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...633A.163C__Aalto_et_al._2015_Instance_2 | 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"
] | [
"We recall that in these models (see also",
"the dense clouds can be either self-gravitating virialised clouds, which implies that their internal velocity dispersion (Δvsg) is locked to their mass (Mvir) and size (R) through Δvsg = (GMvir/G)1/2, or unbound clouds, for which Δv ≫ Δvsg."
] | [
"Uses",
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] | [
[
522,
539
]
] | [
[
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[
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2019MNRAS.486..360K__Nättilä_&_Pihajoki_2018_Instance_1 | We have presented the principles and framework for calculating the radio signal from a PSR in an EMRB. We restrict our study to the extreme mass ratio of EMRB systems and so do not consider PSRs in stellar-mass BH binaries with finite mass ratios (e.g. Blanchet 2014; Liu et al. 2014). We account for both relativistic a... | [
"Nättilä & Pihajoki 2018"
] | [
"We approximate the PSR body as a perfect sphere. However, due to the spin of the PSR the true shape is more oblate. This will ultimately influence the pitch angle of the ray with the neutron star surface. This effect is considered to be minor, but the method could easily be extended to account for this oblateness ... | [
"Future Work"
] | [
[
2115,
2138
]
] | [
[
1795,
2114
]
] |
2018ApJ...866L...1S__Pecharromán_et_al._1999_Instance_6 | It was found that the complex dielectric function from Pecharromán et al. (1999) for the sample obtained by heating bayerite at 1273 K, assuming a spheroid with depolarization parameters of (0.35, 0.003), produced an opacity with 11, 20, 28, and 32 μm features, so this component was included in the models. However, wit... | [
"Pecharromán et al. (1999)"
] | [
"XRD performed by",
"of the sample of bayerite prepared at 1273 K suggests only θ-alumina was present, and their infrared and NMR spectroscopy confirms this."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1612,
1637
]
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1595,
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2022AandA...667A..97A__Xiong_(1986)_Instance_1 | The temperature gradient of the 3-equation model is comparable to results of different TCM approaches (Xiong & Deng 2001; Li & Yang 2007) for the base of the solar convective envelope. Both Zhang & Li (2012; their Figs. 6 and 7) and Xiong & Deng (2001; their Fig. 8) find a temperature gradient that transitions graduall... | [
"Xiong (1986)"
] | [
"From the convective flux as presented in",
"one also would expect a similar temperature gradient in the overshooting zone."
] | [
"Similarities",
"Similarities"
] | [
[
538,
550
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] | [
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[
551,
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2022MNRAS.514.2010M__Feng_&_Holder_2018_Instance_2 | In the last few years, several experiments have reported upper limits on the power spectrum of 21-cm fluctuations during reionization (Parsons et al. 2014; Patil et al. 2017; Barry et al. 2019; Mertens et al. 2020; The HERA Collaboration 2021b) and the earlier cosmic-dawn era (Eastwood et al. 2019; Gehlot et al. 2019, ... | [
"Feng & Holder 2018"
] | [
"Of course, the recent report of an absorption signal in the sky-averaged spectrum at z ∼ 17 from EDGES (Bowman et al. 2018)",
"or a brighter background",
"than models in ΛCDM cosmologies generally predict."
] | [
"Motivation",
"Motivation",
"Motivation"
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]
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1521,
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2022AandA...659A...5Y__Mills_et_al._2018_Instance_1 | Since its discovery more than five decades ago (Cheung et al. 1968), ammonia (NH3) has been a most valuable molecule for investigating the physical properties of molecular clouds (e.g., Ho & Townes 1983). While thermally excited transitions in the centimeter-wavelength inversion transitions of ammonia are regarded as a... | [
"Mills et al. 2018"
] | [
"Subsequent observations have led to the detection of new metastable ammonia masers, including",
"NH3 (2,2)"
] | [
"Background",
"Background"
] | [
[
786,
803
]
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[
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703
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[
775,
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2019AandA...622A.106M__Herranz_et_al._2009_Instance_1 | 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... | [
"Herranz et al. 2009"
] | [
"However, over the last few years a number of multifrequency compact source detection techniques have been proposed in the literature"
] | [
"Motivation"
] | [
[
1846,
1865
]
] | [
[
1691,
1823
]
] |
2019AandA...629A..93Y__Hopkins_2018_Instance_1 | The evolution of galaxies sensitively depends on the stellar initial mass function (IMF). The understanding of the IMF has changed rapidly in the past decade. Despite a direct conflict (Kroupa et al. 2013) with the theoretical expectation that the IMF should vary as the star-forming environment alters (e.g. ambient gas... | [
"Hopkins 2018"
] | [
"Despite a direct conflict",
"with the theoretical expectation that the IMF should vary as the star-forming environment alters",
"the observed IMFs of star clusters in the local Universe are consistent with no variation"
] | [
"Compare/Contrast",
"Compare/Contrast",
"Compare/Contrast"
] | [
[
632,
644
]
] | [
[
159,
184
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[
206,
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2017MNRAS.470.1442C__Hurley_et_al._2002_Instance_1 | We then allow the synthetic single or binary system to evolve until present time, adopting for our reference model a thin disc age of 10 Gyr (Cojocaru et al. 2014) and a thick disc age of 12 Gyr. This is motivated by the findings of Feltzing & Bensby (2009), who presented a sample of very likely thick disc candidates w... | [
"Hurley et al. (2002)"
] | [
"In this case, the mass of the white dwarf is also calculated from the IMFR of"
] | [
"Uses"
] | [
[
1245,
1265
]
] | [
[
1167,
1244
]
] |
2021ApJ...920...89C__Aragón-Calvo_et_al._2007_Instance_1 | As mentioned in Section 1, once the sample of matching halos between the twin N-body simulations is established, we can study the halo−LSS correlations. We employ the Hessian matrix method used in many previous articles (e.g., Hahn et al. 2007a, 2007b; Zhang et al. 2009; Kang & Wang 2015) to define the matrix as:
4
... | [
"Aragón-Calvo et al. 2007"
] | [
"Many previous works",
"used a constant smoothing length."
] | [
"Uses",
"Uses"
] | [
[
831,
855
]
] | [
[
804,
823
],
[
1016,
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]
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2020AandA...635A..81P__simulations,_Georgobiani_et_al._(2003)_Instance_2 | Furthermore, Duvall et al. (1993) noticed an inversion of the sense of asymmetry between spectrometric and photometric measurements, with line profiles in the velocity spectrum featuring more power in their low-frequency wing than in their high-frequency wing and vice-versa for line profiles in the intensity spectrum. ... | [
"Georgobiani et al. (2003)"
] | [
"Using 3D simulations,",
"computed mode line profiles in both the velocity and the intensity power spectrum alternatively at mean unity optical depth and instantaneous unity optical depth. Their results indeed show that the modulation of the “observed” intensity fluctuations due to radiative transfer could be sig... | [
"Background",
"Background"
] | [
[
1688,
1713
]
] | [
[
1666,
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[
1714,
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2016MNRAS.458.1504S__Wang_et_al._2012_Instance_1 | The energy levels calculated by Fritzsche, Fischer & Fricke (1998) with grasp92 code are more closer to the NIST values as compared with other calculations within 3.6 per cent for the levels in the ground configurations. Our calculated MCDF energies agree well with NIST data within 6.8 per cent and the maximum error ap... | [
"Wang et al. 2012"
] | [
"For the lowest 41 energy levels, we see that our calculated energies and previous fac energies",
"belonging to the n = 3 complex in Ni xiv agree well with each other and both set of calculation are of the same accuracy.",
"However, our calculated ground state configuration levels show better agreement with mea... | [
"Similarities",
"Similarities",
"Differences"
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[
594,
610
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] | [
[
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[
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[
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2018AandA...618A..24V__Reeth_et_al._2015_Instance_1 | Gamma Doradus (γ Dor) stars, with 1.4 M⊙ ≲ M* ≲ 2.0 M⊙, and slowly-pulsating B-type (SPB) stars, with 2.5 M⊙ ≲ M* ≲ 8 M⊙, exhibit high-order gravity-mode (g-mode) pulsations, gravito-inertial pulsations (Van Reeth et al. 2016), and/or purely inertial pulsations, such as r-modes (Saio et al. 2018). The restoring forces ... | [
"Van Reeth et al. 2015",
"Van Reeth et al. 2015"
] | [
"As predicted by asymptotic theory, the pulsation periods for γ Dor and SPB stars were observed to form period spacing patterns (e.g.",
"On the other hand, the stellar rotation leads to shifts in the observed pulsation mode frequencies"
] | [
"Background",
"Motivation"
] | [
[
740,
761
],
[
1253,
1274
]
] | [
[
498,
630
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[
1112,
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2017MNRAS.469.2720G__Maoz_et_al._2005_Instance_1 | With all this in mind, our last question is: What powers soft X-rays and [O III] in LINERs? This has no clear answer, but both are not tracing the same mechanism, since none of them match in morphologies. This is a clear difference between type-2 Seyferts and LINERs. In favour of the soft X-ray emission being originate... | [
"Maoz et al. 2005"
] | [
"Indeed, the ultraviolet and X-ray variability detected for many of these LINERs",
"is in favour of a direct view of the AGNs (i.e. perpendicular to the disc under the UM).",
"This is consistent with the fact that most of the [O III] morphologies found for LINERs are spheroids, if we assume that the [O III] tra... | [
"Compare/Contrast",
"Compare/Contrast",
"Similarities"
] | [
[
1060,
1076
]
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[
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[
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2018AandA...615A..57M__Remillard_&_McClintock_2006_Instance_1 | A huge amount of data at all wavelengths has been collected in the past 20 years on black hole X-ray binaries, hereafter XrBs (for a global review see Dunn et al. 2010). These objects spend most of their time in quiescence at very low accretion rates, but occasionally, they produce outbursts that last from a few months... | [
"Remillard & McClintock 2006"
] | [
"These objects spend most of their time in quiescence at very low accretion rates, but occasionally, they produce outbursts that last from a few months to a year. Their flux then rises by several orders of magnitude across the whole electromagnetic spectrum (see, e.g.,"
] | [
"Background"
] | [
[
479,
506
]
] | [
[
170,
438
]
] |
2021MNRAS.501.2897G__Pribulla_&_Rucinski_2006_Instance_2 | 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"
] | [
"WDS 02499+0856 turned out to be a quadruple system, when the northern component was found to be a double-lined (SB2) binary from the DDO spectroscopic observations"
] | [
"Background"
] | [
[
893,
917
]
] | [
[
728,
891
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] |
2016ApJ...833..216G__Gopalswamy_et_al._2014a_Instance_1 | SEP events with gigaelectronvolt particles are generally rare. Typically about a dozen events occur during each solar cycle, although only two GLEs were reported in cycle 24, probably due to the change in the state of the heliosphere (Gopalswamy et al. 2013a, 2014a; Thakur et al. 2014). It appears that the 2012 July 23... | [
"Gopalswamy et al.",
"2014a"
] | [
"Typically about a dozen events occur during each solar cycle, although only two GLEs were reported in cycle 24, probably due to the change in the state of the heliosphere"
] | [
"Background"
] | [
[
235,
252
],
[
260,
265
]
] | [
[
63,
233
]
] |
2016ApJ...833..216G___2010_Instance_2 | SEP events with gigaelectronvolt particles are generally rare. Typically about a dozen events occur during each solar cycle, although only two GLEs were reported in cycle 24, probably due to the change in the state of the heliosphere (Gopalswamy et al. 2013a, 2014a; Thakur et al. 2014). It appears that the 2012 July 23... | [
"Gopalswamy et al.",
"2010"
] | [
"SEP events with gigaelectronvolt components are accompanied by type II radio bursts from meter (m) wavelengths to kilometer (km) wavelengths"
] | [
"Background"
] | [
[
2149,
2166
],
[
2174,
2178
]
] | [
[
2007,
2147
]
] |
2022MNRAS.516.2500C__Lin_et_al._2009_Instance_2 | 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"
] | [
"Many important results were noticed based on the spectral fitting of RXTE data of this source. The mass accretion rate was found to be constant along with the Z phase in Sco-like variation and different mechanisms were proposed to explain the spectral and timing variations during the Z phase variations"
] | [
"Background"
] | [
[
2166,
2181
]
] | [
[
1861,
2164
]
] |
2022MNRAS.515.1276C__Regály_et_al._2012_Instance_1 | Vortex formation in protoplanetary discs has been shown to proceed through various mechanisms. Klahr & Bodenheimer (2003) demonstrated that in discs with a radial entropy gradient, azimuthal perturbations are baroclinically unstable and can lead to the formation of vortices. The most commonly invoked mechanism to form ... | [
"Regály et al. 2012"
] | [
"he RWI can be triggered at steep radial density gradients",
"such a gradient may be generated at the viscosity transition between regions in which the magnetorotational instability can operate (e.g."
] | [
"Background",
"Background"
] | [
[
711,
729
]
] | [
[
405,
462
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[
509,
646
]
] |
2021AandA...646L...4I__Zheng_et_al._2014_Instance_1 | Our initial sample comprised all 40 stars of the MMT-HVS survey that were revised by Kreuzer et al. (2020), together with 30 runaway stars from the collection of Silva & Napiwotzki (2011) for which we were able to obtain spectra. This covers the majority of objects with high ejection velocities in that compilation. Thi... | [
"Zheng et al. 2014"
] | [
"This group was complemented by",
"the four candidate HVSs from the LAMOST survey"
] | [
"Uses",
"Uses"
] | [
[
665,
682
]
] | [
[
317,
347
],
[
617,
663
]
] |
2020ApJ...899..147F__Venot_et_al._2015_Instance_1 | The C/O ratio varies across exoplanets’ host star populations (Delgado Mena et al. 2010; Brewer & Fischer 2016; Brewer et al. 2017), and this variation is likely to be reflected in the composition of exoplanet atmospheres, assuming that they are formed with the same materials as their stars. Moreover, various processes... | [
"Venot et al. 2015"
] | [
"Numerous studies have been performed using chemical models"
] | [
"Background"
] | [
[
797,
814
]
] | [
[
700,
758
]
] |
2019AandA...632A.104G__Hirabayashi_et_al._2016_Instance_3 | Finally, our observations are consistent with the bilobate shape of the nucleus of comet 8P/Tuttle. As noted in Sect. 1, this shape is likely common among comets because it was found for four out of the six comets for which we have spatially resolved images. This is also the case of the trans-Neptunian object 2014 MU69... | [
"Hirabayashi et al. 2016"
] | [
"For comet 8P/Tuttle, it is however not possible to distinguish the solution of a binary nucleus that formed in the first billion years of our Solar System",
"from a more recent origin following its injection into the inner Solar System (e.g.,"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
2582,
2605
]
] | [
[
2314,
2468
],
[
2497,
2581
]
] |
2020AandA...643A.178T__Friesen_et_al._(2016)_Instance_1 | Most of the clumps analyzed in this study lie in the optimal range of precise Tkin determination when using NH3 (1,1) and (2,2) lines (see Sects. 1 and 3.3). Figure 8 indicates that there is a large number of cold clumps with Tkin 20 K. The gas and dust are expected to be coupled at densities above about 104.5 or 105 ... | [
"Friesen et al. (2016)"
] | [
"Low gas temperatures are associated with Serpens South ranging from 8.9 to 16.8 K with an average of 12.3 ± 1.7 K, which is consistent with the mean value of 11 ± 1 K found by"
] | [
"Similarities"
] | [
[
789,
810
]
] | [
[
613,
788
]
] |
2021MNRAS.500.3083C__Lupi_&_Bovino_2020_Instance_1 | Previous theorethical studies have outlined that the [C ii] emission originates from the cold (with temperatures of a few 100 K) neutral medium and from photo-dissociation regions (PDR, Vallini et al. 2013). This seems to suggest that its presence closely traces star formation sites, resulting in a linear relation, as ... | [
"Lupi & Bovino 2020"
] | [
"This seems to suggest that its presence closely traces star formation sites, resulting in a linear relation, as found by De Looze et al. (2014) and Herrera-Camus et al. (2015). While at low-redshift and close to solar metallicity such a relation is well established, as shown by several observations",
"and also n... | [
"Similarities",
"Similarities",
"Compare/Contrast"
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[
600,
618
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] | [
[
208,
507
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[
558,
599
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[
621,
815
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2018ApJ...856...65W__Betoule_et_al._2014_Instance_1 | Improvements in cosmological measurement in recent years have been said to hail an era of “precision cosmology,” with observations of the cosmic microwave background (CMB) temperature anisotropies (Hinshaw et al. 2013; Planck Collaboration et al. 2016a, 2016b), baryon acoustic oscillation (BAO) wiggles in the galaxy po... | [
"Betoule et al. 2014"
] | [
"Improvements in cosmological measurement in recent years have been said to hail an era of “precision cosmology,” with observations of",
"luminosity distance–redshift relation of Type Ia supernovae (SNIa;",
"providing constraints on cosmological model parameters at percent, or subpercent, level precision."
] | [
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[
510,
529
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[
0,
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[
709,
807
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2020ApJ...898...25T__Pavlovskii_et_al._2017_Instance_1 | Recent detections of gravitational waves (GWs) have shown evidence for a high rate of black hole (BH)–BH and neutron star (NS)–NS mergers in the universe (Abbott et al. 2016a, 2016b, 2017a, 2017b, 2017c, 2019a; Zackay et al. 2019, 2020; Venumadhav et al. 2020). However, the proposed astrophysical pathways to mergers re... | [
"Pavlovskii et al. 2017"
] | [
"Possible compact-object merger pathways include isolated binary evolution",
"accompanied by mass transfer"
] | [
"Background",
"Background"
] | [
[
624,
646
]
] | [
[
341,
414
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[
571,
599
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] |
2020AandA...640L..11B__Segretain_1996_Instance_3 | Another possibly important cooling delay may arise from the phase separation of 22Ne during crystallization (Isern et al. 1991; Althaus et al. 2010). Our current best understanding is that at the small 22Ne concentrations typical of C/O white dwarfs (∼1% by number), the presence of 22Ne should not affect the phase diag... | [
"Segretain 1996"
] | [
"These parameters are entirely consistent with those found in preliminary studies"
] | [
"Similarities"
] | [
[
1626,
1640
]
] | [
[
1544,
1624
]
] |
2021MNRAS.503.1319G__Kochanek_1992_Instance_1 | Independent of the traditional redshift surveys, in this work, we constrain the VDF of ETGs using the statistics of strong gravitational lensing systems (Turner et al. 1984; Biesiada 2006; Cao et al. 2012b,c). Assuming the concordance cosmological model (ΛCDM), several efforts have been made to include the distribution... | [
"Kochanek 1992"
] | [
"Here, we present a new approach to derive the VDF based on the lens redshift distribution",
"and to constrain its evolution out to z ∼ 1, given its strong dependency on the dynamical properties of galaxies (i.e. stellar velocity dispersion) and the number density of gravitational lenses (i.e. galaxy evolution)."... | [
"Uses",
"Uses"
] | [
[
930,
943
]
] | [
[
839,
928
],
[
945,
1164
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] |
2022AandA...663A..44K__Blundell_et_al._1999_Instance_1 | The remarkably bright nature of radio-jetted active galactic nuclei (AGNs) allows us to observe them at extreme redshifts and thus use their properties as an observational tracer of cosmological principles (Wang et al. 2021). Blazars, in particular, benefit from increased apparent luminosities due to relativistic boost... | [
"Blundell et al. 1999"
] | [
"Beyond this redshift, matters are complicated by uncertainties about the density evolution and the build-up of high black hole masses in the early universe"
] | [
"Background"
] | [
[
1596,
1616
]
] | [
[
1439,
1594
]
] |
2016AandA...585A..48G__Mostardi_et_al._(2013)_Instance_2 | On the same SSA22 field, Nestor et al. (2011) and Nestor et al. (2013) show nine LBGs and 20 Lyman-α emitters (LAEs) with LyC detection out of a sample of 41 LBGs and 91 LAEs (all spectroscopically confirmed). They started from a different narrowband image centred at ~3640 Å, which is deeper than that used by Iwata et ... | [
"Mostardi et al. (2013)"
] | [
"These conclusions have been strengthened by recent observations by Siana et al. (2015), who found no convincing detection in their deep HST imaging with WFC3-UVIS of five LyC emitters extracted from the sample of Nestor et al. (2011), or by Mostardi et al. (2015), who only found one robust LyC emitter after a rean... | [
"Similarities"
] | [
[
1894,
1916
]
] | [
[
1542,
1893
]
] |
2019MNRAS.488.4638L__Drabek-Maunder_et_al._2016_Instance_2 | In Fig. 10, we plot the variation of the ratio of the outflow contribution to the FWHM and turbulent energy. The ratio of the outflow contribution = 1 – ‘non-outflow contribution’/‘all contributions’. We observe that the outflow has a contribution in the FWHM: about 20 per cent in the local region at the H ii region (... | [
"Drabek-Maunder et al. (2016)"
] | [
"However,",
"reported that there is no correlation between the turbulent and outflow energies."
] | [
"Differences",
"Differences"
] | [
[
1780,
1808
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] | [
[
1771,
1779
],
[
1832,
1913
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] |
2021MNRAS.500.3083C__Meneghetti_et_al._2017_Instance_1 | A natural help in observational studies of particularly faint objects is provided by strong gravitational lensing. In the last few years, much progress in this field has been driven by deep observations of massive galaxy clusters, carried out in the context of large Hubble Space Telescope programmes, in particular the ... | [
"Meneghetti et al. 2017"
] | [
"Robust lens models of galaxy clusters are built thanks to the identification of large numbers of multiply lensed sources, which can span a large redshift range"
] | [
"Background"
] | [
[
537,
559
]
] | [
[
376,
535
]
] |
2020ApJ...904...91V__Zanon_et_al._2018_Instance_1 | When in a rotation-powered state, many spiders exhibit a nonthermal (synchrotron radiation; SR) orbitally modulated emission component in the X-ray band, attributed to particle acceleration in an intrabinary pulsar wind termination shock (IBS) and Doppler boosting of a bulk flow along the shock tangent (e.g., Wadiasing... | [
"Miraval Zanon et al. 2018"
] | [
"The existence of a shock is also indicated by orbital-phase- and frequency-dependent radio eclipses of the MSP (since plasma structures at the shock attenuates the radio), where in RBs the eclipse fraction can be >50% (e.g.",
"of the orbital phase (while the MSP remains largely uneclipsed at inferior conjunction... | [
"Background",
"Background"
] | [
[
879,
904
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] | [
[
602,
825
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[
906,
1008
]
] |
2015MNRAS.454.3134M__Wilkinson_&_Uttley_2009_Instance_1 | In order to study the behaviour of the soft residuals and attempt to distinguish between possible origins, we require a source that evolves across a dynamic range in spectral hardness; as can be seen from fig. 8 and tables 2 and 3 of M15, the ideal source for such a study is NGC 1313 X-1. However, both the inferred (de... | [
"Wilkinson & Uttley 2009"
] | [
"M15 show, via use of covariance spectra (see",
"for a review of the technique), that the ULX continuum emission originates from at least two components that cross at ∼1 keV."
] | [
"Background",
"Background"
] | [
[
493,
516
]
] | [
[
448,
492
],
[
537,
662
]
] |
2016ApJ...826..134D__Wiedenbeck_et_al._2013_Instance_1 | Solar energetic particle (SEP) events as can be observed in the Earth’s orbit are determined by a combination of the underlying acceleration, injection and transport conditions, and therefore carry fundamental information on these processes. In the classical picture introduced by Reames (1999), SEP events are separated... | [
"Wiedenbeck et al. 2013"
] | [
"Recent observations during the STEREO era, however, question this simple picture, especially since the nature of events showing wide longitudinal SEP spreads appears to be more complicated. It was found that 3He-rich events extend over more than 130° in longitude",
"and that near-relativistic electron events can... | [
"Background",
"Background"
] | [
[
1233,
1255
]
] | [
[
968,
1231
],
[
1258,
1344
]
] |
2022MNRAS.516.5618P__Helton_et_al._2021_Instance_1 | At present, direct detection of the CGM in emission poses an observational challenge due to its diffuse nature (with hydrogen densities of the order of nH 0.1 cm−3). Cosmological hydrodynamical simulations concur that the emission signal is faint by current observational standards (Augustin et al. 2019; Péroux et al. 2... | [
"Helton et al. 2021"
] | [
"For these reasons, detections in emission at high-redshifts are currently limited to deep fields",
"while detections at z1 are now becoming available"
] | [
"Motivation",
"Motivation"
] | [
[
936,
954
]
] | [
[
444,
540
],
[
785,
834
]
] |
2015MNRAS.450.3840C__Dunn_et_al._2010_Instance_1 | In order to understand the uniqueness of the recurrence of the 4U 1630–472 outbursts and to correlate this with the lack of high-energy emission, we investigated the ASM and BAT light curves of some of the brightest and active transient black hole X-ray binaries (BHXRBs) during the seven years (2005–2011) in which both... | [
"Dunn et al. 2010"
] | [
"Many studies of the outburst evolution of these sources have been reported in the literature (e.g.",
"the various outbursts observed do not have any detectable recurrence period and, in addition, show a complex behaviour in both soft and hard energy ranges and very different luminosities."
] | [
"Background",
"Background"
] | [
[
488,
504
]
] | [
[
351,
449
],
[
531,
718
]
] |
2021ApJ...923..233G__Carlton_et_al._2011_Instance_1 | One major difficulty afflicts the study of SNRs to learn about their supernovae: separating ejected material from swept-up surrounding unmodified interstellar medium (ISM) or modified CSM. Abundance clues are powerful but have limitations. Ideally, one would observe the youngest possible remnant that is large enough fo... | [
"Carlton et al. 2011"
] | [
"The angular expansion rate of 0.64 arcsec yr−1 obtained from comparing X-ray images from 2007 and 2009",
"gives an upper limit for the age of about 160 yr, less if (as is almost certainly the case) deceleration has occurred;"
] | [
"Uses",
"Uses"
] | [
[
866,
885
]
] | [
[
762,
864
],
[
887,
1005
]
] |
2020AandA...644A..97C__Leroy_et_al._2013_Instance_1 | 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"
] | [
"This boils down to quantifying the relation between molecular gas and star formation rate (SFR), which appears nearly linear in nearby discs"
] | [
"Background"
] | [
[
747,
764
]
] | [
[
569,
709
]
] |
2015MNRAS.451.2610H__Hinshaw_et_al._2013_Instance_1 | The ability to test the hypothesis that a set of data samples is drawn from some general n-dimensional probability distribution $f(\boldsymbol {x})$ has an interesting application in the validation of Bayesian inference analyses (indeed this application provided our original motivation for seeking to extend the K–S tes... | [
"Hinshaw et al. 2013"
] | [
"In precision cosmology, Bayesian inference is the main tool for setting constraints on cosmological parameters"
] | [
"Background"
] | [
[
745,
764
]
] | [
[
633,
743
]
] |
2021ApJ...913..115A__Linden_et_al._2012_Instance_2 | The origin of the GC VHE emission remains undetermined, due in part to source confusion and the limitations of current instruments. The source of VER J1745–290 may be Sgr A* (Atoyan & Dermer 2004; Aharonian & Neronov 2005; Ballantyne et al. 2011; Chernyakova et al. 2011; Fatuzzo & Melia 2012; Kusunose & Takahara 2012; ... | [
"Linden et al. 2012"
] | [
"Both the correlation of VHE emission with the CMZ and the lack of a cutoff in the diffuse spectrum support a hadronic scenario, capable of explaining both VER J1745–290 and the diffuse emission"
] | [
"Background"
] | [
[
1737,
1755
]
] | [
[
1518,
1711
]
] |
2018MNRAS.479.3923Z__Welsh_&_Lallement_2012_Instance_1 | Simulations are performed in Fig. 6 to compare the spectrum profiles of the S ii triplets for a synthetic absorption spectrum of a DLA with and without the magnetic alignment included. Fig. 6 was designed up to illustrate the effect in a realistic instrumental set-up, with a given typical pixel size and S/N for an opti... | [
"Welsh & Lallement 2012"
] | [
"The three transitions of singly ionized Sulfur (Sii; upper ionization potential 23.3 eV) at λλ1250.58, 1253.81, 1259.52Å represent important tracers for neutral and weakly ionized gas in the local interstellar and intergalactic medium and in distant galaxies (e.g."
] | [
"Uses"
] | [
[
815,
837
]
] | [
[
529,
793
]
] |
2018AandA...616A..99K__Narang_et_al._2016_Instance_4 | The high-resolution imaging observations of TR from IRIS reveal the ubiquitous presence of network jets. We have used three different IRIS observations of the quiet sun, which are located near the disk center. On the basis of careful inspection, 51 network jets are identified from three QS observations and used for fur... | [
"Narang et al. 2016"
] | [
"In addition, the apparent speed and length of these network jets are positively correlated, which is very similar to what has already been reported in previous works"
] | [
"Similarities"
] | [
[
1837,
1855
]
] | [
[
1670,
1835
]
] |
2022AandA...666A..80N__Piatti_2022_Instance_1 | Many studies indicate a much more complicated star formation history (SFH; e.g., Pagel & Tautvaišvienė 1998; Carrera et al. 2008; Harris & Zaritsky 2009; Rubele et al. 2012; Meschin et al. 2014; Palma et al. 2015; Perren et al. 2017) or AMR for star clusters (e.g., Olszewski et al. 1991; Hill et al. 2000; Dirsch et al.... | [
"Piatti 2022"
] | [
"with the sole exception of cluster ESO121-3 and very recently also KMHK1592, as reported by"
] | [
"Differences"
] | [
[
690,
701
]
] | [
[
598,
689
]
] |
2016AandA...591A..13V__Clarke_2004_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... | [
"Clarke 2004"
] | [
"Later, indirect evidence of the existence of intracluster magnetic fields has been given by several statistical studies on the effect of the Faraday rotation on the radio signal from background galaxies or galaxies embedded in galaxy clusters"
] | [
"Background"
] | [
[
615,
626
]
] | [
[
284,
526
]
] |
2019AandA...622A..62A__Aviles_et_al._(2018)_Instance_1 | On the other hand, PT has experienced many developments in recent years (Matsubara 2008a; Baumann et al. 2012; Carlson et al. 2013), in part because it can be useful to analytically understand different effects in the power spectrum and correlation function for the dark matter clustering. These effects can be confirmed... | [
"Aviles et al. 2018"
] | [
"The nonlinear PT for MG was developed initially in",
"and has been further studied in several other works"
] | [
"Uses",
"Extends"
] | [
[
1176,
1194
]
] | [
[
785,
835
],
[
858,
909
]
] |
2015MNRAS.450...45G__Klypin_et_al._1999_Instance_1 | The Λ cold dark matter (CDM) model has had tremendous success in providing a cosmogony that links the state of the very high redshift Universe as inferred from cosmic microwave background observations and big bang nucleosynthesis considerations, with the observed large-scale distribution of galaxies and its evolution a... | [
"Klypin et al. 1999"
] | [
"Observations on smaller, sub galactic scales, have proven more problematic for ΛCDM, with suggestions that the low abundance (e.g.",
"inferred for haloes hosting Milky Way satellites are inconsistent with the numerous substructures with cuspy density profiles that form in Milky Way-like CDM haloes."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
880,
898
]
] | [
[
749,
879
],
[
998,
1163
]
] |
2015AandA...584A.103S__Lattimer_&_Swesty_1991_Instance_1 | The energy in the inner crust is largely influenced by the properties of the neutron gas and, therefore, the EoS of neutron matter of the different calculations plays an essential role. The NV calculation (Negele & Vautherin 1973) is based on a local energy density functional that closely reproduces the Siemens-Pandhar... | [
"Lattimer & Swesty 1991"
] | [
"The LS-Ska",
"EoSs were constructed using the Skyrme effective nuclear forces Ska and SLy4, respectively."
] | [
"Background",
"Background"
] | [
[
974,
996
]
] | [
[
962,
972
],
[
1050,
1141
]
] |
2018MNRAS.479.3923Z__Yan_&_Lazarian_2006_Instance_1 | As illustrated in this paper, the variation of spectral line intensity induced by GSA varies among different spectral lines. Thus, such influence could be precisely analysed if multispectral lines for the same element is achievable. In addition, the alignment on the ground state is transferred to the levels of atoms on... | [
"Yan & Lazarian 2006"
] | [
"The collision effect can become important in the case of higher density medium where the collision rate $\\tau _c^{-1}$ (either inelastic collision rate or Van der Waals collision rate) dominates over optical pumping rate $B_{lu}\\bar{J}^0_0$ (see"
] | [
"Background"
] | [
[
1118,
1137
]
] | [
[
872,
1117
]
] |
2019MNRAS.490.5478W__Facchini_et_al._2016_Instance_1 | The focus of this work is to address the proplyd lifetime problem from a modelling perspective using recent developments in both the theory of photoevaporating discs and observations of the star and disc population in the ONC. The most similar study to this work is that of Scally & Clarke (2001), who produced an N-body... | [
"Facchini et al. 2016"
] | [
"First, thermodynamic calculations of conditions in photodissociation regions (PDRs) have been coupled with self-consistent equations for the thermally driven disc wind"
] | [
"Uses"
] | [
[
1029,
1049
]
] | [
[
841,
1008
]
] |
2020ApJ...901..130Z___2020_Instance_1 | Fast radio bursts (FRBs), a promising new and mysterious astrophysical phenomenon, are a class of bright transients with millisecond durations detected at ∼GHz (Lorimer et al. 2007; Keane et al. 2011; Thornton et al. 2013; Burke-Spolaor & Bannister 2014; Spitler et al. 2014; Masui & Sigurdson 2015; Petroff et al. 2015,... | [
"Li et al.",
"2020"
] | [
"The confirmation of their cosmological origin allows them to be widely proposed as promising tools for studying the universe and fundamental physics, e.g., the distribution of baryons in the intergalactic medium (IGM) or diffuse gas"
] | [
"Motivation"
] | [
[
1540,
1549
],
[
1556,
1560
]
] | [
[
1254,
1486
]
] |
2015ApJ...805...88Y__Metzger_et_al._2011_Instance_1 | GRB 100814A is another special event with an early-time shallow decay phase and late-time significant rebrightening in its optical afterglow light curve (Nardini et al. 2014). The power-law (
) temporal index of the early shallow decay is
, which is inconsistent with expectations from the external shock mode... | [
"Metzger et al. 2011"
] | [
"As a result, magnetars have been suggested as the central engines for some GRBs, including both long and short events"
] | [
"Background"
] | [
[
825,
844
]
] | [
[
664,
781
]
] |
2017AandA...607A.120P__Warnecke_et_al._(2016)_Instance_1 | Outside the TC, the MHD simulation behaves similarly to its HD counterpart, with baroclinicity being the dominant contribution. In terms of balance between left- and right-hand sides of (13), panels A and D show a very good agreement in most of the CZ. Differences are only evident inside the TC in the top layers and sl... | [
"Warnecke et al. (2016)"
] | [
"This problem might be alleviated in future simulations by introducing more realistic top boundary conditions like that used in"
] | [
"Future Work"
] | [
[
979,
1001
]
] | [
[
852,
978
]
] |
2019ApJ...871L..22W__Alexandrova_2008_Instance_1 | In analogy to the hydrodynamic case, the nonlinear coherent vortex structure also plays an important role in plasma dynamics and transport processes (Hasegawa & Mima 1978; Shukla et al. 1985; Petviashvili & Pokhotelov 1992; Horton & Hasegawa 1994). These vortices tend to have a long lifetime and are widely observed in ... | [
"Alexandrova 2008"
] | [
"These vortices tend to have a long lifetime and are widely observed in space, laboratory, and numerical simulation of plasma"
] | [
"Background"
] | [
[
503,
519
]
] | [
[
249,
373
]
] |
2016ApJ...827...47L__Dmitruk_et_al._2004_Instance_1 | Given the time-consuming nature of simulating energetic particle acceleration in multiple contracting and reconnecting (merging) small-scale magnetic islands produced by magnetohydrodynamic (MHD) turbulence and particle-in-the-cell (PIC) models on large spatial scales and in three dimensions, there has been an increase... | [
"Dmitruk et al. 2004"
] | [
"It was argued that magnetic flux ropes in the solar wind can be viewed to first order as being quasi-two-dimensional (quasi-2D) helical contracting and merging flux-rope structures based on three-dimensional (3D) simulations of compressible MHD turbulence that included a strong guide magnetic field"
] | [
"Background"
] | [
[
1263,
1282
]
] | [
[
962,
1261
]
] |
2018ApJ...869...47H__Hoppe_et_al._1994_Instance_1 | As for Mg, one would expect to find a positive correlation between δ29Si and initial 18O/16O ratios for the parent stars of category A grains if these quantities represent GCE. Indeed, there is a correlation between δ29Si and initial 18O/16O, as can be seen from Figure 10. The observed trend is a bit shallower than pre... | [
"Hoppe et al. 1994"
] | [
"Following the approach of Nguyen et al. (2010), we have inferred a GCE relationship between δ29Si and initial 18O/16O, which is based on a tight correlation between 29Si/28Si and 46Ti/48Ti ratios in SiC mainstream grains (Figure 11, left; data from"
] | [
"Uses"
] | [
[
1191,
1208
]
] | [
[
942,
1190
]
] |
2021MNRAS.503.1319G__Chae_&_Mao_2003_Instance_1 | In the first scenario, we assume that neither the characteristic velocity dispersion (σ*) nor the number density (n*) of galaxies evolves with redshifts (νn = νv = 0). Given the redshift coverage of the lensing galaxies in the lens sample (0.06 zl 1.0), if we constrain a non-evolving VDF using the lens data, then, as... | [
"Chae & Mao 2003"
] | [
"Such non-evolving VDF has been extensively applied in the previous studies on lensing statistics"
] | [
"Background"
] | [
[
570,
585
]
] | [
[
472,
568
]
] |
2022ApJ...934...63O__Werf_et_al._1988_Instance_1 | Cosmic rays (CRs) play a vital role in the chemistry of cold (10–30 K), dense (>102 cm−3) molecular clouds as they can pierce deep into them, unlike interstellar UV radiation (for a review see Indriolo & McCall 2013). These high-energy interstellar particles primarily consisting of protons can be heavier elements and e... | [
"van der Werf et al. 1988"
] | [
"n these regions, CRs have a wide variety of effects, one of the most important is being a producer of atomic hydrogen through the dissociation of H2"
] | [
"Background"
] | [
[
713,
737
]
] | [
[
563,
711
]
] |
2021MNRAS.502.5935S__Hani_et_al._2018_Instance_1 | We now turn to constraining c1. First, note that $\mathcal {Z} \gt 0$ for all x. In practice, we ask that $\mathcal {Z} \gt \mathcal {Z}_{\rm {min}}$ for some fiducial $\mathcal {Z}_{\rm {min}} \approx 0.01$. For x ≫ 1, this gives
(42)$$\begin{eqnarray*}
c_1 \gt \left(\mathcal {Z}_{\mathrm{min}}-\frac{\mathcal {S}}{\m... | [
"Hani et al. 2018"
] | [
"Secondly, the total metal flux into the disc across the outer boundary cannot exceed that supplied by advection of gas with metallicity $\\mathcal {Z}_{\\rm CGM}$ into the disc, since otherwise this would imply the presence of a metal reservoir external to the disc that is supplying metals to it, which is true onl... | [
"Uses"
] | [
[
928,
944
]
] | [
[
536,
906
]
] |
2020AandA...644L...7G__Magdis_et_al._2020_Instance_2 | As in G18, we compiled existing constraints on the molecular gas fraction fgas of quiescent and pSB galaxies from recent literature, namely: local QGs consisting of the ATLAS3D (Young et al. 2011; Cappellari et al. 2013; Davis et al. 2014) and HRS (Boselli et al. 2014; Lianou et al. 2016) ETG samples as well as the sam... | [
"M20"
] | [
"The dust-based estimates of G18 and",
"(and, by extension, the z ∼ 3 semi-constraints) assume a gas-to-dust ratio (G/D)."
] | [
"Background",
"Background"
] | [
[
1647,
1650
]
] | [
[
1611,
1646
],
[
1651,
1732
]
] |
2015ApJ...814....2M__Davies_&_Taylor_1950_Instance_1 | The 3D view provided in Figure 1 can be completed through the time evolution of the cross section of the same tube presented in Figure 2 for times t = 13, 35, 48 and 62. In the figure, magnetic field strength (top row) and vorticity (bottom row) maps are drawn on a vertical cut that coincides with the midplane of the b... | [
"Davies & Taylor 1950"
] | [
"We recall a few salient features obtained in those papers and reproduced here: in the initial stages (two leftmost panels), the rising portion of the flux tube has a mushroom shape, akin to an air bubble rising in water (e.g.,"
] | [
"Similarities"
] | [
[
909,
929
]
] | [
[
682,
908
]
] |
2017ApJ...844..152L__Famaey_et_al._2008_Instance_1 | Figure 3 shows the metallicity distribution of the LS. We divided the whole region into square bins with size 3 km s−1 and used color to represent the mean metallicity of each bin. The most prominent feature is the Hyades–Pleiades structure, which includes the Hyades stream (peak 0) and Pleiades stream (peak 1). It exh... | [
"Famaey et al. 2008"
] | [
"We speculate that some stars of the Hyades stream might be remnants of the Hyades cluster, while others may be the dynamical effect of non-axisymmetric components"
] | [
"Uses"
] | [
[
638,
656
]
] | [
[
474,
636
]
] |
2015ApJ...807...26T__Zucker_&_Mazeh_1994_Instance_1 | The numerous historical radial-velocity (RV) measurements of Capella have been discussed at length in our T09 study, which highlighted how challenging it has been to determine accurate values for the rapidly rotating secondary star (
km s−1), whereas those of the sharp-lined primary (
km s−1) have been quit... | [
"Zucker & Mazeh 1994"
] | [
"The RVs were measured using the two-dimensional cross-correlation algorithm TODCOR"
] | [
"Uses"
] | [
[
590,
609
]
] | [
[
506,
588
]
] |
2015MNRAS.453.3461S__Shakura_et_al._2012_Instance_1 | The recent detection of X-ray pulsations in PSR J1023+0038 during the accretion active state (Archibald et al. 2015; Bogdanov et al. 2015) implies that channelled accretion, similar to that seen in higher luminosity accreting millisecond X-ray pulsars, is occurring at a much lower accretion rate, implying that the inne... | [
"Shakura et al. 2012"
] | [
"The captured material can form a quasi-spherical shell"
] | [
"Background"
] | [
[
793,
812
]
] | [
[
716,
770
]
] |
2019ApJ...884..132K__Tanihata_et_al._2003_Instance_1 | 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 standard internal shock model of blazars considers that the discrete ejecta with higher speeds (with Lorentz factor Γf) catch up with the preceding slower ejecta (with Lorentz factor Γs), and the collision leads to the nonthermal emission (e.g.,"
] | [
"Background"
] | [
[
754,
774
]
] | [
[
485,
734
]
] |
2021MNRAS.508.2743A__Kennedy_et_al._2019_Instance_1 | Star formation from molecular cloud cores collapse is a chaotic process that is expected to result in initially misaligned and warped discs (Bonnell & Bastien 1992; Bate, Lodato & Pringle 2010; Offner et al. 2010; Bate 2018). We expect this to be the general case for circumbinary discs as well as circumstellar ones. In... | [
"Kennedy et al. 2019"
] | [
"Indeed, some misaligned circumbinary discs have already been reported",
"and HD 98800B"
] | [
"Motivation",
"Motivation"
] | [
[
683,
702
]
] | [
[
318,
387
],
[
669,
682
]
] |
2015ApJ...800...97T___2012_Instance_1 | The spectral evolution of an ensemble of stars of various masses can be combined through an IMF and followed over time. Such spectral synthesis codes are valuable tools for ultraviolet spectral libraries (Robert et al. 1993; Rix et al. 2004; Leitherer et al. 2014) and stellar population synthesis codes such as Starb... | [
"Ekström et al. 2012"
] | [
"The two panels show model spectra at times t = 0, 1, 3, 5, and 7âMyr after a coeval burst of star formation, using evolutionary tracks with rotation, at solar metallicity (Z = 0.014 from"
] | [
"Uses"
] | [
[
684,
705
]
] | [
[
495,
683
]
] |
2021ApJ...922...78X__Nan_et_al._2011_Instance_1 | Fast radio bursts (FRBs) are bright, cosmological origin, and millisecond-duration bursts in radio wavelengths (Lorimer et al. 2007; Thornton et al. 2013; Bassa et al. 2017; Macquart et al. 2020). After the discovery of the first FRB (Lorimer et al. 2007), a number of dedicated facilities have been conducted to search ... | [
"Nan et al. 2011"
] | [
"After the discovery of the first FRB",
"a number of dedicated facilities have been conducted to search FRBs, such as",
"and the Five-hundred-meter Aperture Spherical radio Telescope (FAST;",
"All these efforts result in an increasing rate of new FRB detections. Among them, more than 20 repeating FRBs have be... | [
"Background",
"Background",
"Background",
"Background"
] | [
[
871,
886
]
] | [
[
197,
233
],
[
257,
333
],
[
802,
870
],
[
905,
1034
]
] |
2018AandA...615A.148D__Weidner_et_al._(2010)_Instance_2 | 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)"
] | [
"If Tr 24 is also slightly younger than NGC 6231, as we argue below, our M-stars in Tr 24 will reach down to lower masses than in NGC 6231, with a steep increase in the detected M-star population: adopting the IMF from",
"the predicted number of cluster M stars doubles considering the mass interval 0.25–0.5 M⊙ ra... | [
"Uses",
"Uses"
] | [
[
1766,
1787
]
] | [
[
1548,
1765
],
[
1789,
1903
]
] |
2017MNRAS.470.1442C__Hurley_et_al._2002_Instance_2 | We then allow the synthetic single or binary system to evolve until present time, adopting for our reference model a thin disc age of 10 Gyr (Cojocaru et al. 2014) and a thick disc age of 12 Gyr. This is motivated by the findings of Feltzing & Bensby (2009), who presented a sample of very likely thick disc candidates w... | [
"Hurley et al. 2002"
] | [
"The second scenario involves mass transfer episodes and the evolution of the binary is obtained following the prescriptions of the bse package",
"following the parameter assumptions detailed in Camacho et al. (2014)."
] | [
"Uses",
"Uses"
] | [
[
1411,
1429
]
] | [
[
1267,
1409
],
[
1432,
1502
]
] |
2018MNRAS.476..814H__Byun_et_al._2017_Instance_1 | The most general third-order statistics is the three-point correlation function (hereafter referred to as 3PCF), which is defined in configurations space. Alternatively, one can study its Fourier space counterpart, the bispectrum. These two statistics contain, in principle, the same information. However, their analyses... | [
"Byun et al. 2017"
] | [
"The covariance of the 3PCF, on the other hand, is not diagonal, even for Gaussian fluctuations, which makes the modelling more difficult"
] | [
"Background"
] | [
[
1403,
1419
]
] | [
[
1222,
1358
]
] |
2020MNRAS.494.4382S___2010_Instance_1 | It has been thought that QPOs originate from the innermost part of an accretion disc, which is associated with strong gravity, so that we might detect general relativistic effects. Miller et al. (1998) proposed beat-frequency models and estimated the parameters of NSs using this model. Stella & Vietri (1999) developed ... | [
"Shi & Li",
"2010"
] | [
"In the last 20 years, disc-oscillation and resonance models and wave models have been proposed (e.g."
] | [
"Background"
] | [
[
595,
603
],
[
610,
614
]
] | [
[
355,
455
]
] |
2018ApJ...854...17L__Larionov_et_al._2016_Instance_1 | Early 15 GHz images using the very long baseline interferometry (VLBI) technique obtained from the very long baseline array (VLBA) indicated a twisted morphology with jet bending on a scale of ∼20 mas (Kellermann et al. 1998), and multi-epoch 43 GHz observations show jet knots with complex kinematics involving a mixtur... | [
"Larionov et al. 2016"
] | [
"Temporal variability studies during the 2012 September–October multi-band flaring period found a near-simultaneous γ-ray and optical flaring behavior, inferring a co-spatial origin"
] | [
"Compare/Contrast"
] | [
[
1035,
1055
]
] | [
[
834,
1014
]
] |
2021ApJ...914L...6A__Chhiber_et_al._2018_Instance_2 | On 2017 November 24 the MMS orbit allowed us to collect measurements in the pristine solar wind, well outside the Earth's magnetosheath and the bow shock, for a long period (i.e., a few times longer than the typical correlation scale) of approximately 1 hour from 01:10 to 02:10 UT. Figure 1 (upper panel) displays an ov... | [
"Chhiber et al. 2018"
] | [
"As reported in previous works",
"this interval is characterized by two different spectral scalings: a typical inertial range ∼ τ5/3 is found at large scales (i.e., τ > τb), while a steeper scaling ∼ τ7/3 is found at small scales (i.e., τ τb), with τb ∼ 2.4 s"
] | [
"Uses",
"Uses"
] | [
[
1020,
1039
]
] | [
[
962,
991
],
[
1070,
1295
]
] |
2017MNRAS.471.4286F__McConnell_&_Ma_2013_Instance_1 | One of the key model ingredients that determines the TDE rates is the distribution of stars in galactic nuclei (Magorrian & Tremaine 1999; Wang & Merritt 2004). Depending on the merger history of the galaxy and the efficiency of feedback on star formation, the stellar density profile can develop either a core or a cusp... | [
"McConnell & Ma 2013"
] | [
"For a galaxy of halo mass Mh, the relation between the halo mass and the velocity dispersion is simply Mh = 2σ2R/G; while the velocity dispersion can be directly related to the black hole mass using the MBH–σ relation"
] | [
"Uses"
] | [
[
723,
742
]
] | [
[
484,
701
]
] |
2022AandA...662A..42M__Vázquez_2007_Instance_1 | A number of fundamental results have been rigorously proved in the mathematical literature concerning the asymptotic behaviour in time of some of the solutions of the porous medium equation and related equations (e.g. Kamin & Vázquez 1991; Bernis et al. 1993; Hulshof et al. 2001). What is of interest for us here is, pr... | [
"Vázquez 2007"
] | [
"The most basic result, already mentioned in Sect. 4.4.1, is that initial conditions which have a finite nonzero flux integral (called ‘the mass’ in the mathematical literature for the PME) converge toward the ZKBP solution with the same flux integral (‘mass’) asymptotically in time",
"Theorem 18.2); here, allowa... | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
813,
825
]
] | [
[
529,
811
],
[
827,
964
]
] |
2017ApJ...846...52G__Mauche_et_al._1995_Instance_1 | In addition to the above problem in the UV spectroscopy of disk-dominated systems, X-ray data of CVs have also been in strong disagreement with theoretical expectations for more than three decades (Ferland et al. 1982). The culprit has been the difficult to study boundary layer (BL) between the accretion disk and the W... | [
"Mauche et al. 1995"
] | [
"However, systems in a state of high mass accretion often do not show an optically thick soft X-ray component; instead, many exhibit optically thin hard X-ray emission",
"with an X-ray luminosity much smaller than expected, i.e., much smaller than the disk luminosity."
] | [
"Background",
"Background"
] | [
[
1319,
1337
]
] | [
[
1117,
1283
],
[
1408,
1505
]
] |
2021AandA...655A..98A__Agliozzo_et_al._2019_Instance_1 | We have employed a simple grey-body fitting method to model the infrared SED of individual sources. In the LMC, which has the most numerous list of LBVs, large amounts of dust are observed (∼10−3 − 10−2 M⊙), similar to Galactic LBVNe. We stacked the infrared images of the LMC LBVs and extracted the photometry of the re... | [
"Agliozzo et al. 2019"
] | [
"A significant contribution to the stack SED comes from a few sources, the most important one is RMC143. This was already identified as a massive nebula"
] | [
"Background"
] | [
[
1001,
1021
]
] | [
[
848,
999
]
] |
2022MNRAS.513.1459M__Kaviraj,_Martin_&_Silk_2019_Instance_1 | Hierarchical structure formation scenarios (e.g. Fall & Efstathiou 1980; van den Bosch et al. 2002; Agertz, Teyssier & Moore 2011) predict that massive galaxies acquire much of their stellar mass through a combination of continuous cold gas accretion and mergers with smaller objects (e.g. Press & Schechter 1974; Moster... | [
"Kaviraj, Martin & Silk 2019"
] | [
"Signatures of past mergers take the form of faint extended tidal features such as tails (e.g.",
"– which are typically produced by major mergers"
] | [
"Background",
"Background"
] | [
[
1387,
1414
]
] | [
[
1219,
1312
],
[
1445,
1492
]
] |
2016ApJ...830..156M__Villforth_et_al._2014_Instance_1 | Comparison to a sample of inactive galaxies is also key to demonstrating that an observed merger fraction is actually related to AGN activity. Large samples of inactive galaxies are observed at all merger stages, so it is clear that a major merger alone is not a sufficient condition for quasar activity. Thus, to conclu... | [
"Villforth et al. 2014"
] | [
"Several studies of lower-luminosity AGN host morphologies with inactive control samples have been conducted in HST extragalactic survey fields (e.g.,"
] | [
"Background"
] | [
[
803,
824
]
] | [
[
527,
676
]
] |
2019MNRAS.488.5029H__Stacey_et_al._2010_Instance_1 | For the first time, we detected [C ii] 158-μm emission from a GRB host galaxy at z > 2. This is the second detection of [C ii] 158-μm emission among known GRB host galaxies, following GRB 980425 (Michałowski et al. 2016). The [C ii] 158-μm fine structure line is the dominant cooling line of the cool interstellar medium... | [
"Stacey et al. 2010"
] | [
"[C ii] 158-μm luminosity, L[C II], has been discussed as an indicator of SFR (e.g."
] | [
"Motivation"
] | [
[
617,
635
]
] | [
[
534,
616
]
] |
2016MNRAS.459.3161C__Lorimer_&_Kramer_2012_Instance_1 | For an informed opinion on the expected fluxes and durations of short transients, we have to understand coherent emission processes. What we know from incoherent emission physics is that the intrinsic brightness temperature of sources is likely limited to 1011 − 12 K (e.g. Kellermann & Pauliny-Toth 1969; Singal 1986, w... | [
"Lorimer & Kramer 2012"
] | [
"One important thing to note, that is particularly relevant here, is that most of those coherent emitters for which we know the properties of the radio spectrum have quite steep spectra, typically going as ν−2 or even ν−3 (see e.g.",
", in contrast with a typical ν−0.8 for optically thin synchrotron emission. Thi... | [
"Motivation",
"Motivation"
] | [
[
1086,
1107
]
] | [
[
841,
1071
],
[
1108,
1349
]
] |
2020ApJ...889..164M__Romani_et_al._2004_Instance_1 | The hard X-ray band has been crucial to studying some of the most powerful blazars (see e.g., Tavecchio et al. 2000; Massaro et al. 2004a, 2004b, 2006; Donato et al. 2005). More recently, the outstanding sensitivity of the Nuclear Spectroscopic Telescope Array (NuSTAR, 3–79 keV, Harrison et al. 2013) has enabled us to ... | [
"Romani et al. 2004"
] | [
"the farthest blazar detected so far is at z = 5.47,"
] | [
"Background"
] | [
[
1054,
1072
]
] | [
[
1002,
1053
]
] |
2019AandA...629A..54U__Marinucci_et_al._2015_Instance_3 | NGC 2110. NGC 2110 is another nearby (z = 0.00779, Gallimore et al. 1999), X-ray bright Seyfert galaxy. Diniz et al. (2015) report a black hole mass of
2
.
7
−
2.1
+
3.5
×
10
8
M
⊙
$ 2.7^{+ 3.5}_{- 2.1} \times 10^{8}\,{{M}_{\odot}} $
, from the relation with the stellar velocity dispersion. From Bepp... | [
"Marinucci et al. 2015"
] | [
"From 2008–2009 INTEGRAL data, Beckmann & Do Cao (2010) report a cut-off of ∼80 keV with a hard photon index, but these results are not confirmed by NuSTAR"
] | [
"Compare/Contrast"
] | [
[
1795,
1816
]
] | [
[
1639,
1793
]
] |
2020MNRAS.499..462S__Quillen_2002_Instance_1 | The physical nature of the X-structures themselves is also an open question, although significant progress has already been made in this direction. The spatial resolution of the models was not very good in the first numerical studies of 3D bar structure (≈103−104 particles represented the disc component). X-structures ... | [
"Quillen 2002",
"Quillen 2002"
] | [
"Studies of orbit composition of B/PS bulges and X-structures in different numerical and analytical models",
"showed that an X-shape is observed in these models due to a tendency of a star to spend more time near turning points of its trajectory.",
"This is indeed the case for the realistic bar potential"
] | [
"Background",
"Background",
"Background"
] | [
[
1088,
1100
],
[
2282,
2294
]
] | [
[
945,
1050
],
[
1183,
1319
],
[
2205,
2260
]
] |
2020MNRAS.499.4206B__Johnston_2020_Instance_1 | Lempo–Paha—Hiisi is a trans-Neptunian hierarchical triple system composed of a tight inner binary with components of similar size and an outer companion about half their size orbiting 10 times further away (Trujillo & Brown 2002; Benecchi et al. 2010). All large trans-Neptunian objects like Pluto have multiple small mo... | [
"Johnston 2020"
] | [
"In contrast to the Lempo system, all other known triples in the Solar system have their orbits almost regularly spaced, with one component much smaller than the others, with the most distant component being the largest"
] | [
"Differences"
] | [
[
715,
728
]
] | [
[
495,
713
]
] |
2019AandA...629A..92G__Octau_et_al._2016_Instance_1 | The Nançay Radio Telescope (NRT) is a meridian telescope equivalent to a 94 m parabolic dish located near Orléans (France). Owing to its design, the NRT can track objects with declinations δ > −39° for approximately one hour around culmination, and is thus well suited for the long-term timing of pulsars, for example, ... | [
"Octau et al. 2016"
] | [
"With the goal of identifying new exotic pulsar systems or highly stable MSPs suitable for PTA studies, the SPAN512 pulsar survey",
"was conducted between 2012 and 2018 at the NRT."
] | [
"Motivation",
"Motivation"
] | [
[
741,
758
]
] | [
[
588,
716
],
[
788,
835
]
] |
2018MNRAS.480.4154C__Li_et_al._2011a_Instance_1 | In addition to the unconstrained optimization problems of (11) and (12), many CS-based approaches consider constrained forms of the analysis and synthesis models, which are, respectively, given by
(14)
\begin{eqnarray*}
\min _{\boldsymbol{x}} \Vert \boldsymbol {\mathsf {\Psi }}^\dagger {\boldsymbol{x}}\Vert _1, \qua... | [
"Li et al. 2011a"
] | [
"CS approaches based on constrained optimization problems, solved via convex optimization techniques, have been applied broadly in RI imaging",
"These techniques have shown promising results, with improvements in terms of image fidelity and flexibility compared to traditional approaches such as clean-based method... | [
"Background",
"Compare/Contrast"
] | [
[
947,
962
]
] | [
[
762,
902
],
[
1035,
1214
]
] |
2018MNRAS.476..814H__Scoccimarro_2000_Instance_1 | The most general third-order statistics is the three-point correlation function (hereafter referred to as 3PCF), which is defined in configurations space. Alternatively, one can study its Fourier space counterpart, the bispectrum. These two statistics contain, in principle, the same information. However, their analyses... | [
"Scoccimarro 2000"
] | [
"This approximation works well, even for evolved density fields, while deviations from Gaussianity can also be taken into account"
] | [
"Compare/Contrast"
] | [
[
1162,
1178
]
] | [
[
1032,
1160
]
] |
2018MNRAS.474.2444S__Merloni_et_al._2015_Instance_1 | Other examples of AGN variability are given by the so-called changing-look AGN, which present a change in the AGN type (e.g. from Type 1 to Type 1.9) due to broadening or narrowing of the Balmer lines4 (Denney et al. 2014; LaMassa et al. 2015; Ruan et al. 2015; Gezari et al. 2016; Husemann et al. 2016; McElroy et al. 2... | [
"Merloni et al. 2015"
] | [
"and possible alternative explanations of the changing-look behaviour are",
"transient events, e.g. tidal disruption of a star by the central black hole (e.g."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
970,
989
]
] | [
[
729,
801
],
[
865,
946
]
] |
2022ApJ...927...91V__Koopmann_&_Kenney_2004_Instance_1 | According to simulations, blue galaxies infalling from the field reach pericenter in about 2.4 Gyr (McGee et al. 2009; see also Oman et al. 2013), and we can hypothesize that, by the time they get there, they lose most of their gas. In the first part of this time frame, they can start feeling the action of the ram pres... | [
"Koopmann & Kenney 2004"
] | [
"Stripping and star formation consume the available gas and galaxies first appear as truncated disks"
] | [
"Background"
] | [
[
1063,
1085
]
] | [
[
962,
1061
]
] |
2017AandA...607L...7M__Menezes_et_al._(2013)_Instance_1 | Andromeda is a galaxy that lies in the green valley (Mutch et al. 2011; Tempel et al. 2011; Jin et al. 2014). According to Belfiore et al. (2016), it is typically a low-ionisation emission-line region (LIER), as first observed by Rubin & Ford (1971) and discussed by Heckman (1996). González-Martín et al. (2015) discuss... | [
"Menezes et al. (2013)"
] | [
"Optical ionised gas has been observed by",
"next to the black hole in a field of view1 of 5′′ × 3.5′′, but this emission is weak."
] | [
"Background",
"Background"
] | [
[
632,
653
]
] | [
[
591,
631
],
[
654,
739
]
] |
2021MNRAS.502.4794N__Dullo_&_Graham_2012_Instance_1 | Alongside the above theoretical uncertainties in the physics of core formation in ellipticals, there have also been observational challenges. In particular, determining the size of the core has proven to be a non-trivial task. The light profiles of ellipticals are well described by the 3-parameter Sérsic profile (Sérsi... | [
"Dullo & Graham 2012"
] | [
"Initially the core size of a galaxy was determined by fitting the so-called ‘Nuker-profile’",
"to the surface brightness profile, a method that however depends sensitively on the radial fitting range and yields unreliable results when fit to surface brightness profiles with a large radial extent (e.g."
] | [
"Background",
"Background"
] | [
[
964,
983
]
] | [
[
624,
715
],
[
736,
943
]
] |
2020ApJ...895...51M__Rogers_&_McElwaine_2017_Instance_1 | The mechanism(s) driving the transport of angular momentum (e.g., Aerts et al. 2019a) and chemical elements (e.g., Salaris & Cassisi 2017) within stars are still not understood from stellar evolution theory. Discrepancies between observations and theory have been shown for stars with birth masses between 1.3 and 8 M
... | [
"Rogers & McElwaine 2017"
] | [
"In these radiative envelopes, the transport of chemical elements on a macroscopic scale is ascribed to",
"or internal gravity waves (IGWs, e.g.,"
] | [
"Background",
"Background"
] | [
[
753,
776
]
] | [
[
523,
625
],
[
714,
752
]
] |
2018MNRAS.477.4308R__Matteo,_Springel_&_Hernquist_2005_Instance_1 | It is well known that the accretion on to compact objects may influence the nearby ambient around SMBHs in the centre of galaxies (e.g. Salpeter 1964; Fabian 1999; Barai 2008; Germain, Barai & Martel 2009). Together with the outflow phenomena, it is believed to play a major role in the feedback processes invoked by mod... | [
"Di Matteo, Springel & Hernquist 2005"
] | [
"The problem of accretion on to an SMBH has been studied via hydrodynamical simulations (e.g."
] | [
"Background"
] | [
[
666,
702
]
] | [
[
549,
641
]
] |
2021AandA...646A..53P__Roman-Oliveira_et_al._2019_Instance_1 | In addition, the Abell 901/902 field has deep and extensive photometry in the UV (Galex, Gray et al. 2009), optical (COMBO-17 survey, Wolf et al. 2003), near-infrared (Spitzer 24 μm, Bell et al. 2007), and X-ray (XMM-Newton, Gilmour et al. 2007) wavelength range. Out of the four main substructures that embody Abell 901... | [
"Roman-Oliveira et al. 2019"
] | [
"More recently, the emission-line OMEGA-OSIRIS survey provided similar results"
] | [
"Background"
] | [
[
980,
1006
]
] | [
[
815,
892
]
] |
2020MNRAS.492..686L__Shiokawa_et_al._2015_Instance_2 | After the disruption phase, the star is tidally stretched into a very long thin stream and the evolution of the stream structure in the transverse and longitudinal directions are decoupled (Kochanek 1994). Thus, the system enters the free-fall phase where each stream segment follows its own geodesic like a test particl... | [
"Shiokawa et al. 2015"
] | [
"Many simulations consider either an intermediate-mass BH (e.g."
] | [
"Background"
] | [
[
1495,
1515
]
] | [
[
1376,
1438
]
] |
2022MNRAS.512.5165A__Uhlemann_et_al._2016_Instance_1 | The number of objects in a specific volume such as a sphere is called counts-in-cells (CIC) (Hubble 1936; Zwicky 1957; Balian & Schaeffer 1989). We know that in small scales, the distribution of CIC or equivalently one-point probability of the matter density field is not Gaussian and follows approximately a lognormal d... | [
"Uhlemann et al. 2016"
] | [
"Accordingly, it is informative to investigate the shape of the probability distribution of the matter density field and its evolution"
] | [
"Motivation"
] | [
[
807,
827
]
] | [
[
621,
754
]
] |
2016MNRAS.462.3912Q__Pinnington_et_al._1974_Instance_1 | When comparing the results obtained with our computational approach with the previously published decay rates, we find an overall good agreement. This is illustrated in Figs 2–5, where our calculations are compared with the experimental data reported by Salih et al. (1985), Crespo López-Urrutia et al. (1994), Mullman e... | [
"Pinnington et al. 1974"
] | [
"However, it is worth noting that the gA-values obtained by the latter authors were deduced from the combination of branching ratio measurements with available experimental lifetimes for the 3d74p z5F, z5D, z5G levels",
"but also with estimated lifetimes for the z3G, z3F and z3D levels from the measurement of tot... | [
"Background",
"Background"
] | [
[
1294,
1316
]
] | [
[
1041,
1257
],
[
1337,
1528
]
] |
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