 1114+445"
] | [
"Background",
"Background"
] | [
[
1404,
1427
]
] | [
[
1099,
1177
],
[
1387,
1402
]
] |
2022AandA...662A..42M__Nóbrega-Siverio_et_al._2020b_Instance_1 | In the second part of the paper, we propose the set of self-similar solutions as tests for MHD numerical codes with ambipolar diffusion capabilities. To show their usefulness and validity, a battery of tests was carried out for the Bifrost code in two spatial dimensions starting from initial conditions with cylindrical... | [
"Nóbrega-Siverio et al. 2020b"
] | [
"We showed that the ambipolar diffusion module in Bifrost can cope with the passage of the solutions through the current sheets, with the level of accuracy increasing the higher the spatial resolution and in spite of the intrinsic singularity in them. Vice versa, the tests show that these functions can probe the ca... | [
"Compare/Contrast"
] | [
[
821,
849
]
] | [
[
341,
780
]
] |
2015ApJ...799..170C__Roxburgh_&_Vorontsov_2003_Instance_1 | Stellar properties were determined using three different techniques to model the oscillation frequencies extracted from the data. The first method relies on a dense grid of stellar models computed with the GARching STellar Evolution Code (GARSTEC; Weiss & Schlattl 2008) including the effects of microscopic diffusion, a... | [
"Roxburgh & Vorontsov 2003"
] | [
"The results were obtained implementing a Bayesian scheme that uses the spectroscopic constraints and frequency ratios as the parameters in the fit",
", the latter being almost insensitive to the surface effects in solar-like oscillators"
] | [
"Uses",
"Uses"
] | [
[
705,
730
]
] | [
[
434,
580
],
[
617,
703
]
] |
2015AandA...577A..43S__Odstrčil_&_Karlický_(1997)_Instance_2 | The initialization of solar flares remains an unsolved problem. Early ideas on how the initialization might occur were described by Norman & Smith (1978). They argued that flare process cannot start in the entire flare volume at one instant, and proposed that the flare onset was localized in a small part of an active r... | [
"Odstrčil & Karlický (1997)"
] | [
"studied the mechanism for the flare trigger by shock waves. They used a 2D magnetohydrodynamic model with the MHD shock wave propagating towards the current sheet. A portion of the shock wave passed through the sheet, and the rest was reflected. Nothing occurred at the very beginning of the wave-current sheet inte... | [
"Background",
"Motivation"
] | [
[
1524,
1550
]
] | [
[
1551,
2009
],
[
2010,
2138
]
] |
2022AandA...659A.124H__Harrison_et_al._2018_Instance_1 | Active galactic nuclei (AGN) have drawn a lot of attention over the last decades because they have been beacons for the existence and demographics of super-massive black holes (BHs) throughout the history of the Universe (e.g., Soltan 1982; Kollmeier et al. 2006; Greene & Ho 2007; Schulze & Wisotzki 2010; Kelly & Shen ... | [
"Harrison et al. 2018"
] | [
"The release of gravitational binding energy via accretion of matter onto these BHs is expected to have a profound impact on the evolution of their host galaxies (e.g.,"
] | [
"Motivation"
] | [
[
714,
734
]
] | [
[
389,
556
]
] |
2019AandA...623A.140G__Pohl_et_al._2017_Instance_1 | HD 169142 is a very young Herbig Ae-Be star with a mass of 1.65–2 M⊙ and an age of 5–11 Myr (Blondel & Djie 2006; Manoj et al. 2007) that is surrounded by a gas-rich disk (i = 13°; Raman et al. 2006; PA = 5°; Fedele et al. 2017) that is seen almost face-on. The parallax is 8.77 ± 0.06 mas (Gaia DR2 2018). Disk structur... | [
"Pohl et al. (2017)"
] | [
"Figure 1 shows the view obtained from polarimetric observations: the left panel shows the QΦ image in the J band obtained by",
"using SPHERE on a linear scale, and the two rings are clearly visible."
] | [
"Uses",
"Uses"
] | [
[
523,
541
]
] | [
[
398,
522
],
[
542,
612
]
] |
2022AandA...666A.190S___2014b_Instance_1 | For our dataset of absolute magnitudes, we used data collected at the Institute of Astronomy of V. N. Karazin Kharkiv National University within the long-term observational programme to study asteroid magnitude-phase curves (Shevchenko et al. 2010, 2012, 2014a, 2016; Slyusarev et al. 2012). We also used some observatio... | [
"Shevchenko et al.",
"2014b"
] | [
"We also used some observational data obtained within several other programmes"
] | [
"Uses"
] | [
[
582,
599
],
[
618,
623
]
] | [
[
292,
369
]
] |
2017AandA...598A..21B__Formicola_et_al._(2004)_Instance_1 | In this section, we describe a few numerical experiments carried out to analyse the importance of various hypotheses used to compute structural kernels. All models were computed using the Clés stellar evolution code (Scuflaire et al. 2008b) with the following ingredients: the CEFF equation of state (Christensen-Dalsgaa... | [
"Formicola et al. (2004)"
] | [
"The nuclear reaction rates are those from the NACRE project",
", supplemented by the updated reaction rate from"
] | [
"Uses",
"Uses"
] | [
[
681,
704
]
] | [
[
552,
611
],
[
632,
680
]
] |
2017ApJ...835...25E__Rutten_1984_Instance_2 | We compare our results with a new reduction of observations from the Lowell Observatory SSS, which is running a long-term stellar activity survey complementary to the MWO HK Project. The SSS observes solar and stellar light with the same spectrograph, with the solar telescope consisting of an exposed optical fiber that... | [
"Rutten 1984"
] | [
"Ccf is a factor that removes the color term from S and is a function of Johnson"
] | [
"Uses"
] | [
[
1122,
1133
]
] | [
[
1034,
1113
]
] |
2016AandA...587A.133G__Bruzual_&_Charlot_(2003)_Instance_1 | Notes. Intrinsic Lν(1400)/Lν(900) ratios obtained from different stellar population models: the BC03, assuming different initial mass functions (Salpeter, Salp, and Chabrier, Chab), star-formation histories (constant, cSFR, exponentially declining with τ = 0.1Gyr, exponentially rising with τ = −0.1Gyr), metallicties (Z... | [
"Bruzual & Charlot (2003)"
] | [
"Intrinsic Lν(1400)/Lν(900) ratios obtained from different stellar population models: the BC03, assuming different initial mass functions (Salpeter, Salp, and Chabrier, Chab), star-formation histories (constant, cSFR, exponentially declining with τ = 0.1Gyr, exponentially rising with τ = −0.1Gyr), metallicties (Z⊙ ... | [
"Uses",
"Uses",
"Uses",
"Background"
] | [
[
669,
693
]
] | [
[
7,
366
],
[
653,
668
],
[
695,
842
],
[
843,
1024
]
] |
2021AandA...656A..64R__Ruiz-Lara_et_al._2020_Instance_1 | Finally, we confirm our hypothesis on the origin of the bi-modal A(Li) distribution, and of the isthmus, by comparing results from our GCE model with data. In Fig. 8 we show the normalised A(Li) distribution of all the stars in our sample (blue histogram) compared with the result from three models of GCE: (i) imposing ... | [
"Ruiz-Lara et al. 2020"
] | [
"The SFR_2b model is the one that best reproduces the observed A(Li) distribution while recovering the presently observed SFR and the thin-disk stellar and HI mass"
] | [
"Compare/Contrast"
] | [
[
1002,
1023
]
] | [
[
809,
971
]
] |
2016MNRAS.457.2236K__Ouyed_&_Pudritz_1997_Instance_1 | Strong outflows are commonly associated with the early stages of stellar evolution. They are likely responsible for transporting excess angular momentum away from the star–disc system and regulating the mass-accretion process and spin evolution of newly born stars (e.g. Hartmann & Stauffer 1989; Matt & Pudritz 2005; Bo... | [
"Ouyed & Pudritz 1997"
] | [
"There are at least three possible types of outflows around young stellar objects: (1) a disc wind launched from the accretion disc (e.g."
] | [
"Background"
] | [
[
552,
572
]
] | [
[
340,
476
]
] |
2021AandA...647A.177D__Awad_&_Abu-Shady_2020_Instance_1 | An estimate of a sputtering cross-section can be inferred from our measurements with σs ≈ V∕d, where V is the volume occupied by
${Y}_{\textrm{s}}^{\infty}$Ys∞
molecules and d the depth of sputtering.
$\sigma_{\textrm{s}}\approx {Y}_{\textrm{s}}^{\infty}/l_{\textrm{d}}/\textrm{ml}$σs≈Ys∞/ld/ml
, where ml is the nu... | [
"Awad & Abu-Shady 2020"
] | [
"The net radiolysis is the combined effect of the direct primary excitations and ionisations, the core of the energy deposition by the ion, and the so-called delta rays (energetic secondary electrons) travelling at much larger distances from the core; that is, several hundreds of nanometres at the considered energi... | [
"Uses"
] | [
[
1119,
1140
]
] | [
[
699,
1029
]
] |
2021MNRAS.502.3179T__Sreenivasan,_Ramshankar_&_Meneveau_1989_Instance_1 | These properties can also be related to the fractal nature of radiative mixing layers. Recently, Fielding et al. (2020) showed that the area of the cooling surface in radiative mixing layer simulations obeys a fractal scaling, with
(31)$$\begin{eqnarray*}
\frac{A_{\rm T}}{A_{\rm L}} = \left(\frac{\lambda }{L} \right)^... | [
"Sreenivasan, Ramshankar & Meneveau 1989"
] | [
"Experimental measurements by e.g. instantaneous laser tomography have given values ranging from D = 2.1−2.4 in a variety of flow geometries, with a preferred value of D = 2.35"
] | [
"Uses"
] | [
[
847,
886
]
] | [
[
642,
817
]
] |
2020AandA...644A..88K__Shapovalova_et_al._2010b_Instance_1 | Type 1 AGN (NLSy1, quasars) and aligned CB-SMBH models expected signatures. Two SMBH and their BLRs induce more rich and complex differential phase patterns. There are many configurations for which the aligned CB-SMBH differs between them and single SMBH. The features of synthetic spectra given in Figs. C.2b and C.2c s... | [
"Shapovalova et al. 2010b"
] | [
"If a single SMBH model with a BLR d of 95 light days is true (see",
"a differential signal would be 0.9°."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
942,
966
]
] | [
[
876,
941
],
[
968,
1004
]
] |
2020ApJ...903...46C__Banerjee_et_al._2009_Instance_1 | The large values of α (significantly larger than unity) observed in clouds of low column densities or masses are often interpreted in terms of the presence of a large external confining pressure (P/
e.g., Keto & Myers 1986; Oka et al. 2001; Field et al. 2011; Leroy et al. 2015; Traficante et al. 2018a), al... | [
"Banerjee et al. 2009"
] | [
"Instead, it is most likely that these values correspond to ram pressure, in which case they imply mass, momentum, and energy flux across Eulerian cloud boundaries, or a displacement of Lagrangian boundaries"
] | [
"Uses"
] | [
[
863,
883
]
] | [
[
622,
828
]
] |
2019MNRAS.488..803M__Long_2017_Instance_1 | The identification and confirmation of extragalactic SNRs are mainly done using data from the radio (Lacey, Duric & Goss 1997; Hyman et al. 2001; Lacey & Duric 2001), visible (Matonick & Fesen 1997; Matonick et al. 1997; Gordon et al. 1998; Blair & Long 2004; Sonbas, Akyuz & Balman 2009; Sonbaş et al. 2010), and X-Ray ... | [
"Long 2017"
] | [
"The radiation of SNRs in different wavelength ranges is under the influence of biases as they cover different aspects of the ISM environment and SNR age and evolution"
] | [
"Background"
] | [
[
777,
786
]
] | [
[
529,
695
]
] |
2018AandA...610A..10C__Montaigne_et_al._2005_Instance_1 | According to chemical models, the molecules HCS+ and CS are among the most closely related species present in the ISM, as they participate in a direct exchange in both the formation and destruction of CS (Drdla et al. 1989; Lucas & Liszt 2002). In the reaction network considered by Drdla et al. (1989) and Lucas & Liszt... | [
"Montaigne et al. 2005"
] | [
"However, recent experiments indicate that this product channel occurs in only 19 percent of collisions, with 81 percent of collisions forming CH + S"
] | [
"Compare/Contrast"
] | [
[
754,
775
]
] | [
[
604,
752
]
] |
2020ApJ...904..117K___2014b_Instance_1 | Simultaneously solving the MHD equations and the global angle- and energy-dependent radiation transport equation, in general relativity, is both computationally expensive (typically prohibitively so) and technically challenging. Even so, significant progress has been made in the last decade, though the problem is usual... | [
"Jiang et al.",
"2014b"
] | [
"Even so, significant progress has been made in the last decade, though the problem is usually made tractable by introducing at least one of the following simplifying assumptions: abandoning general relativity in favor of a pseudo-Newtonian description of the gravitational potential while performing realistic, mult... | [
"Background"
] | [
[
579,
591
],
[
599,
604
]
] | [
[
229,
577
]
] |
2022MNRAS.513.5377F__Blum_et_al._2017_Instance_2 | At each heliocentric distance rh, the activity model (Fulle et al. 2020b) is defined by five analytical equations fixing (i) the gas pressure P(s) depending on the depth s from the nucleus surface (Fig. 1 for the CO2 case), (ii) the gas flux Q from the nucleus surface, (iii) the temperature gradient ∇T at depths of a f... | [
"Blum et al. 2017"
] | [
"The value R ≈ 5 mm has been constrained by several data collected at comet 67P, by laboratory experiments of dust accretion in conditions expected to occur in the solar protoplanetary disc and by observations of other protoplanetary discs"
] | [
"Uses"
] | [
[
2783,
2799
]
] | [
[
2543,
2781
]
] |
2015ApJ...805..105C__Li_1995_Instance_1 | As we said in the previous section, the evolution of the magnetic fields in the two domains (the disk and the magnetosphere) are related. It is important to note here that there is an important complication that enters into the matching between the two domains and this has to do with the abrupt transition between the d... | [
"Li 1995"
] | [
"The astrophysical disk transition region is at least equally complicated since it is not only the base of the disk corona, but also the origin of purported disk winds and outflows (e.g.,"
] | [
"Motivation"
] | [
[
1020,
1027
]
] | [
[
806,
992
]
] |
2019ApJ...871..257P__Gabuzda_et_al._2018_Instance_1 | We note that it is unlikely that poloidal magnetic fields are responsible for the observed RMs of M87 because in that case one expects ρ ∝ r0 from B ∝ r−2, which is impossible to explain with the accretion models currently available (Yuan & Narayan 2014). However, there is indication of non-negligible poloidal fields a... | [
"Gabuzda et al. 2018"
] | [
"However, there is indication of non-negligible poloidal fields as well as toroidal fields—resulting in helical magnetic fields—in the jet environment of other distant AGNs, which results in transverse RM gradients with no sign changes (e.g.,"
] | [
"Background"
] | [
[
561,
580
]
] | [
[
256,
497
]
] |
2016ApJ...822...15S__Brogaard_et_al._2012_Instance_1 | However, a significant outstanding problem of using red giants is that modeling their individual frequencies is too time consuming for the analysis of tens of thousands of stars. We therefore rely on using asteroseismic scaling relations,
ν
max
∝
gT
eff
−
1
/
2
and
Δ
ν
∝
ρ
(Brown et al. ... | [
"Brogaard et al. 2012"
] | [
"Open clusters have been used to test the scaling relations for giants"
] | [
"Background"
] | [
[
1507,
1527
]
] | [
[
1436,
1505
]
] |
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