adsabs/AstroCLIMB huggingface dataset:
Paper: Gaia 0007–1605: An Old Triple System with an Inner Brown Dwarf–White Dwarf Binary and an Outer White Dwarf Companion
Authors: Alberto Rebassa-Mansergas, Siyi Xu, Roberto Raddi, Anna F. Pala, Enrique Solano, Santiago Torres, Francisco Jiménez-Esteban, and Patricia Cruz
Figure caption: Top panel: the ratio between the brown dwarf’s flux (FBD) and the irradiated flux from the white dwarf on the brown dwarf’s surface (Firr) as a function of orbital period. Bottom panel: the orbital separation as a function of orbital period. The dashed black lines represent the values for 1.0446 days, which is assumed to be the orbital period of Gaia 0007–1605 A,C.
Paper: Magnetocentrifugal Origin for Protostellar Jets Validated through Detection of Radial Flow at the Jet Base
Authors: Chin-Fei Lee, Zhi-Yun Li, Hsien Shang, and Naomi Hirano
Figure caption: The HH 212 jet and model. Panel (a) shows the SiO total intensity map (orange) of the jet within 1400 au of the protostar at 0.″036 × 0.″032 resolution integrated from −16.1 to 17.6 km s−1, with the 350 GHz continuum map (gray; adopted from Lee et al. 2021b) of the dusty disk. They are rotated by 22.°5 clockwise to align the jet axis vertically. The dotted blue curves show the shells previously detected in SO (Lee et al. 2021b). Panel (b) shows the innermost jet within ∼200 au of the protostar, with the nomenclature of the knots from Lee et al. (2017a). Panel (c) shows the PV diagram along the jet axis for the innermost jet, made with a transverse width of 8 au. The contours start at 3σ with a step of 4.5σ, where σ = 5.8 K. The green lines show the FWHM line widths obtained from a Gaussian fit. Panel (d) shows the number density and velocity in our X-wind model, with the dusty disk (dark gray) and shells (light gray), illustrating the increase of the SiO line width of the jet toward the protostar. Here the jet is the densest core of the wind outlined by the gray curves.
Paper: Magnetocentrifugal Origin for Protostellar Jets Validated through Detection of Radial Flow at the Jet Base
Authors: Chin-Fei Lee, Zhi-Yun Li, Hsien Shang, and Naomi Hirano
Figure caption: Jet velocity of HH 212 measured at a distance from ∼40 to 160,000 au. It is derived from the proper motion of the SiO jet measured here from ∼100 to 1000 au (see the Appendix) and those previously reported at other distances along the jet axis (Claussen et al. 1998; Lee et al. 2015; Reipurth et al. 2019). Red and blue data points are for the redshifted and blueshifted jet components, respectively. Since the jet is almost in the plane of the sky, the jet velocity is the same as the proper motion. In panel (b), the data points are shifted to their expected positions at the mean date (2016 November) of the new ALMA observations, assuming ballistic motion.
Paper: Magnetocentrifugal Origin for Protostellar Jets Validated through Detection of Radial Flow at the Jet Base
Authors: Chin-Fei Lee, Zhi-Yun Li, Hsien Shang, and Naomi Hirano
Figure caption: Comparison of the X-wind model and the observations of the HH 212 jet. Panel (a) shows the SiO map of the jet and the 350 GHz continuum map of the disk derived from the model. Panel (b) shows the map of the jet and disk convolved to the observed resolution. Panel (c) shows the observed SiO jet and dusty disk. Panel (d) shows the comparison of the PV structures between the model (red contours) and observations (gray image with black contours). Contour levels are the same as those in Figure 1(c).
Paper: Magnetocentrifugal Origin for Protostellar Jets Validated through Detection of Radial Flow at the Jet Base
Authors: Chin-Fei Lee, Zhi-Yun Li, Hsien Shang, and Naomi Hirano
Figure caption: Comparison of the velocity gradients in the PV structures across the knots in the innermost jet due to jet rotation. The observed PV structures (black contours with gray image) were adopted from Lee et al. (2017a) at 8 au spatial resolution and 1.7 km s−1 velocity resolution. The model PV structures (red contours) are derived from the X-wind model at the same resolutions. The contour levels start at 4σ with a step of 1σ, where σ = 21.3 K.
Paper: Magnetocentrifugal Origin for Protostellar Jets Validated through Detection of Radial Flow at the Jet Base
Authors: Chin-Fei Lee, Zhi-Yun Li, Hsien Shang, and Naomi Hirano
Figure caption: Comparison of the shell and PV structure along the jet axis between the model and observations. The model structure (red dotted curves) and model PV structure (red solid curves) of the shells are derived from an interaction of the X-wind with an extended disk wind. The dotted blue curves outline the shells previously detected in SO (Lee et al. 2021b). The contours start at 3σ with a step of 4.5σ, where σ = 5.8 K.
Paper: Magnetocentrifugal Origin for Protostellar Jets Validated through Detection of Radial Flow at the Jet Base
Authors: Chin-Fei Lee, Zhi-Yun Li, Hsien Shang, and Naomi Hirano
Figure caption: Proper-motion measurement of the SiO jet by comparing the SiO total intensity maps in two epochs at 0.″036 × 0.″032 resolution. The white arrows show the position shifts of the isolated knots and internal shocks (marked with white ellipses) between the two epochs.
Paper: Circumbinary Disk Evolution in the Presence of an Outer Companion Star
Authors: Rebecca G. Martin, Stephen Lepp, Stephen H. Lubow, Matthew A. Kenworthy, Grant M. Kennedy, and David Vallet
Figure caption: Test-particle orbits. Top panel: particle libration and KL timescales. The black line shows the KL timescale given by Equation (4). The blue and red lines show the nodal libration periods given by Equation (2) for aA/aAB = 0.5/15 and aA/aAB = 1/15, respectively. Each point shows a numerical test-particle simulation result. The error bars on the KL periods show the range of values with 10 different starting true anomaly values. The size of the error bars on the libration periods would be smaller than or equal to the size of the points. The lower panels show test-particle stability for a range of initial inclinations. Each pixel consists of 10 simulations that begin with different values of true anomaly.
Paper: Circumbinary Disk Evolution in the Presence of an Outer Companion Star
Authors: Rebecca G. Martin, Stephen Lepp, Stephen H. Lubow, Matthew A. Kenworthy, Grant M. Kennedy, and David Vallet
Figure caption: Hydrodynamical gas-disk simulations for the wide inner binary with aA/aAB = 1/15 and eA = 0.5 with initial disk inclinations of 70° (left) and 60° (right). The blue lines show the inner disk at R = 2 aA, and the red lines show the outer disk at R = (1/3)aAB. The time is in units of the orbital period of the outer companion. From top to bottom, the panels show the disk eccentricity, inclination, longitude of ascending node, and the circumbinary disk mass.
Paper: Circumbinary Disk Evolution in the Presence of an Outer Companion Star
Authors: Rebecca G. Martin, Stephen Lepp, Stephen H. Lubow, Matthew A. Kenworthy, Grant M. Kennedy, and David Vallet
Figure caption: Same as the left panel of Figure 2 except for aA/aAB = 0.5/15.
Paper: Circumbinary Disk Evolution in the Presence of an Outer Companion Star
Authors: Rebecca G. Martin, Stephen Lepp, Stephen H. Lubow, Matthew A. Kenworthy, Grant M. Kennedy, and David Vallet
Figure caption: Close inner binary simulation with aA/aAB = 0.5/15 and eA = 0.5 at times of t = 0, 1.1, 3.4, and 6 PAB from top to bottom. The red circles show the three stars scaled to the size of their sink radius. The left panels show the x−y plane in which both the inner binary and the outer companion orbit. The right panels show the x−z plane. In the final time, the circumbinary disk is perpendicular to the inner binary and the outer companion orbits. The highly eccentric outer parts of the circumbinary disk have transferred material to the outer companion, and it has a low-mass disk.
Paper: Circumbinary Disk Evolution in the Presence of an Outer Companion Star
Authors: Rebecca G. Martin, Stephen Lepp, Stephen H. Lubow, Matthew A. Kenworthy, Grant M. Kennedy, and David Vallet
Figure caption: Analytic estimates for the global precession period around a binary with eccentricity eA = 0.2 (blue line), 0.3 (yellow line), and 0.5 (green line) and the KL oscillation timescale (red line) for a disk with Σ ∝ R−3/2 from Rin = 2.3 aA out to (1/3)aAB. The vertical dashed lines show the values of the semimajor axis ratios used in the SPH simulations (“close inner binary” on the left and “wide inner binary” on the right).
Paper: Stellar Revival and Repeated Flares in Deeply Plunging Tidal Disruption Events
Authors: C. J. Nixon, and Eric R. Coughlin
Figure caption: Debris distributions from the tidal disruption of a solar-like star by a supermassive black hole with β = 16. This simulation is performed with 128 M particles (see Norman et al. 2021 for details). The left panel shows the core-less debris at a time of ∼0.5 days postpericenter, while the right panel shows the debris at a time of ∼5 days with a reformed core near the geometric center. The inset on the right panel shows a zoom-in on the core. The core dominates the local gravity, and contains ≳22% of the mass of the original star.
Paper: Stellar Revival and Repeated Flares in Deeply Plunging Tidal Disruption Events
Authors: C. J. Nixon, and Eric R. Coughlin
Figure caption: The density profiles of the stream corresponding to the times shown in Figure 1. In the left panel we can see that the star has been stretched into a long stream, of length ∼100 R⊙ and the peak density is substantially reduced from that of the original star (∼8 g cm−3). In the right panel we can see that a sharp peak has formed near the stream’s geometric center, corresponding to the reformed core seen in the right panel of Figure 1. The different curves correspond to the resolutions shown in the legend. It is clear that the properties and location of the reformed core do not depend strongly on resolution once a large enough particle number (several million) is reached.
Paper: Stellar Revival and Repeated Flares in Deeply Plunging Tidal Disruption Events
Authors: C. J. Nixon, and Eric R. Coughlin
Figure caption: The temporal evolution of the density of an SPH particle that is within, and near the center of, the reformed core; the left panel is for times very near the time at which the pericenter is reached, whereas the right panel extends to later times. The spike in the left panel coincides with when the star is maximally compressed in the vertical direction, while the first relative maximum in the right panel (around a time of ∼0.2 days) corresponds with the in-plane compression. The core has formed when the density plateaus near a constant value. The different curves are for the resolutions shown in the legend.
Paper: H I Gas Playing Hide-and-seek around a Powerful FRI-type Quasar at z ∼ 2.1
Authors: N. Gupta, R. Srianand, E. Momjian, G. Shukla, F. Combes, J.-K. Krogager, P. Noterdaeme, and P. Petitjean
Figure caption: Top: SALT spectrum of M1540–1453 overlaid with the SDSS template spectrum (magenta) of quasars tilted by λ0.6. The locations of various emission lines are marked, and cyan hashed regions correspond to the CCD gaps. It is evident that while the profiles of the C IV and C III] emission lines roughly follow the template, the Lyα emission is relatively weak and narrow. Bottom left: spectrum around the Lyα emission. The vertical dashed lines show the expected locations of different low-ionization absorption from the H I 21 cm absorber at zabs = 2.1139. The solid blue curve is the predicted spectrum if the H I 21 cm absorber (with N(H I) = 1021.3 cm−2) completely covers the quasar emission. Bottom right: Gaussian fit (magenta curve) to the C IV profile after masking the absorption line features.
Paper: H I Gas Playing Hide-and-seek around a Powerful FRI-type Quasar at z ∼ 2.1
Authors: N. Gupta, R. Srianand, E. Momjian, G. Shukla, F. Combes, J.-K. Krogager, P. Noterdaeme, and P. Petitjean
Figure caption: The VLBA 1.53 GHz image of M1540–1453. The rms noise in the image is 65 μJy beam−1. The restoring beam of 9.0 mas × 3.1 mas with a position angle of +2.°4 is shown as an ellipse at the bottom left corner. The contour levels are 250 × (−2, −1, 1, 2, 4, 8, 16, ...) μJy beam−1. The peak intensity is 6.3 mJy beam−1. The plus sign represents the location of the putative radio core/AGN.
Paper: H I Gas Playing Hide-and-seek around a Powerful FRI-type Quasar at z ∼ 2.1
Authors: N. Gupta, R. Srianand, E. Momjian, G. Shukla, F. Combes, J.-K. Krogager, P. Noterdaeme, and P. Petitjean
Figure caption: Cartoon depicting a quadrant of M1540–1453 embedded in a clumpy ISM. The quasar’s optical sight line (dashed line) may not intercept infalling high-N(H I) clouds. In comparison, extended radio emission (>425 pc) from the lobes will be intercepted by several such clouds, producing the broad redshifted H I 21 cm absorption line. The extent of the H I halo and radio emission could be as large as 10 kpc.
Paper: Solar Toroidal Field Evolution Spanning Four Sunspot Cycles Seen by the Wilcox Solar Observatory, the Solar and Heliospheric Observatory/Michelson Doppler Imager, and the Solar Dynamics Observatory/Helioseismic and Magnetic Imager
Authors: Allison L. Liu, and Philip H. Scherrer
Figure caption: Bl and θ as derived from the solar disk are illustrated in relation to the central meridian and the inclined magnetic field line, B. Br is the radial field. The figure is adapted from Duvall et al. (1979) and Shrauner & Scherrer (1994).
Paper: Solar Toroidal Field Evolution Spanning Four Sunspot Cycles Seen by the Wilcox Solar Observatory, the Solar and Heliospheric Observatory/Michelson Doppler Imager, and the Solar Dynamics Observatory/Helioseismic and Magnetic Imager
Authors: Allison L. Liu, and Philip H. Scherrer
Figure caption: Sin(latitude)–time diagrams of the toroidal fields from WSO (top) and MDI and HMI (middle) data. The temporal profile of the monthly averaged sunspot number is exhibited in the bottom panel. Blue indicates a positive toroidal field in the direction of solar rotation, i.e., westward; red indicates a negative toroidal field in the direction opposite to solar rotation, i.e., eastward.
Paper: Solar Toroidal Field Evolution Spanning Four Sunspot Cycles Seen by the Wilcox Solar Observatory, the Solar and Heliospheric Observatory/Michelson Doppler Imager, and the Solar Dynamics Observatory/Helioseismic and Magnetic Imager
Authors: Allison L. Liu, and Philip H. Scherrer
Figure caption: Temporal profiles of toroidal fields at different latitudes for the northern (top) and southern hemispheres (bottom). The irregular, jagged curves with different colors refer to the calculated toroidal fields at different latitudes. The smoothed thicker curves represent the 11th order polynomial functions fitted to the toroidal fields.
Paper: Solar Toroidal Field Evolution Spanning Four Sunspot Cycles Seen by the Wilcox Solar Observatory, the Solar and Heliospheric Observatory/Michelson Doppler Imager, and the Solar Dynamics Observatory/Helioseismic and Magnetic Imager
Authors: Allison L. Liu, and Philip H. Scherrer
Figure caption: Sin(latitude)–time diagrams of the toroidal fields from MDI data. Top: sin(latitude)–time diagram from all the data. Middle: sin(latitude)–time diagram from upside-up data only. Bottom: sin(latitude)–time diagram from upside-down data only. The pattern becomes much clearer when only upside-up data are used (middle panel) while there is no clear pattern in the upside-down map (bottom panel).
Paper: Revisiting the Rates and Demographics of Tidal Disruption Events: Effects of the Disk Formation Efficiency
Authors: Thomas Hong Tsun Wong, Hugo Pfister, and Lixin Dai
Figure caption: The host MBH distribution of the observed TDE candidates compared to the intrinsic distribution from the LC theory. The solid lines represent our chosen observed TDE candidates, while the colors indicate the methods used to constrain MBH (orange: MBH−σ; blue: MBH−Mgal). Similar to the bootstrapping method, the error bars of individual TDEs are modeled as a Gaussian distribution with the scattering from the MBH-scaling relations and the measurement errors from σ and Mgal. Both observed TDE MBH distributions center around 106–107 M⊙, while the intrinsic TDE MBH distribution derived from the LC dynamics (black dashed curve) peaks toward lighter BHs. The small peak of the orange curve at 108−109 M⊙ is due to a single event ASASSN-15lh.
Paper: Revisiting the Rates and Demographics of Tidal Disruption Events: Effects of the Disk Formation Efficiency
Authors: Thomas Hong Tsun Wong, Hugo Pfister, and Lixin Dai
Figure caption: Comparison between the intrinsic and ﹩{ \mathcal C }﹩-corrected differential TDE rates. For MBH/M⊙ = {104, 106, 108} (top, middle, and bottom rows), the intrinsic and corrected differential TDE rates are shown in the left and right panels, respectively. The white regions represent the parameter space where stars directly plunge into the BH event horizon. Contours of disk formation efficiencies ﹩{ \mathcal C }﹩ are overplotted in the left panels. ﹩{ \mathcal C }﹩ has a monotonically increasing trend toward the upper-left corner (higher β and lower m⋆). One can see that the ﹩{ \mathcal C }﹩-correction leads to a significant drop in TDE rates at low β for lighter BHs. For MBH = 108 M⊙, ﹩{ \mathcal C }\approx 1﹩ across the TDE-allowed parameter space.
Paper: Revisiting the Rates and Demographics of Tidal Disruption Events: Effects of the Disk Formation Efficiency
Authors: Thomas Hong Tsun Wong, Hugo Pfister, and Lixin Dai
Figure caption: The intrinsic and ﹩{ \mathcal C }﹩-corrected volumetric TDE rates and MBH distributions. Panel (a) shows the TDE volumetric rates as a function of MBH, with different ways of implementing the disk formation efficiency correction. Panel (b) shows how the value of ﹩{{ \mathcal C }}_{\mathrm{thres}}﹩ affects the TDE MBH distribution. The intrinsic and observed distributions (orange dotted: MBH−σ), same as in Figure 1, are included for comparison. The distribution with ﹩{{ \mathcal C }}_{\mathrm{thres}}=0.1﹩ (red solid) best replicates the median of the observed TDE samples. Overall, the rate suppression around light SMBHs due to slow disk formation is evident in both plots.
Paper: Revisiting the Rates and Demographics of Tidal Disruption Events: Effects of the Disk Formation Efficiency
Authors: Thomas Hong Tsun Wong, Hugo Pfister, and Lixin Dai
Figure caption: Numerical and empirically fitted β-distributions derived from intrinsic and ﹩{ \mathcal C }﹩-corrected TDE rates. Different colors indicate different MBH = 104 M⊙(blue), 106 M⊙(green), 108 M⊙(red). In panels (a) and (b), empirical fitting formulae of Equations (12a) and (12b) are plotted in dashed lines with their corresponding numerical results in solid lines. In panel (c), two different ﹩{{ \mathcal C }}_{\mathrm{thres}}=0.1(\mathrm{dashed})﹩ and 0.5 (dotted) are included.
Paper: Revisiting the Rates and Demographics of Tidal Disruption Events: Effects of the Disk Formation Efficiency
Authors: Thomas Hong Tsun Wong, Hugo Pfister, and Lixin Dai
Figure caption: The stellar-mass probability density functions in TDEs before and after the correction with ﹩{ \mathcal C }﹩. For four distinct MBH = 104 M⊙ (blue), 106 M⊙ (green), 107 M⊙ (orange), and 108 M⊙ (red), we show the intrinsic (solid), ﹩{ \mathcal C }﹩-corrected (dashed), and ﹩{{ \mathcal C }}_{\mathrm{thres}}=0.1﹩ case (dotted) stellar-mass distributions in TDEs. The Kroupa initial mass function is plotted for comparison (gray solid). Low-mass stars have a lower intrinsic presentation in TDEs due to a combination of the LC physics as well as their direct plunge when MBH is large. For TDEs with MBH ≳ 108 M⊙, there exists a cutoff of low-mass stars. For TDEs with MBH ≲ 106 M⊙, the ﹩{ \mathcal C }﹩-correction can overcompensate for the suppression of low-mass stars.
Paper: Revisiting the Rates and Demographics of Tidal Disruption Events: Effects of the Disk Formation Efficiency
Authors: Thomas Hong Tsun Wong, Hugo Pfister, and Lixin Dai
Figure caption: TDE host MBH distribution for X-ray-strong or optical/UV-strong TDEs. The two colored curves in Figure 1 are further decomposed into two groups: optical/UV strong (magenta) or X-ray strong (green). The optical/UV TDE MBH distribution still peaks somewhere between 106 and 107M⊙, while that of the X-ray TDEs exhibits a double peak behavior.
Paper: Revisiting the Rates and Demographics of Tidal Disruption Events: Effects of the Disk Formation Efficiency
Authors: Thomas Hong Tsun Wong, Hugo Pfister, and Lixin Dai
Figure caption: TDE peak luminosity Lbb,peak vs. MBH from Table A1 (modified from Figure 16 Hung et al. 2017). The optical/UV-strong TDEs are marked by magenta dots and the X-ray strong by green crosses, with the horizontal line showing the error bar of MBH. The dashed lines correspond to four different Eddington ratios, while the dotted line shows the ﹩{\dot{M}}_{\mathrm{peak}}\propto {M}_{\mathrm{BH}}^{-1/2}﹩ proportionality relation derived in Guillochon & Ramirez-Ruiz (2013), their Equation (A1), with m⋆ = 1M⊙, γ = 4/3, β = 1, and radiative efficiency η = 0.1. We find here that some TDEs have peak luminosity exceeding the Eddington limits of their host SMBHs: ASASSN-14ae, ASASSN-15lh, ASASSN-15oi, ASASSN-19dj, AT 2018hyz, AT 2018lna, AT 2019meg, PS1-10jh, and SDSS J1323–4827. Overall, no apparent correlation is found between Lbb,peak and MBH.
Paper: Revisiting the Rates and Demographics of Tidal Disruption Events: Effects of the Disk Formation Efficiency
Authors: Thomas Hong Tsun Wong, Hugo Pfister, and Lixin Dai
Figure caption: Regenerated Figure 3 using the 95% confidence regions of the BHMF in Figure 2 in Gallo & Sesana (2019). The upper (lower) panel corresponds to using the BHMF’s upper (lower) margin in the light yellow areas of Gallo & Sesana (2019) Figure 2. The distributions with ﹩{{ \mathcal C }}_{\mathrm{thres}}=0.1﹩ (red solid) still best replicate the median of the observed TDE samples. The rate suppression around light SMBHs due to slow disk formation is more dominant than that by the lower 2σ of the unconstrained BHMF.
Paper: Periodic Oscillations in LASCO Coronal Mass Ejection Speeds: Space Seismology
Authors: Grzegorz Michalek, Nat Gopalswamy, and Seiji Yashiro
Figure caption: Examples of fitted curves (dashed lines) to speed–distance/time profiles for two CMEs. The left panels show a CME on 2004 February 11, and the right panels show a CME on 2004 February 8, respectively. The upper panels display speed–distance profiles and the lower panels speed–time profiles. In the case of the first CME (left panels), we observe a clear speed oscillation with an amplitude of about 250 m s−1. The other CME (right panels) shows no speed oscillation. In this case, the best fit is a linear function. Error bars show the minimum speed error for the C2 and C3 instruments.
Paper: Periodic Oscillations in LASCO Coronal Mass Ejection Speeds: Space Seismology
Authors: Grzegorz Michalek, Nat Gopalswamy, and Seiji Yashiro
Figure caption: Distributions of the most important attributes of speed oscillations (left panels, a–d) and CMEs revealing these oscillations (right panels, e–h). In the left panels are the distributions of (a) the amplitude of oscillation (parameter a0), (b) spatial period of oscillation (obtained from time period oscillation), (c) time period of oscillation (parameter a1), and (d) acceleration (parameter a4). Basic statistics (mean, median, and standard deviation) are reported at the top of the panels. In the right panels are the distributions of (e) speed, (f) width, (g) absolute latitude, and (h) acceleration of CMEs revealing speed oscillations. The fraction is the ratio of the number of CMEs with the given parameters falling within the ranges under consideration to all CMEs with an oscillation pattern.
Paper: Periodic Oscillations in LASCO Coronal Mass Ejection Speeds: Space Seismology
Authors: Grzegorz Michalek, Nat Gopalswamy, and Seiji Yashiro
Figure caption: Temporal evolution of the occurrence rate of CMEs showing an oscillation pattern: (a) the absolute and (b) fractional occurrence rates (the ratio of CMEs with an oscillation pattern to the total number of CMEs in a given period of time).