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 |
|---|---|---|---|---|---|---|
2015MNRAS.450.4505H__Weiss_et_al._2013_Instance_1 | In the case of systems detected via transits, passage through an inclination resonance is likely to prevent a planet from being observed in transit, assuming the natal planetary system is edge-on in the first place. Such excitations may explain inner holes in otherwise densely packed systems observed by Kepler. An exam... | [
"Weiss et al. 2013"
] | [
"KOI-94",
"is interesting because of the presence of a Saturn mass planet in a similar orbit to 55 Cancri.",
"The innermost planet lies just outside a pair of secular resonances at 3.0 d (eccentricity) and 3.4 d (inclination) and so is consistent with a lack of inclination excitation. If we allow for the existe... | [
"Motivation",
"Motivation",
"Compare/Contrast"
] | [
[
1101,
1118
]
] | [
[
1093,
1099
],
[
1120,
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[
1216,
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]
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2021ApJ...923L..22A__Rosado_et_al._2015_Instance_3 | Pulsar timing experiments (Sazhin 1978; Detweiler 1979) allow us to explore the low-frequency (∼1–100 nHz) part of the gravitational-wave (GW) spectrum. By measuring deviations from the expected arrival times of radio pulses from an array of millisecond pulsars, we can search for a variety of GW signals and their sourc... | [
"Rosado et al. 2015"
] | [
"We expect to detect the GWB first, followed by detection of individual SMBHBs",
"that stand out above the GWB."
] | [
"Background",
"Background"
] | [
[
1369,
1387
]
] | [
[
1269,
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],
[
1433,
1462
]
] |
2019AandA...631A..35B__Bridges_et_al._(1996)_Instance_3 | The collision velocity dependence of the coefficient of restitution between particles was observed in experiments (Bridges et al. 1996; Higa et al. 1996) and is discussed in the literature (e.g., Ramírez et al. 1999; Zhang & Vu-Quoc 2002). However, the experiments by Heißelmann et al. (2010), used in the present paper ... | [
"Bridges et al. (1996)"
] | [
"In particular, the damping behavior of a large plate or surface is expected to differ from that of a same-sized particle, so that the velocity dependence of the coefficient of restitution might be an effect of the experimental setup in",
"and Higa et al. (1996)."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1290,
1311
]
] | [
[
1054,
1289
],
[
1312,
1335
]
] |
2016ApJ...822...72C__Liu_et_al._2010_Instance_1 | Here, for the first time, we have identified highly dynamic non-potential activity on QS-like supergranular network scales. These events overlie mixed polarity network flux elements near the spatial resolution of HMI, and are the first non-potential structures to be unassociated with strong concentrations of bipolar ma... | [
"Liu et al. 2010"
] | [
"Strong non-potential field arcades have been observed in hot X-ray sigmoids on scales of hundreds of arseconds",
"This range of lengths over a range of temperatures and magnetic field topologies points directly to self-similar mechanisms influencing plasma and magnetic field dynamics at a range of scales."
] | [
"Background",
"Background"
] | [
[
890,
905
]
] | [
[
739,
849
],
[
1144,
1336
]
] |
2016AandA...588A...2L__Mätzler_(1998)_Instance_1 | H2O ice on Pluto has long escaped spectroscopic detection, and based on initial New Horizons data appears to be exposed only in a number of specific locations, usually associated with red color, suggestive of water ice/tholin mix (Grundy et al. 2015; Cook et al. 2015). Nonetheless, water ice is likely to be ubiquitous ... | [
"Mätzler (1998)"
] | [
"Absorption coefficients for pure water ice (kH2O) at sub-mm-to-cm wavelengths are discussed extensively by",
"who also provides several analytic formulations to estimate them as a function of frequency and temperature along with illustrative plots."
] | [
"Background",
"Background"
] | [
[
545,
559
]
] | [
[
438,
544
],
[
561,
699
]
] |
2021AandA...655A..99D__Carigi_et_al._2005_Instance_2 | Another way of obtaining information about the nucleosynthesis processes involved in producing carbon is to compare it with other elements that are characterised by a well-known source of production, as in the case of oxygen. In Fig. 5, we show the variation of [C/O] as a function of [Fe/H], which serves as a first-ord... | [
"Carigi et al. (2005)"
] | [
"This trend is in agreement with the metallicity dependent yields from",
"which provide higher carbon as [Fe/H] increases from massive stars (i.e. also increasing the O production) but lower carbon from low and intermediate mass stars as [Fe/H] increases (i.e. less production of C)."
] | [
"Similarities",
"Similarities"
] | [
[
1909,
1929
]
] | [
[
1839,
1908
],
[
1931,
2140
]
] |
2021MNRAS.500.3002B__Kremer_et_al._2020_Instance_1 | It is as well of wide interest and diverse implications (e.g. Abadie et al. 2010; Mandel & Farmer 2017) to consider how and under which conditions NSs and BHs would pair up in tight-enough binaries so that they can spiral in by emitting GW radiation and merge within the Hubble time. Recent numerical studies based on an... | [
"Kremer et al. 2020"
] | [
"Recent numerical studies",
"show that the retention of BHs in dense stellar clusters of wide mass range, beginning from low-/medium-mass young and open clusters",
"through globular clusters",
"comprise environments where BHs can pair up through close dynamical interactions, which, furthermore, lead to genera... | [
"Background",
"Background",
"Background",
"Background"
] | [
[
1148,
1166
]
] | [
[
284,
308
],
[
481,
613
],
[
808,
833
],
[
1341,
1514
]
] |
2020AandA...641A..85S__Orienti_&_Dallacasa_2008_Instance_1 | To derive the equipartition magnetic field of J1146+4037, we predict the rest-frame 8.4 GHz (redshifted to 1.4 GHz at z = 5.0059) flux density from our spectral model. However, there is no source size measurement at 1.4 GHz. We make use of the full width at half maximum (FWHM) source size of 0.74 ± 0.01 mas derived by ... | [
"Orienti & Dallacasa (2008)"
] | [
"We note that in our calculations, we assume a source size that is 1.8 times larger than the FWHM, following the approach of Readhead (1994) and"
] | [
"Uses"
] | [
[
553,
579
]
] | [
[
409,
552
]
] |
2022AandA...663A..77N__Krolik_et_al._1981_Instance_1 | In our model, we used a non-hydrodynamical approach based on assumptions of the motion of separate clouds under gravity and the action of radiation pressure acting on dust. This has considerable limitations but they are justified as the first approximation for modeling the LIL part of the BLR. As discussed in the class... | [
"Krolik et al. 1981"
] | [
"We followed the second approach since there are natural thermal instabilities in the plasma, such as instability caused by X-ray irradiation"
] | [
"Uses"
] | [
[
1207,
1225
]
] | [
[
1065,
1205
]
] |
2016MNRAS.458.2870V__Busha_et_al._2011_Instance_1 | Unfortunately, since the study by Onions et al. only used a single dark matter halo, albeit at exquisite numerical resolution, the comparison is limited to the relatively low-mass end of the subhalo mass function (SHMF), where the cumulative mass function N( > m), exceeds unity. In order to study the massive end of the... | [
"Busha et al. 2011"
] | [
"The abundances of these rare but massive subhaloes has important implications for, among others, the statistics of massive satellite galaxies (e.g."
] | [
"Motivation"
] | [
[
575,
592
]
] | [
[
399,
546
]
] |
2020ApJ...892..103Z__Melia_&_Shevchuk_2012_Instance_1 | Similarly, according to Equation (2), angular diameter distances can be calculated from observed angular sizes as
7
and we also treated the length scale lm as a free parameter. In order to test the CDDR using different samples one should use a redshift matching criterion Δz 0.005 (Li et al. 2011; Liao et al. 2016... | [
"Melia & Shevchuk 2012)"
] | [
"The prior mean functions that we discussed are the following: zero mean function, the theoretical function of angular size calculated from the angular diameter distance under the assumption of three cosmological models: flat ΛCDM with Ωm = 0.27, so-called Rh = ct universe"
] | [
"Uses"
] | [
[
1460,
1482
]
] | [
[
1186,
1458
]
] |
2021AandA...649A..58L__Bemporad_et_al._(2018)_Instance_1 | The leading edges of the transients normally leave bright traces in the images of visible light, inspiring many methods that were developed to derive their locations and velocities, such as the icecream cone model (Fisher & Munro 1984), the graduated cylindrical shell (GCS) model (Thernisien 2011), geometric triangulat... | [
"Bemporad et al. (2018)"
] | [
"A cross-correlation method was applied to derive continuous 2D speed maps of a CME from coronagraphic images by"
] | [
"Uses"
] | [
[
1144,
1166
]
] | [
[
1032,
1143
]
] |
2022MNRAS.516.5289M__Thompson_et_al._2015_Instance_1 | 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"
] | [
"As seen in Fig. 8 there are no Bullet cluster analogues (structures of approximate mass and dissociation) in L210N1024NR, this is unsurprising as a simulation requires a significantly larger volume than that of L210N1024NR ((210cMpc h−1)3) to expect such an object (e.g."
] | [
"Uses"
] | [
[
763,
783
]
] | [
[
401,
671
]
] |
2021MNRAS.504..444C__Russell_et_al._2020b_Instance_1 | To better visualize the jet behaviour in this phase, we show in Fig. 10 the radio light curve at the core location for the first 25 d of the outburst, taken from Fig. 2. The compact jet emission peaks on MJD 58520 and then starts to decay on MJD 58521, 1 d before the system enters in the soft state and 2 d after the in... | [
"Russell et al. 2020b"
] | [
"This phenomenon is observed to start at higher frequencies (where the emission is produced closer to the compact object) and terminates as the jet break evolves through the radio band"
] | [
"Background"
] | [
[
863,
883
]
] | [
[
650,
833
]
] |
2019MNRAS.488..902C__Svensson_et_al._2012_Instance_1 | Long-duration gamma-ray bursts (GRBs) give rise to a synchrotron afterglow, detectable at optical wavelengths if sufficiently rapid and deep follow-up observations are made. A substantial fraction, however, lack such emission even when it would be expected from extrapolation of the X-ray spectral slope (Groot et al. 19... | [
"Svensson et al. 2012"
] | [
"There are two primary causes for darkness in GRBs: attenuation by dust, or rest frame ultraviolet H i absorption at high redshift"
] | [
"Background"
] | [
[
928,
948
]
] | [
[
712,
841
]
] |
2015ApJ...807...92Y__Yi_et_al._2013_Instance_1 | The assumptions of the equilibrium of pressures and equality of velocities along the contact discontinuity lead to
and
, respectively. With the jump condition for the shocks and the equilibrium of pressures, we can obtain
1
The Lorentz factor of the reverse shock
could be approximated as
2
... | [
"Yi et al. 2013"
] | [
"The number density of the ambient medium is assumed to be"
] | [
"Uses"
] | [
[
991,
1005
]
] | [
[
845,
902
]
] |
2020AandA...637A..82D__Mason_et_al._2004_Instance_1 | The emission in the diffuse interstellar medium of these bands, dominated by an aromatic vibrational character, also called AIBs (aromatic infrared bands), has led to the so-called polycyclic aromatic hydrocarbon (PAH) hypothesis. Under this theory, the observed emission is related to the infrared fluorescence emission... | [
"Mason et al. 2004"
] | [
"In absorption, bands at 3.4, 6.85, and 7.25 μm are also observed in the diffuse interstellar medium (ISM) of our Galaxy, as well as in extragalactic ISM, and can be well represented by a material with a significant amount of aliphatic character, also called HAC or a-C:H, which is a family of hydrogenated amorphous... | [
"Similarities"
] | [
[
2213,
2230
]
] | [
[
1831,
2160
]
] |
2015MNRAS.450.3458C__Cichowolski_et_al._2001_Instance_6 | The kinetic energy stored in the CO shell can be estimated as $E_{\rm kin} = 0.5\, M_{\rm shell}\, V^2_{\rm exp}$, where Vexp is the expansion velocity of the shell and Mshell is the total (molecular, atomic, and ionized) shell mass. Adopting an expansion velocity equal to half the velocity interval where the structure... | [
"Cichowolski et al. 2001"
] | [
"there is a second OB star mentioned by",
"but its location is actually outside the structure"
] | [
"Background",
"Background"
] | [
[
2695,
2718
]
] | [
[
2656,
2694
],
[
2719,
2769
]
] |
2016MNRAS.457..875P__Kotov,_Churazov_&_Gilfanov_2001_Instance_1 | After the discovery of hard X-ray lag relative to soft X-rays in binary system (e.g. Miyamoto et al. 1988; Nowak et al. 1999), similar lags were also observed in AGN (Papadakis, Nandra & Kazanas 2001; McHardy et al. 2004). The origin of hard lag is not clearly known. One possible explanation is provided by the propagat... | [
"Kotov, Churazov & Gilfanov 2001"
] | [
"The origin of hard lag is not clearly known. One possible explanation is provided by the propagation fluctuation model in which fluctuations associated with accretion flow propagate inwards in an accretion disc and thus resulting in the emission of the soft photons from relatively outer regions earlier than the ha... | [
"Background"
] | [
[
594,
625
]
] | [
[
223,
575
]
] |
2021MNRAS.503..354G__Hou_&_Han_2014_Instance_1 | The spatial distribution of OB stars and associations, young long-period Cepheids and open clusters, star-forming regions, H ii regions, interstellar dust, and giant molecular and neutral gas clouds in the solar vicinity that have been in existence generally τ ≲ 108 yr is known to correlate with the location of the inn... | [
"Hou & Han 2014"
] | [
"The Sun is situated at the inner edge of the Orion arm"
] | [
"Background"
] | [
[
614,
628
]
] | [
[
538,
592
]
] |
2018MNRAS.480..927P__Richardson_&_Fairbairn_2014_Instance_1 | The core/cusp problem is a clear example of this controversy: on the one hand, cosmological dark matter only N-body simulations predict cuspy dark halo density profiles; on the other hand, the rotation curves of low surface brightness disc and gas-rich dwarf galaxies favour shallower or cored dark matter density distri... | [
"Richardson & Fairbairn 2014"
] | [
"Also for dSphs, for which the determination of the dark matter density distribution is more difficult, there are indications that cored dark matter density profiles may be favoured with respect to cuspy profiles",
"though this finding is still debated"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
778,
805
]
] | [
[
367,
578
],
[
740,
776
]
] |
2019MNRAS.485.4343C__Rodriguez-Bernal_2012_Instance_1 | We obtain computationally credible samplings of the posterior probability (equation 8) by removing the burn-in steps of the random walk according to the autocorrelation time. We can then create synthetic data sets by drawing a parameter sample $\pmb {\theta }_k$ from the posterior and using it to draw from the likeliho... | [
"de la Horra & Teresa Rodriguez-Bernal 2012"
] | [
"The discrepancy can be calculated using a statistic like χ2",
"but here we will work with the Freeman–Tukey discrepancy since it is weight independent"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1015,
1057
]
] | [
[
936,
995
],
[
1060,
1147
]
] |
2021MNRAS.507.4564P__Murgia_2003_Instance_1 | For the radio galaxies in our sample, we estimate the minimum jet power, Pj following Wójtowicz et al. (2020):
(4)$$\begin{eqnarray}
P_{\rm j} &\sim & 1.5 \times 10^{45} \times \left(\frac{{\rm LS}}{{\rm 100 \, pc}} \right)^{9/7} \left(\frac{\tau _{\rm j}}{{\rm 100 \, yr}} \right)^{-1} \\
&&\times \, ... | [
"Murgia 2003"
] | [
"We assume ages between about 100 yr, for the most compact sources, and 105 yr for sources with LS of several kpc, as derived from radiative and kinematic ages of sources (e.g."
] | [
"Uses"
] | [
[
850,
861
]
] | [
[
634,
809
]
] |
2020MNRAS.493...87T__Maraston_et_al._2013_Instance_1 | The other significant source of scatter in the size–mass plane is the uncertainty in measuring the total stellar mass of galaxies from the integrated stellar mass density profile of the objects. As explained in Section 5.4, we measure our total stellar mass by integrating the stellar mass density profiles. To quantify ... | [
"Maraston et al. 2013"
] | [
"These values were computed by an analysis of the differences between the Portsmouth stellar masses of our galaxies"
] | [
"Uses"
] | [
[
789,
809
]
] | [
[
673,
787
]
] |
2019MNRAS.482.5430B__Eerten_&_MacFadyen_2012_Instance_1 | In light of this, the allowed structure of gamma-ray burst (GRB) jets and the efficiency at which it produces gamma-rays at large angles remains a topic of major importance, and it is useful to consider what types of jet structures are consistent with GRB observations (see also Beniamini et al. 2018b). Previous studies... | [
"van Eerten & MacFadyen 2012"
] | [
"Previous studies have considered the implications of structure models on the true energetics and rates of GRBs"
] | [
"Background"
] | [
[
546,
573
]
] | [
[
304,
414
]
] |
2021MNRAS.505.5833F__Crocce_&_Scoccimarro_2006_Instance_1 | Besides the Patchy and the LN mocks, we also model the multipoles of the BOSS CMASS two-point correlation function using an analytic approach, which is required to run the Monte Carlo analysis (see Section 5). The 2PCF can be obtained from the Fourier transform of the matter power spectrum, P(k), for which we assume th... | [
"Crocce & Scoccimarro 2006"
] | [
"while the Σnl parameter encodes the smoothing of the BAO peak due to non-linear effects"
] | [
"Uses"
] | [
[
858,
883
]
] | [
[
769,
856
]
] |
2019ApJ...875...90L__Li_et_al._2018a_Instance_1 | When energy flows from the interior of the Sun outward into the solar atmosphere, why is the Sun’s outer atmosphere, the corona, much hotter than the inner atmosphere, the underlying chromosphere and photosphere? This is the long-standing problem of the coronal heating, which is one of the eight key mysteries in modern... | [
"Li et al. 2018a"
] | [
"Especially during recent decades, high-resolution observations of solar super-fine structures indicate that small spicules, minor hot jets along small-scale magnetic channels from the low atmosphere upwards to the corona, petty tornados and cyclones, and small explosive phenomena such as mini-filament eruptions an... | [
"Background"
] | [
[
1400,
1415
]
] | [
[
824,
1246
]
] |
2018ApJ...854..155K__Mei_et_al._2012_Instance_1 | From ∼17:07 UT onward, especially during 17:12–17:14 UT, we detected multiple blobs in the bright, inverted-V-shaped structure below the flux rope, along with the fast rise of the filament (Figure 3). In Figure 12(b), boxes U and D encompass the upward- and downward-moving blobs, whose projected speeds are ∼135 and 55 ... | [
"Mei et al. 2012"
] | [
"In this case, the multiple bright blobs are plasmoids formed by bursty reconnection in this current sheet, another phenomenon commonly found in high-Lundquist-number reconnection simulations (e.g.,"
] | [
"Uses"
] | [
[
953,
968
]
] | [
[
619,
816
]
] |
2015ApJ...799..149J___2014_Instance_6 | With our joint analysis of stellar mass fraction and source size, we find a larger stellar mass fraction than earlier statistical studies. In Figure 2, we compare our determination of the stellar surface density fraction to a simple theoretical model and to the best fit of a sample of lens galaxies by Oguri et al. (2... | [
"Oguri et al. 2014"
] | [
"Our estimate of the stellar mass fraction agrees",
"and with the estimates from strong lensing studies (see for example",
"which produced stellar mass fractions in the range 30%â70% integrated inside the Einstein radius of the lenses."
] | [
"Similarities",
"Similarities",
"Similarities"
] | [
[
3880,
3898
]
] | [
[
3402,
3450
],
[
3697,
3764
],
[
3900,
4013
]
] |
2021AandA...656A..16C__Bruno_&_Carbone_2013_Instance_4 | Investigations of the turbulent nature of solar wind fluctuations have been ongoing for more than half a century (see, e.g., Bruno & Carbone 2016). Advances have been made consistently thanks to the increasingly accurate measurements of several dedicated space mission as well as to the enormous improvement of numerical... | [
"Bruno & Carbone 2013"
] | [
"In particular, solar wind samples containing more Alfvénic fluctuations are typically associated with less developed turbulence, as inferred from both shallower spectra and reduced intermittency (see",
"and references therein)."
] | [
"Background",
"Background"
] | [
[
2337,
2357
]
] | [
[
2137,
2336
],
[
2359,
2383
]
] |
2021MNRAS.508.2019B__Körding,_Jester_&_Fender_2008_Instance_1 | In the context of AGN models, for SAD-dominated sources the ratio Lradio/$L_{\rm X} \propto \eta _{\rm jet} \, \bar{a}^{2}$ (Yi & Boughn 1999) is expected to be constant and limited to a narrow range of values, as we find for our Seyferts, if the $\bar{a}$ range is finite. Conversely, for LINERs, that are powered by RI... | [
"Körding, Jester & Fender 2008"
] | [
"Conversely, for LINERs, that are powered by RIAF discs, the relation between bolometric AGN and jet power is difficult to model because jet emission can dominate their entire SED"
] | [
"Compare/Contrast"
] | [
[
454,
483
]
] | [
[
274,
452
]
] |
2020MNRAS.498.1480S__Bharadwaj_&_Sethi_2001_Instance_1 | After the recombination epoch, the CMB hardly interacts with the neutral intervening medium. This restricts the CMB from probing the evolution of the structures till the end of EoR. The 21-cm radiation, which is involved in the hyperfine transition of H i, is a promising probe to study the high-redshift universe includ... | [
"Bharadwaj & Sethi 2001"
] | [
"The foregrounds, system noise, and calibration errors together keep the current observations at bay from directly detecting the EoR 21-cm signal. As a consequence, the first detection is likely to be statistical in nature. These observations plan to measure the power spectrum (PS) of the EoR 21-cm signal (e.g."
] | [
"Motivation"
] | [
[
1219,
1241
]
] | [
[
907,
1218
]
] |
2015AandA...584A..75V__Essen_et_al._(2014)_Instance_3 | The data presented here comprise quasi-simultaneous observations during secondary eclipse of WASP-33 b around the V and Y bands. The predicted planet-star flux ratio in the V-band is 0.2 ppt, four times lower than the accuracy of our measurements. Therefore, we can neglect the planet imprint and use this band to measur... | [
"von Essen et al. (2014)"
] | [
"Therefore, during our fitting procedure we use the frequencies determined in",
"as starting values plus their derived errors as Gaussian priors"
] | [
"Uses",
"Uses"
] | [
[
1007,
1030
]
] | [
[
930,
1006
],
[
1031,
1094
]
] |
2019MNRAS.490.5353M__Chen_&_Podsiadlowski_2017_Instance_1 | An independent approach to constrain the strength of magnetic fields in accretion flow models in binary systems is by measuring how much angular momentum is lost from the system via magnetized outflows and estimating the corresponding orbital decay in the system due to magnetic braking. The orbital decay in A0620-00 is... | [
"Chen & Podsiadlowski 2017"
] | [
"Magnetic braking of the system is a possible explanation for the measured $\\dot{P}$, but other explanations, such as resonant interactions between the binary and the possible circumbinary disc, have been proposed"
] | [
"Compare/Contrast"
] | [
[
732,
757
]
] | [
[
518,
730
]
] |
2020MNRAS.492.1295P__Bonning_et_al._2012_Instance_2 | The evolution of colour or the spectral index, α, (F(ν) ∝ ν−α where ν is the radiation frequency and F(ν) is the flux density provides an insight into the particle distribution giving rise to the observed flux density and its variability. In particular, at the synchrotron frequencies, within the simplest scenario of si... | [
"Bonning et al. 2012"
] | [
"while ‘achromatic’ flux variability (no colour evolution,",
"have also been reported."
] | [
"Background",
"Background"
] | [
[
1164,
1183
]
] | [
[
1086,
1143
],
[
1252,
1276
]
] |
2019AandA...630A.131M__Uttley_et_al._2014_Instance_1 | Comptonisation Monte Carlo code (MoCA; see Tamborra et al. 2018 for a detailed description of the code) is based on a single photon approach, working in a fully special relativistic scenario. MoCA allows for various and different physical and geometrical conditions of the accretion disc and of the Comptonising corona. ... | [
"Uttley et al. 2014"
] | [
"Even though arguments (e.g. variability,",
"exist that favour a compact corona, we used extended coronae."
] | [
"Differences",
"Differences"
] | [
[
561,
579
]
] | [
[
520,
560
],
[
709,
770
]
] |
2021AandA...656A..44R__Sérsic_1968_Instance_1 | The detection of LSBGs is usually carried out by a sequence of tasks. The first step is a broad detection of LSBG candidates. Both the depth of the data and the efficiency of this detection in the low-surface-brightness regime will define the completeness of the sample, and so a high efficiency in the detection of diff... | [
"Sérsic 1968"
] | [
"To obtain the structural parameters of the LSBG candidates, the detected sources are usually fitted with a Sérsic model",
"Specific procedures such as GALFIT",
"or IMFIT",
"are used to obtain accurate morphological and structural parameters. However, the computational cost of these is very high, becoming a b... | [
"Compare/Contrast",
"Compare/Contrast",
"Compare/Contrast",
"Compare/Contrast"
] | [
[
913,
924
]
] | [
[
792,
911
],
[
927,
961
],
[
981,
989
],
[
1003,
2035
]
] |
2021ApJ...919...30D__Staguhn_et_al._2014_Instance_1 | The first SMGs were detected using SCUBA at 850 μm (Smail et al. 1997; Barger et al. 1998; Hughes et al. 1998), which remains one of the prime wavelengths to detect these galaxies (e.g., Geach et al. 2017), thanks to a combination of available instruments, spectral window, and the negative k-correction at that waveleng... | [
"Staguhn et al. 2014"
] | [
"Other single-dish samples of SMGs have also been obtained at 1.1–1.3 mm using",
"and at 2 mm with GISMO"
] | [
"Background",
"Background"
] | [
[
606,
625
]
] | [
[
324,
401
],
[
582,
604
]
] |
2018AandA...620A..84B__Hua_et_al._1998_Instance_1 | The PN IC 5148 (PN G002.7-52.4) is a nebula which is to date not well investigated in detail. First listed in the Second Index Catalogue of Nebulae and Clusters of Stars (Dreyer 1910) with two independent entries as numbers IC 5148 and IC 5150 discovered by Swift (1899) and Gale (1897) independently, it was finally dis... | [
"Hua et al. 1998"
] | [
"A few years later the authors searched with a larger field systematically around many nebulae for extended emission features without detecting the very low surface brightness halo we investigate here"
] | [
"Background"
] | [
[
901,
916
]
] | [
[
700,
899
]
] |
2015ApJ...811L..32H__Matthews_1994_Instance_1 | In this Letter, we directly test the relationship between proton kinetic instabilities and plasma turbulence in the solar wind using a hybrid expanding box model that allows us to study self-consistently physical processes at ion scales. In the hybrid expanding box model, a constant solar wind radial velocity vsw is as... | [
"Matthews 1994"
] | [
"The model uses the hybrid approximation where electrons are considered as a massless, charge-neutralizing fluid and ions are described by a particle-in-cell model"
] | [
"Uses"
] | [
[
941,
954
]
] | [
[
777,
939
]
] |
2021MNRAS.502.4858S__Yung_et_al._2020_Instance_1 | One of our main long-term goals is to work towards a full forward modelling pipeline for multiwavelength galaxy surveys. Over the next decade, wide area surveys from DESI, VRO, Euclid, the Nancy Grace Roman Space Telescope, 4MOST, and other facilities will be carried out. We can use the legacy observations from surveys... | [
"Yung et al. 2020"
] | [
"It has been shown elsewhere that these models produce similar results to those of numerical cosmological simulations and other SAMs",
"and that they are also in agreement with higher redshift observations of galaxy populations",
"the reionization history"
] | [
"Similarities",
"Similarities",
"Similarities"
] | [
[
893,
909
]
] | [
[
593,
724
],
[
751,
842
],
[
867,
891
]
] |
2019ApJ...882...65M__Kennicutt_et_al._2003_Instance_1 | Given this correlation between dust luminosity and SFR, it is reasonable to expect the dust mass to scale with SFR as well. In the top panel of Figure 10 we show this relation for our data with the additional parameter of the dust temperature indicated by color. This dust temperature is a weighted average of the temper... | [
"Kennicutt et al. 2003"
] | [
"We also show the Spitzer Infrared Nearby Galaxy Sample",
"analyzed in da Cunha et al. (2008) as purple stars for comparison."
] | [
"Uses",
"Uses"
] | [
[
911,
932
]
] | [
[
855,
909
],
[
934,
1000
]
] |
2015ApJ...806..199B__Balser_et_al._2011_Instance_1 | The most prominent metallicity structure in the Milky Way disk is the decrease of metallicity with increasing Galactic radius—the radial metallicity gradient. All of the major tracers reveal radial gradients, typically with slopes between −0.03 and −0.09
. The radial metallicity gradient can be explained by an in... | [
"Balser et al. 2011"
] | [
"But why is there such a wide range of radial gradient slopes measured? There are several possibilities. (1) Measurement uncertainty. Measurement errors will cause some variations, but it is unlikely to produce a factor of 3 difference in slope. Homogeneity in observing procedures and data analysis may be more impo... | [
"Compare/Contrast"
] | [
[
929,
947
]
] | [
[
466,
888
]
] |
2019ApJ...871..243Y__Saito_et_al._1999_Instance_1 | There are two possibilities resulting in the different magnetic field strengths inferred from the polarimetric and molecular-line observations: (1) the rotational-to-gravitational energy βrot is overestimated, and (2) there are additional contributions in the polarized intensity from other mechanisms, such as dust scat... | [
"Saito et al. 1999"
] | [
"The angular speed was estimated based on the global velocity gradient along the major axis of the dense core observed with single-dish telescopes"
] | [
"Uses"
] | [
[
649,
666
]
] | [
[
502,
647
]
] |
2015AandA...575A.111D__Pinsonneault_et_al._(2001)_Instance_1 | The difference in iron abundance between the two XO-2 stellar components poses an interesting question. They belong to a visual binary and, as normally assumed for such systems, they should share the same origin and initial bulk metallicity. A relevant characteristic of this system is that both of the stars host planet... | [
"Pinsonneault et al. (2001)"
] | [
"Following the results shown in Fig. 2 of",
"we roughly estimated that XO-2N could have ingested an amount of iron slightly higher than 5 M⊕ to increase its photospheric iron content by ~0.05 dex, given its Teff ~ 5300 K."
] | [
"Uses",
"Uses"
] | [
[
1450,
1476
]
] | [
[
1409,
1449
],
[
1478,
1654
]
] |
2017AandA...607A..85L__Zeipel_1924_Instance_1 | The LCs analyses were made using the phoebe v.0.29d software (Prša & Zwitter 2005) that is based on the 2003 version of the Wilson-Devinney (W-D) code (Wilson & Devinney 1971; Wilson 1979, 1990). In the absence of spectroscopic mass ratios, the “q-search” method (for details see Liakos & Niarchos 2012) was applied in m... | [
"von Zeipel 1924"
] | [
"The Albedos, A1 and A2, and gravity darkening coefficients, g1 and g2, were set to generally adopted values for the given spectral types of the components"
] | [
"Uses"
] | [
[
1003,
1018
]
] | [
[
832,
986
]
] |
2015ApJ...800...72T__Kroupa_1995_Instance_1 | The binarity or binary fraction, f, is defined as the ratio of the number of binary or higher-order systems, Nbin, to the total number of systems, Nsys. Here, the term system includes multiple systems and singles (their number being noted as Nsng) as well. Then
6For the star-like population, we apply the binary DPS met... | [
"Kroupa 1995",
"Kroupa 1995"
] | [
"Marks et al. (2014, in preparation) show that random pairing with subsequent dynamical processing does indeed reproduce at least the observed low-mass stellar population (see also",
"This initial binary population is then altered by dynamical evolution. Close binaries with orbital periods below about 10Â days u... | [
"Background",
"Background",
"Background"
] | [
[
1121,
1132
],
[
1472,
1483
]
] | [
[
940,
1120
],
[
1320,
1470
],
[
1485,
1695
]
] |
2016ApJ...822...72C__Mandrini_et_al._2005_Instance_1 | Here, for the first time, we have identified highly dynamic non-potential activity on QS-like supergranular network scales. These events overlie mixed polarity network flux elements near the spatial resolution of HMI, and are the first non-potential structures to be unassociated with strong concentrations of bipolar ma... | [
"Mandrini et al. 2005"
] | [
"Strong non-potential field arcades have been observed in",
"micro-sigmoids in soft X-ray imaging on scales of ∼50″",
"and now at EUV temperatures in QS-like mixed network fields with lengths down to ∼10″. This range of lengths over a range of temperatures and magnetic field topologies points directly to self-s... | [
"Compare/Contrast",
"Compare/Contrast",
"Compare/Contrast"
] | [
[
964,
984
]
] | [
[
739,
795
],
[
908,
962
],
[
1057,
1336
]
] |
2019MNRAS.482.3757B__Rankin_1990_Instance_1 | Subpulse drifting has been a topic of intensive research with the phenomenon expected to be present in 40–50 per cent of the pulsar population. There are around 120 pulsars known at present to exhibit some form of periodic modulations in their single-pulse sequence (Weltevrede et al. 2006, 2007; Basu et al. 2016). The ... | [
"Rankin 1990"
] | [
"A number of detailed studies suggest that the radio emission beam consists of a central core emission surrounded by conal emission arranged in nested rings"
] | [
"Background"
] | [
[
1385,
1396
]
] | [
[
1228,
1383
]
] |
2020ApJ...905..111Z__Jirička_et_al._2001_Instance_1 | Surveys of radio bursts in decimetric wavelengths is presented in papers by Isliker & Benz (1994) and Jirička et al. (2001), within 1–3 GHz and 0.8–2.0 GHz frequency ranges, respectively. Some of these bursts are still not well understood. This is a case of the slowly positively drifting bursts (SPDBs). They appear in ... | [
"Jirička et al. (2001)"
] | [
"Surveys of radio bursts in decimetric wavelengths is presented in papers by Isliker & Benz (1994) and",
"within 1–3 GHz and 0.8–2.0 GHz frequency ranges, respectively."
] | [
"Background",
"Background"
] | [
[
102,
123
]
] | [
[
0,
101
],
[
125,
187
]
] |
2022MNRAS.515.4430M__Iucci_et_al._1979b_Instance_1 | Forbush decreases (FD) are the results of influence of solar wind (SW) large-scale disturbances on the background cosmic ray (CR) flux. They often demonstrate relatively fast CR intensity decrease, accompanied by large and extremely variable CR anisotropy, which is followed by a slower recovery (Forbush 1937; Lockwood ... | [
"Iucci et al. 1979b"
] | [
"FDs caused by high-speed streams (HSS) from coronal holes (CHs) have a recurrent character"
] | [
"Background"
] | [
[
683,
701
]
] | [
[
591,
681
]
] |
2020MNRAS.492.3420B__Hildebrandt_et_al._2018_Instance_1 | Given the potential huge information content of these observables advocated by some recent works (Patton et al. 2017), the predictions from first principles developed in this paper could be successfully applied to forthcoming data along with the standard power spectrum based analysis and could bring additional informat... | [
"Hildebrandt et al. 2018"
] | [
"Let us stress that implementing nulling in weak-lensing analysis is central in order to avoid extracting biased information from the small scales that lack a full theoretical understanding (including due to the effect of baryon physics that needs to be modelled in weak-lensing surveys"
] | [
"Future Work"
] | [
[
720,
743
]
] | [
[
434,
719
]
] |
2019MNRAS.484.1645O__Hummel_et_al._1991_Instance_1 | We justify our use of the Two-Zone approximation as follows: we anticipate that the magnetic structure within the outflow would be perpendicular to the plane of the host galaxy and thus perpendicular to the magnetic field orientation within the Zone B ISM region. Indeed, such perpendicular magnetic structure in outflow... | [
"Hummel et al. 1991"
] | [
"This magnetic structure would also be consistent with polarised radio synchrotron emission above and below the planes of galaxies known to host outflows in the nearby Universe, with the polarisation direction aligned with the orientation of the outflow cone (see, e.g."
] | [
"Similarities"
] | [
[
1014,
1032
]
] | [
[
697,
965
]
] |
2017MNRAS.469.3322G__Narayan_&_Yi_1994_Instance_1 | The induction equation of the magnetic field is
(10)
\begin{equation}
\frac{\partial \boldsymbol {B}}{\partial t}={\nabla }\times \left(\boldsymbol {v}\times \boldsymbol {B}-\frac{4\pi }{c}\eta \boldsymbol {J}\right),
\end{equation}
where $\boldsymbol {J}=\frac{c}{4\pi }{\nabla }\times \boldsymbol {B}$ is the curre... | [
"Narayan & Yi 1994"
] | [
"Also, we consider $Q^{+}_{{\\rm diss}}-Q^{-}_{{\\rm rad}}=fQ^{+}_{{\\rm diss}}$ in ADAFs (where f, the advection parameter, is defined by"
] | [
"Uses"
] | [
[
1153,
1170
]
] | [
[
1018,
1152
]
] |
2020AandA...639A..46B__Štverák_et_al._(2009)_Instance_1 | The linear relationship that we observe between breakpoint energy and core temperature is in line with previous measurements (e.g. McComas et al. 1992; Štverák et al. 2009), for both the halo and strahl. According to Scudder & Olbert (1979), a linear trend in the halo relation also follows under the assumption that bin... | [
"Štverák et al. 2009"
] | [
"The linear relationship that we observe between breakpoint energy and core temperature is in line with previous measurements (e.g.",
"for both the halo and strahl."
] | [
"Similarities",
"Similarities"
] | [
[
152,
171
]
] | [
[
0,
130
],
[
174,
203
]
] |
2018MNRAS.479.4509R__Kingma_&_Ba_2014_Instance_1 | After each step of calculations, the network should optimize the model based on its current and previous states to improve the subsequent mapping. Our model utilizes a computationally memory efficient optimization due to its dependence to only the first-order gradients, namely the ‘adaptive moment estimation’ (or Adam)... | [
"Kingma & Ba (2014)"
] | [
"For more details, we refer the readers to"
] | [
"Background"
] | [
[
364,
382
]
] | [
[
322,
363
]
] |
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"
] | [
"While we know that very massive stars (VMS) above 100 M⊙ exist",
"this mass is significantly diminished via stellar winds already during core hydrogen (H) burning"
] | [
"Background",
"Background"
] | [
[
955,
975
]
] | [
[
751,
814
],
[
857,
953
]
] |
2019AandA...622A.146M__Arribas_et_al._(2014)_Instance_1 | Previous works (e.g. Holt et al. 2011; Arribas et al. 2014; Villar Martín et al. 2014, 2015) have found very high reddening and densities associated with ionised outflows in local objects (e.g. Hα/Hβ ∼ 4.91 and ne ≳ 1000 cm−3, Villar Martín et al. 2014). Concerning the reddening, although we find that the outflowing ga... | [
"Arribas et al. 2014"
] | [
"Previous works",
"have found very high reddening and densities associated with ionised outflows in local objects"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
39,
58
]
] | [
[
0,
14
],
[
93,
187
]
] |
2019AandA...628L...2C__Cukanovaite_et_al._(2018)_Instance_1 | As a final note, we point out that correcting for the effect of neutrinos did not change the finding that KIC 08626021 has a very thin helium-pure layer on top of its envelope. Such a thin layer might be explained by the presence of any mechanism competing against the separation of He, C, and O in the envelopes of DO a... | [
"Cukanovaite et al. (2018)"
] | [
"Perhaps a more likely mechanism is convective overshooting, which was first studied by Freytag et al. (1996) in a white dwarf context and more recently by Tremblay et al. (2015) and",
"through detailed 3D simulations."
] | [
"Background",
"Background"
] | [
[
955,
980
]
] | [
[
773,
954
],
[
981,
1013
]
] |
2018AandA...618A.145O__Brouillet_et_al._2013_Instance_1 | Such a chemical differentiation has been reported in other multiple systems, like the low-mass protostars IRAS16293-2422 (2004a; 2016; 2011) and IRAS4A (Santangelo et al. 2015; López-Sepulcre et al. 2017), and, recently, towards the intermediate-mass protostars NGC 2264 CMM3 (Watanabe et al. 2017). With four examples a... | [
"Brouillet et al. 2013"
] | [
"High-mass star forming regions (HMSFRs) also present a rich chemical diversity. One of the best known examples is provided by Orion-KL. This source harbours: (i) a dichotomy between the spatial distribution of complex O-bearing and complex N-bearing species, with the latter species probing the hotter gas (see,"
] | [
"Background"
] | [
[
1234,
1255
]
] | [
[
829,
1140
]
] |
2015AandA...584A..75V__Essen_et_al._(2014)_Instance_5 | The data presented here comprise quasi-simultaneous observations during secondary eclipse of WASP-33 b around the V and Y bands. The predicted planet-star flux ratio in the V-band is 0.2 ppt, four times lower than the accuracy of our measurements. Therefore, we can neglect the planet imprint and use this band to measur... | [
"von Essen et al. (2014)"
] | [
"The",
"photometric follow-up started in August, 2010, and ended in October, 2012, coinciding with these LBT data."
] | [
"Background",
"Background"
] | [
[
1515,
1538
]
] | [
[
1511,
1514
],
[
1539,
1645
]
] |
2016AandA...588A..25M__Vassiliadis_&_Wood_(1994)_Instance_1 | The faster evolutionary timescales and higher luminosities of our H-burning sequences should have an important impact on the study of the formation of PNe (Schönberner et al. 2014; Toalá & Arthur 2014). The low-mass models of Schönberner (1983), which are still in use to complement the sequences of Blöcker (1995a), sho... | [
"Vassiliadis & Wood (1994)"
] | [
"The discrepancy is even larger in the case of the low-mass models of"
] | [
"Differences"
] | [
[
625,
650
]
] | [
[
556,
624
]
] |
2018MNRAS.481.5630S__Tody_1993_Instance_1 | We also introduce here NB2071 data, taken as part of the MDCS with the Multi-Object Infrared Camera and Spectrograph (MOIRCS; Ichikawa et al. 2006; Suzuki et al. 2008) on the Subaru Telescope (the same instrument that was used in the past MAHALO-Subaru survey; Koyama et al. 2013a). The observations were executed betwee... | [
"Tody 1993"
] | [
"After combining with the existing NB2071 data (186 min integration), we reconstructed all the data using the reduction pipeline mcsred2",
"which is written as iraf3 scripts"
] | [
"Uses",
"Uses"
] | [
[
681,
690
]
] | [
[
488,
623
],
[
646,
679
]
] |
2019AandA...626A..34C__Ohba_et_al._2005_Instance_1 | The uncertainty for most frequency determinations in the spectrum of NEFA is of a few kHz in view of the high S/N of the data (see Fig. 20). However, we have assigned an uncertainty of 10 kHz for all lines showing a single component and intensity larger than 20 mK (S/N ≥ 20). Unlike linear molecules with a nitrogen ato... | [
"Ohba et al. 2005"
] | [
"Using the diagonal elements of the 14N quadrupole coupling tensor in NEFA",
"we have computed the expected hyperfine splitting of all lines in the W band."
] | [
"Uses",
"Uses"
] | [
[
895,
911
]
] | [
[
820,
893
],
[
914,
991
]
] |
2019MNRAS.486.1781R__Gu_et_al._2006_Instance_1 | To check for any spectral variation in the optical/IR bands, we looked for variation in the V − J band colour against the V-band brightness. This colour variation was analysed for the epochs A, B, D, and E. During epochs A and B, the source showed a ‘redder when brighter’ (RWB) behaviour. During epoch E, a bluer when b... | [
"Gu et al. 2006"
] | [
"From studies on the optical–IR colour–magnitude diagram, it is known that FSRQs in general show an RWB trend, which is attributed to them having a luminous accretion disc"
] | [
"Background"
] | [
[
906,
920
]
] | [
[
734,
904
]
] |
2016ApJ...825...10T___2009_Instance_1 | Although this penalty is small, we can still provide a quantitative estimate based on a few assumptions. The observations of M15 that measured the parallax to VLA J2130+12 (K14) employed an interferometric technique where the position of a weaker potential in-beam calibrator source (M15 S1 and VLA J2130+12) can be meas... | [
"Chatterjee et al.",
"2009"
] | [
"Based on a literature review for papers where VLBI parallax measurements were determined using an in-beam calibrator, we find 24 similar measurements, the majority of which have been used to measure parallaxes to pulsars"
] | [
"Uses"
] | [
[
763,
780
],
[
787,
791
]
] | [
[
498,
718
]
] |
2020MNRAS.497.4293G__Ferguson_et_al._2004_Instance_1 | Recently Izotov et al. (2016a,b, 2018a,b) have discovered significant emission of Lyman continuum (LyC) ionizing radiation leaking with the escape fractions of 2–76 per cent in a sample of 11 low-z compact active star-forming galaxies (SFGs) observed with the Hubble Space Telescope (HST) in conjunction with the Cosmic ... | [
"Ferguson et al. 2004"
] | [
"These galaxies hereafter referred to as LyC leakers, possess many properties similar to those of high-redshift galaxies both at z ∼ 2–3 and z$\\gtrsim$ 6 such as compact morphology with similar galaxy radii (e.g."
] | [
"Compare/Contrast"
] | [
[
581,
601
]
] | [
[
348,
559
]
] |
2019AandA...629A..95S___2017a_Instance_1 | A rough idea of the location of the inert Oort cloud can be obtained from previous works. Gladman et al. (2002) showed that the scattering effect by Neptune is significant over long timescales only for perihelion distances below about 45 astronomical units (au). The precise limit actually increases with the semi-major ... | [
"Saillenfest et al.",
"2017a"
] | [
"Later on, Gomes et al. (2005), Gallardo et al. (2012), and",
"showed that the Lidov–Kozai mechanism raised by the giantplanets inside a mean-motion resonance with Neptune is able to raise the perihelion of small bodies beyond 60 au in a few thousands of million years."
] | [
"Background",
"Background"
] | [
[
832,
850
],
[
858,
863
]
] | [
[
773,
831
],
[
866,
1072
]
] |
2021ApJ...908...40M__Muschietti_&_Lembège_2017_Instance_2 | These signatures are inconsistent with ultra-low frequency waves, which have circular polarization and a period similar to the upstream ion gyroperiod. The waves are also inconsistent with ion Weibel instability, which generates linearly polarized waves. Interaction of reflected ions with incoming solar wind electrons ... | [
"Muschietti & Lembège 2017"
] | [
"Since these characteristics are somewhat consistent with model predictions for drift mode of MTSI",
", we do not rule out the possibility of some waves at certain frequencies and during some intervals being generated by the slow drift mode of MTSI."
] | [
"Similarities",
"Similarities"
] | [
[
1922,
1947
]
] | [
[
1823,
1920
],
[
1948,
2095
]
] |
2015AandA...577A.117S__Kaluzny_et_al._(2013a)_Instance_1 | A lower CB frequency in GCs than in the field has already been noticed by Rucinski (2000). It results most likely from a very low binary frequency of ~0.1 in GCs (but with a significant scatter among different clusters), compared to 0.5 in the field (Milone et al. 2012), together with a low percentage of binaries in th... | [
"Kaluzny et al. (2013a)"
] | [
"We used data for two clusters observed by Kaluzny and his collaborators with the highest number of CBs (except for ω Centauri).",
"In M4,",
"detected nine CBs with one BS among them"
] | [
"Uses",
"Background",
"Background"
] | [
[
728,
750
]
] | [
[
593,
720
],
[
721,
727
],
[
751,
791
]
] |
2019AandA...623A.140G__Pohl_et_al._2017_Instance_2 | 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"
] | [
"Polarimetricimages with",
"SPHERE",
"show a gap at around 36 au, with an outer ring at a separation >40 au from the star."
] | [
"Uses",
"Uses",
"Uses"
] | [
[
1269,
1285
]
] | [
[
1150,
1173
],
[
1261,
1267
],
[
1339,
1423
]
] |
2022MNRAS.516.2597S__Padmanabhan_2002_Instance_1 | Observational data from distant Type Ia supernovae (SNIa) revealed a hidden fact that the present Universe is expanding in an accelerated phase (Riess et al. 1998; Perlmutter et al. 1999; Kowalski et al. 2008). This important fact has been confirmed by other cosmological observations such as the cosmic microwave backgr... | [
"Padmanabhan 2002"
] | [
"In this concern, a large family of dynamical DE models with time-varying EoS parameters has been proposed in the literature (for some earlier attemts, see"
] | [
"Background"
] | [
[
2669,
2685
]
] | [
[
2453,
2607
]
] |
2022ApJ...928..120G__Calzetti_et_al._2007_Instance_1 | As part of this study, we investigate the 8 μm emission within our sample of galaxies using archival data from IRAC on the Spitzer Space Telescope (SST). The rest-frame 8 μm emission from galaxies has historically been used as a monochromatic SFR indicator. This is justified by the fact that polycyclic aromatic hydroca... | [
"Calzetti et al. 2007"
] | [
"However, there is an important caveat; PAHs are destroyed by ionizing radiation from newly formed stars",
"leading to a deficit in the 8 μm luminosity in galaxies with low metallicity, whereas PAHs are less well shielded by metals"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
938,
958
]
] | [
[
599,
702
],
[
788,
911
]
] |
2019AandA...631A...5Z__Mink_et_al._(2013)_Instance_1 | Post-main-sequence mergers. Mergers of evolved stars with their MS companions originate from wider systems than main-sequence mergers (log P ≳ 0.7). We thus roughly estimate
f
P
,
i
∼
IPF
0.7
3.0
∼
0.66
$ f_{P , \mathrm{i}} \sim \mathrm{IPF}_{0.7}^{3.0} \sim 0.66 $
, using log10P = 3 as the maximum in... | [
"de Mink et al. (2013)"
] | [
"Extreme mass ratio systems are prone to unstable mass transfer and thus to CEE, and although the exact value of the boundary is not well-constrained, we assume that this occurs for evolved donors in systems with q ≲ 0.4, following previous works such as Wellstein et al. (2001), Hurley et al. (2002) and"
] | [
"Background"
] | [
[
763,
784
]
] | [
[
459,
762
]
] |
2022AandA...661A..10B__Ghirardini_et_al._2021a_Instance_3 | It is also possible that these clusters have a smaller extent and can just be missed by our extent selection as our detection algorithm sets the extent to zero if it is smaller than 6 (Brunner et al. 2022). Following the method presented in Ghirardini et al. (2021a), we estimated several dynamical properties of the clu... | [
"Ghirardini et al. 2021a"
] | [
"In Fig. 5 we compare the distributions of the core radii (Rcore) constrained by the V06 model and the concentration parameter (cSB) between these two samples.",
"The concentration parameter is defined as the ratio of the surface brightness within 0.1 R500 to the surface brightness within R500",
"Intuitively, t... | [
"Compare/Contrast",
"Background",
"Background",
"Compare/Contrast"
] | [
[
735,
758
]
] | [
[
443,
601
],
[
602,
733
],
[
802,
897
],
[
898,
1309
]
] |
2018MNRAS.477.2220T__Miettinen_2014_Instance_1 | We further restricted our sample to well-defined N2H+ (1–0) spectra that we used to estimate the gas velocity dispersion. The N2H+ (1–0) emission of each clump was evaluated from the MALT90 data cubes by averaging the spectrum across all the pixels within one MALT90 beam, ≃ 38 arcsec. We assumed that all the N2H+ emiss... | [
"Miettinen 2014"
] | [
"assuming a mean beam efficiency ηMB = 0.49"
] | [
"Uses"
] | [
[
985,
999
]
] | [
[
941,
983
]
] |
2022ApJ...925..123N__Tielens_&_Charnley_1997_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... | [
"Tielens & Charnley 1997"
] | [
"In space, an analogous process to carbon soot formation occurring on Earth can be initiated through the completion of that first aromatic ring and may also lead to the synthesis of PAHs"
] | [
"Background"
] | [
[
981,
1004
]
] | [
[
794,
979
]
] |
2022MNRAS.515.5135H__Zenteno-Quinteros,_Viñas_&_Moya_2021_Instance_1 | In the present work, we neglect the processes that generate the halo, but this topic deserves some review. Notably, the apparent growth of the halo at the expense of the anti-sunward suprathermal ‘strahl’ population may imply that the halo is locally formed in the inner heliosphere by scattered strahl electrons (e.g. M... | [
"Zenteno-Quinteros, Viñas & Moya 2021"
] | [
"This has led to significant theoretical development, focused on the resonant interaction of electrons with the whistler and fast-magnetosonic whistler (FM/W) modes (e.g.",
"Observations have struggled to confirm these theories."
] | [
"Background",
"Differences"
] | [
[
637,
673
]
] | [
[
365,
534
],
[
729,
783
]
] |
2015ApJ...800...38G___2003_Instance_1 | The currently accepted cold dark matter dominated model with the cosmological constant (ÎCDM) predicts that structures in our Universe assemble hierarchically, with more massive systems forming later through accretion and mergers of smaller, self-bound dark-matter halos (e.g., Tormen 1997; Moore et al. 1999; Klypin e... | [
"Zhao et al. 2003"
] | [
"Moreover, the degree of central concentration of a halo depends on its formation epoch and hence on its total mass (e.g.,"
] | [
"Compare/Contrast"
] | [
[
750,
767
]
] | [
[
605,
726
]
] |
2015MNRAS.453.2126M__Hubrig_et_al._2013_Instance_1 | There are additional lines of evidence suggesting that accretion in HD 100546 could be magnetospheric, and not through a BL. Equation 3 in Johns-Krull, Valenti & Koresko (1999) provides a lower limit to the magnetic field necessary to drive MA, in terms of the stellar parameters and accretion rate. Assuming a mass accr... | [
"Hubrig et al. 2013"
] | [
"This is consistent with the magnetic field measured by Hubrig et al. (2009), 89 ± 26 G, although non detections have also been reported"
] | [
"Similarities"
] | [
[
914,
932
]
] | [
[
757,
892
]
] |
2022AandA...664A...2T__Virtanen_et_al._2017_Instance_1 | The earliest observations of magnetic fields in astrophysics were sunspot field strength measurements at the Mount Wilson Observatory (MWO) in California, USA, in 1908 (Hale 1908). Observations employed the Zeeman effect and were based on measuring the separation (splitting) between the two components of a spectral lin... | [
"Virtanen et al. 2017"
] | [
"In our long-term project aimed at reconstructing the past magnetic activity on the Sun",
"we also use indirect measurements of magnetic fields obtained, in particular, from chromospheric spectroheliograms."
] | [
"Motivation",
"Motivation"
] | [
[
953,
973
]
] | [
[
838,
924
],
[
991,
1106
]
] |
2016ApJ...832..195N__Jin_et_al._2012_Instance_3 | We ignore the density stratification effect in Case I, II, and IIa, because the width of the horizontal current sheet in our simulations is much shorter than the length. The simulation domain extends from x = 0 to x = L0 in the x-direction, and from
y
=
−
0.5
L
0
to
y
=
0.5
L
0
in the y-dire... | [
"Jin et al. 2012"
] | [
"In the work by",
", the maximum of the field strength was found to be 0.15 T. The magnetic field could be even stronger in the active region near the sunspot. Therefore, we set b0 = 0.05 T in Case I and Case II, and b0 = 0.15 T in Case IIa."
] | [
"Uses",
"Uses"
] | [
[
1676,
1691
]
] | [
[
1661,
1675
],
[
1691,
1913
]
] |
2020AandA...635A..47H__Heckman_et_al._2000_Instance_1 | Finally, the multiphase nature of galactic outflows implies that measurements of the outflow properties based on a single gas phase can lead to misleading conclusions (for a discussion, see e.g., Cicone et al. 2018b). Historically, systematic studies of galactic outflows in nearby and high-z galaxies have focused on th... | [
"Heckman et al. 2000"
] | [
"Historically, systematic studies of galactic outflows in nearby and high-z galaxies have focused on",
"and the atomic phase – based on the Na D or Mg II lines in absorption (e.g.,"
] | [
"Background",
"Background"
] | [
[
659,
678
]
] | [
[
218,
317
],
[
582,
658
]
] |
2022ApJ...940...72R__Camilo_et_al._2006_Instance_2 | Several studies have discussed the radio luminosity of GLEAM-X J1627 during its radio outburst in comparison with the limits of its rotational energy (Erkut 2022; Hurley-Walker et al. 2022). In particular, assuming isotropic emission, the radio luminosity of the brightest single peaks (L
radio ∼ 1030–1031 erg s−1; Hurl... | [
"Camilo et al. 2006"
] | [
"Moreover, it is observed that this relationship does not apply to radio-loud magnetars, which in general show larger duty cycles than what one would expect from the extrapolation of this tentative relation for radio pulsars to magnetars (see, e.g.,"
] | [
"Compare/Contrast"
] | [
[
1468,
1486
]
] | [
[
1219,
1467
]
] |
2019AandA...631A..88Y__Bohren_&_Huffman_(1998)_Instance_1 | Starting from the four aforementioned materials, we consider several composition mixtures and grain structures. For the sake of comparison, we first consider compact grains of purely a-Sil, a-C, or a-C:H. Subsequently, according to Köhler et al. (2015), we consider compact grains made of two thirds a-Sil and one third ... | [
"Bohren & Huffman (1998)"
] | [
"To allow fast calculations, we make the major assumption that the grains are spherical and compute their optical properties using the Mie theory",
"with the Fortran 90 version of the BHMIE routine given in"
] | [
"Uses",
"Uses"
] | [
[
1359,
1382
]
] | [
[
1122,
1266
],
[
1301,
1358
]
] |
2022AandA...667A..35R__Nakajima_&_Ouchi_(2014)_Instance_1 | In the optical range, several proxies can serve as indicators of LyC leakage. In particular, line ratios involving ions with different ionization potentials, produced at different depths, have been proposed as indicators to discriminate between radiation-bounded and density-bounded H II regions. Radiation-bounded regio... | [
"Nakajima & Ouchi (2014)"
] | [
"The oxygen line ratio [O III]λ 5007 Å/[O II] λλ3726, 3728 Å (O32) proposed by Jaskot & Oey (2013) and",
"was successfully used to select LyC-leaking candidates"
] | [
"Uses",
"Uses"
] | [
[
808,
831
]
] | [
[
706,
807
],
[
832,
886
]
] |
2020MNRAS.492.4975M__Iben_1967_Instance_1 | We emphasize that 7Be/H remains larger by at least one order of magnitude than predicted by nova models (Starrfield et al. 1978; Hernanz et al. 1996; José & Hernanz 1998). We note, however, that the final amount of 7Be is sensitive to the amount of 3He in the donor star as a higher abundance of 3He is expected to resul... | [
"Iben 1967"
] | [
"From the theoretical point of view, it is believed that low-mass main-sequence stars synthesize 3He through the p–p chains with peak abundances of few 10−3 by number"
] | [
"Background"
] | [
[
1120,
1129
]
] | [
[
953,
1118
]
] |
2022AandA...663A.110M__Tschudi_&_Schmid_2021_Instance_1 | The presented model calculations provide two-dimensional images for the scattered intensity I(x, y), azimuthal polarization Qφ(x, y), and other radiation parameters. It is useful for the comparison with observations to deduce disk-integrated radiation parameters from these model images that are scaled to the stellar in... | [
"Tschudi & Schmid 2021"
] | [
"We note that the measured values must be corrected for instrumental effects, in particular for the signal convolution with the instrumental PSF, which can introduce significant cancellation of the disk signal"
] | [
"Uses"
] | [
[
1202,
1223
]
] | [
[
905,
1113
]
] |
2015MNRAS.453.3414A__Filippenko_&_Chornock_2001_Instance_1 | Filippenko & Chornock (2001) first presented the dynamical estimate of mass of the source to be around 7.4 ± 1.1 M⊙. Recently, Radhika & Nandi (2014) claimed that the mass of XTE J1859+226 is perhaps in between 6.58 and 8.84 M⊙ which is similar to the prediction of Shaposhnikov & Titarchuk (2009), although the lower ma... | [
"Filippenko & Chornock (2001)"
] | [
"first presented the dynamical estimate of mass of the source to be around 7.4 ± 1.1 M⊙."
] | [
"Uses"
] | [
[
0,
28
]
] | [
[
29,
116
]
] |
2022MNRAS.514.5570N__in_1928_Instance_1 | In this study, we examine the stellar populations of NGC 5053 using the UVIT, on-board the AstroSat. NGC 5053 is a galactic GC that lies in the northern constellation of Coma Berenices, having Galactic coordinates l = 335${_{.}^{\circ}}$70, b = 78${_{.}^{\circ}}$95. This cluster is located at a distance of 17.54 ± 0.23... | [
"Baade 1928"
] | [
"It was only in 1928 that Baade first classified it as a GC owing to its high latitude, richness in faint stars and presence of variable stars"
] | [
"Background"
] | [
[
1011,
1021
]
] | [
[
868,
1009
]
] |
2021MNRAS.506.1258W__Borsa_et_al._2021_Instance_1 | Situated in the closest vicinity of their host stars (0.05 AU) and having no counterparts in our Solar system, ultra-hot Jupiters (Arcangeli et al. 2018; Bell & Cowan 2018; Parmentier et al. 2018) are ideal testbeds for studying the impact of 3D effects on high-resolution spectra. There are two important reasons for th... | [
"Borsa et al. 2021"
] | [
"First, ultra-hot Jupiters are accessible objects to observe. Their short orbital periods (1–2 d) and hot, extended atmospheres make them perfect targets for transmission spectroscopy"
] | [
"Motivation"
] | [
[
580,
597
]
] | [
[
324,
506
]
] |
2019MNRAS.482.5651M__Schweizer_&_Middleditch_1980_Instance_2 | Therefore, the kinetics characteristics of the star could be the only piece to judge whether or not the SM star is the surviving companion of SN 1006. If its space velocity is significantly different from the other stars in the remnant of SN 1006, the probability to be the surviving companion would become high. Otherwi... | [
"Schweizer & Middleditch 1980"
] | [
"Based on a radial velocity of $-13\\pm 17\\, {\\rm km^{\\rm -1}}$ and a distance of 2.07 ± 0.18 kpc",
", we can calculate the UVW velocities of the SM star, i. e. $U=-5.2\\pm 14\\, {\\rm km^{\\rm -1}}$, $V=197\\pm 10\\, {\\rm km^{\\rm -1}}$, and $W=3.1\\pm 5\\, {\\rm km^{\\rm -1}}$."
] | [
"Uses",
"Uses"
] | [
[
1876,
1904
]
] | [
[
1779,
1874
],
[
1950,
2118
]
] |
2016MNRAS.463..382U__Zdziarski_et_al._2000_Instance_1 | Active galactic nuclei (AGN) are thought to be powered by an accretion disc around a supermassive black hole, mostly emitting in the optical/ultraviolet (UV) band. According to the standard paradigm, the X-ray emission is due to thermal Comptonization of the soft disc photons in a hot region, the so-called corona (Haar... | [
"Zdziarski et al. 2000"
] | [
"From the application of Comptonization models, such high-energy data allow to constrain the plasma temperature, which is commonly found to range from 50 to 100 keV"
] | [
"Background"
] | [
[
1081,
1102
]
] | [
[
911,
1074
]
] |
2021AandA...650A.205V__Hippke_&_Heller_2019_Instance_1 | To search for transit events, we will make use of our custom pipeline SHERLOCK (Pozuelos et al. 2020)5. This pipeline provides the user with easy access to Kepler, K2, and TESS data for both SC and LC. The pipeline searches for and downloads the pre-search data conditioning simple aperture (PDC-SAP) flux data from the ... | [
"Hippke & Heller 2019"
] | [
"Each of the new detrended light curves, jointly with the nominal PDC-SAP flux, is then processed through the transit least squares (TLS) package",
"in the search for transits.",
"In contrast to the classical box least-squares (BLS) algorithm",
"the TLS algorithm uses an analytical transit model that takes th... | [
"Uses",
"Uses",
"Compare/Contrast",
"Compare/Contrast"
] | [
[
913,
933
]
] | [
[
767,
911
],
[
935,
962
],
[
963,
1025
],
[
1048,
1146
]
] |
2021AandA...647A..49S__Pérez_et_al._2019_Instance_1 | It has been claimed that, for solar-type stars, CA models could face some difficulties (in principle) explaining the presence of giant planets around metal-poor stars, or massive planets at long radial distances (see e.g., Helled et al. 2014). In particular, HR 8799 is a metal-poor A5 star included in our sample, hosti... | [
"Pérez et al. 2019"
] | [
"For the case of β Pictoris and HD 169142, also having giant planets at long distances, CA models seem to be favored"
] | [
"Background"
] | [
[
979,
996
]
] | [
[
815,
930
]
] |
2018MNRAS.473.4130M__Martin_&_Drissen_2016_Instance_1 | The flux calibration was performed from two calibration sources: (1) the spectrum of the spectrophotometric standard star GD71 (Bohlin 2003), obtained in 2016 January, which is used to eliminate as much as possible any strong wavelength dependence; (2) the median combination of a set of 10 images of the standard star H... | [
"Martin & Drissen 2016"
] | [
"The exact value of the interferometer’s modulation efficiency (ME), which acts essentially as an additional throughput loss, is the major source of uncertainty on the absolute flux calibration"
] | [
"Background"
] | [
[
674,
695
]
] | [
[
480,
672
]
] |
2015ApJ...799..149J___2014_Instance_2 | With our joint analysis of stellar mass fraction and source size, we find a larger stellar mass fraction than earlier statistical studies. In Figure 2, we compare our determination of the stellar surface density fraction to a simple theoretical model and to the best fit of a sample of lens galaxies by Oguri et al. (2... | [
"Oguri et al (2014)"
] | [
"We also show as a gray band the best fit for the stellar fraction in the form of stars determined by",
"in a study of a large sample of lens galaxies using strong lensing and photometry,"
] | [
"Uses",
"Uses"
] | [
[
937,
955
]
] | [
[
836,
936
],
[
956,
1038
]
] |
2018MNRAS.475.1160H__Tumlinson_et_al._2013_Instance_1 | Galaxies are surrounded by vast gaseous haloes which extend well beyond the hosts’ stellar components: Early observations of quasar sight lines attributed the presence of absorption at multiple intermittent redshifts to gaseous haloes of intervening galaxies (e.g. Bergeron 1986; Bergeron & Boissé 1991; Lanzetta et al. ... | [
"Tumlinson et al. 2013"
] | [
"In the past decade, owing to the rise of large spectroscopic surveys of galaxies with well-determined physical properties (e.g. SDSS), all sky UV surveys (e.g. GALEX), and improved sensitivity of UV spectrographs (e.g. COS), studies of the gaseous haloes of galaxies could systematically connect gas absorption prop... | [
"Background"
] | [
[
814,
835
]
] | [
[
385,
769
]
] |
2018ApJ...855...26A__Hsu_et_al._2016_Instance_1 | Ever since the initial measurements of the cosmic infrared background (CIB; for a review, see Hauser & Dwek 2001) revealed that the amount of energy radiated in the far-infrared (IR) and submillimeter spectral windows is comparable to that measured at ultraviolet (UV) and optical wavelengths, it has been widely recogni... | [
"Hsu et al. 2016"
] | [
"the number of known SMGs is now of the order of a few thousand (e.g.,",
"and intensive observational efforts have been devoted to understanding their physical properties."
] | [
"Background",
"Background"
] | [
[
2000,
2015
]
] | [
[
1871,
1940
],
[
2037,
2134
]
] |
2022MNRAS.516.3381J__Lindblom_&_Owen_2002_Instance_1 | Studying the dynamical properties of rotating neutron stars is a domain which brings out various interesting features when one assumes a perfect fluid. It is known that the centrifugal force of a rotating star counters gravitational force and hence one can expect massive stars to be fast rotors, at least in the initial... | [
"Lindblom & Owen 2002"
] | [
"Dissipative effects such as shear and bulk viscosities work towards suppressing GR driven instabilities and has been studied by various authors over the past few years"
] | [
"Background"
] | [
[
1136,
1156
]
] | [
[
924,
1091
]
] |
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