adsabs/AstroCLIMB huggingface dataset:
Paper: Mapping the Complex Kinematic Substructure in the TW Hya Disk
Authors: Richard Teague, Jaehan Bae, Sean M. Andrews, Myriam Benisty, Edwin A. Bergin, Stefano Facchini, Jane Huang, Cristiano Longarini, David Wilner
Figure caption: Comparison of the archival 233 GHz continuum from Macías et al. (2021) and the velocity-integrated intensity (zeroth-moment) maps of CO and CS, shown in panels (a), (b), and (c), respectively. Note that the CO data has a “square-root” stretch applied in order to bring out the morphology. In each panel, the synthesized beam is shown in the lower left and a 100 au scale bar in the lower right. The right-most panel, (d), shows the azimuthally averaged radial profiles of the CO and CS emission. The shaded regions show uncertainties in steps of 1σ.
Paper: Mapping the Complex Kinematic Substructure in the TW Hya Disk
Authors: Richard Teague, Jaehan Bae, Sean M. Andrews, Myriam Benisty, Edwin A. Bergin, Stefano Facchini, Jane Huang, Cristiano Longarini, David Wilner
Figure caption: CO (2–1) channel maps, imaged at 40 m s−1 spacing. The beam size is shown in the bottom left of the panels. The channel velocity is shown in the top left of each panel. Each panel spans ±4.″5 (±270 au) across. Note that the color scaling has been adjusted to bring out the detail in the line wings, and the peak intensity is 176.4 mJy beam−1.
Paper: Mapping the Complex Kinematic Substructure in the TW Hya Disk
Authors: Richard Teague, Jaehan Bae, Sean M. Andrews, Myriam Benisty, Edwin A. Bergin, Stefano Facchini, Jane Huang, Cristiano Longarini, David Wilner
Figure caption: CS (5–4) channel maps, imaged at 40 m s−1 spacing. The beam size is shown in the bottom left of the panels, and the channel velocity is shown in the top left of each panel. Each panel spans ±4.″5 (±270 au) across. Note that the color scaling has been adjusted to bring out the detail in the line wings. The peak intensity is 26.4 mJy beam−1.
Paper: Kepler and TESS Observations of PG 1159-035
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, Alejandro H. Córsico, J. E. S. Costa, J. J. Hermes, S. D. Kawaler, Keaton J. Bell, M. H. Montgomery, J. L. Provencal, D. E. Winget, G. Handler, Bart Dunlap, J. C. Clemens, Murat Uzundag
Figure caption: Location of the known GW Vir variable stars in the ﹩\mathrm{log}{T}_{\mathrm{eff}}\mbox{--}\mathrm{log}g﹩ diagram, depicted with small red circles. Thin solid curves show the post-born-again evolutionary tracks from Althaus et al. (2005) and Miller Bertolami & Althaus (2006) for different stellar masses in the range 0.530–0.741M ⊙. The location of the GW Vir stars observed with TESS (with published results) are emphasized with large orange circles. PG 1159−035 is displayed with a small blue circle with the error bars (within a box with dotted lines), according to Werner et al. (2011; T eff = 140, 000 ± 5000 K and ﹩\mathrm{log}g=7\pm 0.5﹩). The location of PG 1159−035 according to the asteroseismic model (see Section 11.3) is depicted with a black, small circle. The violet curves divide the plane into three regions: one in which all of the g modes have ﹩\dot{{\rm{\Pi }}}\lt 0﹩, another region where some modes have ﹩\dot{{\rm{\Pi }}}\lt 0﹩ and others have ﹩\dot{{\rm{\Pi }}}\gt 0﹩, and finally a region in which all of the modes have ﹩\dot{{\rm{\Pi }}}\gt 0﹩. The gray curves correspond to the theoretical blue edge of the GW Vir instability strip for ℓ = 1 and ℓ = 2 g modes, according to Córsico et al. (2006).
Paper: Kepler and TESS Observations of PG 1159-035
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, Alejandro H. Córsico, J. E. S. Costa, J. J. Hermes, S. D. Kawaler, Keaton J. Bell, M. H. Montgomery, J. L. Provencal, D. E. Winget, G. Handler, Bart Dunlap, J. C. Clemens, Murat Uzundag
Figure caption: The quality function of the period fit in terms of the effective temperature for the PG 1159 sequences with different stellar masses (in solar units), indicated at the left-bottom corner of each panel. Black (red) lines correspond to stages before (after) the ”evolutionary knee” (see Figure 19). Only the periods with m = 0 (see Tables 2 and 3) have been considered. There is a strong minimum in panel (c), marked with an arrow, corresponding to a model with M ⋆ = 0.565M ⊙ and T eff ≃ 129, 600 K. Panel (h) is a zoom of the region with the strong minimum seen in panel (c); the y-axis scale is linear in this case. The vertical dashed line is the spectroscopic T eff of PG 1159−035 (140 kK), and the gray zone depicts its 1σ uncertainty (±5 kK).
Paper: Kepler and TESS Observations of PG 1159-035
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, Alejandro H. Córsico, J. E. S. Costa, J. J. Hermes, S. D. Kawaler, Keaton J. Bell, M. H. Montgomery, J. L. Provencal, D. E. Winget, G. Handler, Bart Dunlap, J. C. Clemens, Murat Uzundag
Figure caption: Upper panel: dipole (ℓ = 1) average of the computed period spacings, ﹩\overline{{\rm{\Delta }}{{\rm{\Pi }}}_{k}}﹩, assessed in a range of periods that includes the periods observed in PG 1159−035, shown as dashed red (solid black) curves corresponding to stages before (after) the maximum T eff for different stellar masses. The location of PG 1159−035 when we use the effective temperature derived by Werner et al. (2011), T eff = 140, 000 ± 5000 K, and the period spacing ΔΠ1 = 21.28 ± 0.02 s derived in Section 6, is highlighted with a blue circle. Lower panel: same as in upper panel, but for the case in which the period spacing is assumed to be associated with ℓ = 2 modes (ΔΠ2 = 13.02 ± 0.04 s).
Paper: Kepler and TESS Observations of PG 1159-035
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, Alejandro H. Córsico, J. E. S. Costa, J. J. Hermes, S. D. Kawaler, Keaton J. Bell, M. H. Montgomery, J. L. Provencal, D. E. Winget, G. Handler, Bart Dunlap, J. C. Clemens, Murat Uzundag
Figure caption: Schematic distribution of the ℓ = 1 and ℓ = 2 (m = 0) pulsation periods of PG 1159−035 observed by K2 (black lines, upper panels), observed by Costa et al. (2008; CEA08, blue lines, middle panels), and observed by Winget et al. (1991; WEA91, red lines, lower panels). At least 14 additional ℓ = 1 modes only detected by K2 at periods longer than 1000 s have been cut off and not shown here, but are detailed in Table 2. The amplitudes have been arbitrarily set to one for clarity.
Paper: Kepler and TESS Observations of PG 1159-035
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, Alejandro H. Córsico, J. E. S. Costa, J. J. Hermes, S. D. Kawaler, Keaton J. Bell, M. H. Montgomery, J. L. Provencal, D. E. Winget, G. Handler, Bart Dunlap, J. C. Clemens, Murat Uzundag
Figure caption: The observed multiplet splittings for 23 ℓ = 1 and 9 ℓ = 2 modes (we do not plot the singlets) centered on the m = 0 component. The k number for each mode is indicated on the right. The dashed and dotted lines indicate the frequency splittings if the star rotates as a rigid body with frequency Ωrot = 8.16 μHz. The width and color of the boxes correspond, respectively, to the uncertainty and the amplitude of the frequencies: the darker the color, the higher the amplitude.
Paper: Kepler and TESS Observations of PG 1159-035
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, Alejandro H. Córsico, J. E. S. Costa, J. J. Hermes, S. D. Kawaler, Keaton J. Bell, M. H. Montgomery, J. L. Provencal, D. E. Winget, G. Handler, Bart Dunlap, J. C. Clemens, Murat Uzundag
Figure caption: Relative change of pulsation period with time ﹩\tfrac{\dot{{\rm{\Pi }}}}{{\rm{\Pi }}}﹩ over time to k = 17, k = 20, k = 21, and k = 22 modes. The error bars were calculated by MCMC simulation.
Paper: Kepler and TESS Observations of PG 1159-035
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, Alejandro H. Córsico, J. E. S. Costa, J. J. Hermes, S. D. Kawaler, Keaton J. Bell, M. H. Montgomery, J. L. Provencal, D. E. Winget, G. Handler, Bart Dunlap, J. C. Clemens, Murat Uzundag
Figure caption: Observed Ledoux rotation coefficients C(ℓ, k) (red) vs. the predicted ones (black) in the best asteroseismic model, in terms of the periods. The horizontal dotted line corresponding to C(ℓ, k) = 0.5 is the asymptotic value for large radial-order modes. If Ωrot = 8.38 μHz, all values are larger than the model ones.
Paper: Kepler and TESS Observations of PG 1159-035
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, Alejandro H. Córsico, J. E. S. Costa, J. J. Hermes, S. D. Kawaler, Keaton J. Bell, M. H. Montgomery, J. L. Provencal, D. E. Winget, G. Handler, Bart Dunlap, J. C. Clemens, Murat Uzundag
Figure caption: Expected value of R c (Equation (11)) as a function of T eff for observations centered on λ = 5500 Å. A blackbody spectrum was assumed for this calculation.
Paper: Kepler and TESS Observations of PG 1159-035
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, Alejandro H. Córsico, J. E. S. Costa, J. J. Hermes, S. D. Kawaler, Keaton J. Bell, M. H. Montgomery, J. L. Provencal, D. E. Winget, G. Handler, Bart Dunlap, J. C. Clemens, Murat Uzundag
Figure caption: How far each δ ν 1 is from the median value, ﹩\overline{\delta {\nu }_{1}}﹩, calculated separately for frequency spacings between m = −1 and m = 0 modes (red points) and for frequency spacings between m = 0 and m = 1 modes (blue points).
Paper: Two-dimensional Configuration and Temporal Evolution of Spark Discharges in Pulsars
Authors: Rahul Basu, George I. Melikidze, Dipanjan Mitra
Figure caption: (a) The upper panel shows a schematic of the evolution of the spark pattern along the polar cap boundary due to the drifting of the sparks. The black curved line is the boundary of the polar cap where two sparks (red circles) develop around a maximally heated point (red dot) on the boundary. The sparks drift by a distance h  s  during their lifetimes as they lag behind the corotation direction. The maximally heated point (open black circle) at the end of the spark process shifts by a distance h  D  due to the drifting of the sparks. After the surface cools down subsequent sparks are formed around the shifted point (open black circle) resulting in a shift of the spark pattern. (b) The lower panel shows a schematic of the elliptical polar cap with major axis a cap, minor axis b cap, and inclined at an angle θ cap in the x–y plane. The spatial shift h  D  along the boundary of the polar cap at a point specified by the polar angle θ PC corresponds to the angular shift θ sft.
Paper: Two-dimensional Configuration and Temporal Evolution of Spark Discharges in Pulsars
Authors: Rahul Basu, George I. Melikidze, Dipanjan Mitra
Figure caption: Angular shift in the spark pattern around the entire boundary of the polar cap (θ PC). Panels (a) and (b) represent circular polar caps where the sparks lag behind the corotation direction along the x-axis in case (a), while the sparks lag behind corotation along an axis, which makes a 45° angle in the x–y plane in case of (b). Panels (c) and (d) show examples of elliptical polar caps with eccentricity 0.6 and sparks lagging behind along the x-axis in both cases. In panel (c) the major axis is oriented along the x-axis while in panel (d) the major axis is oriented along the y-axis.
Paper: Two-dimensional Configuration and Temporal Evolution of Spark Discharges in Pulsars
Authors: Rahul Basu, George I. Melikidze, Dipanjan Mitra
Figure caption: Single pulse simulations demonstrating the phase stationary drifting. (a) Pulse stack with 128 simulated single pulses. There are five components in the average profile and the central core does not exhibit any periodicity. (b) LRFS across the pulse window. The drifting periodicity, P 3 = 9.7P is seen as a peak frequency, f  p  ∼ 0.1 cycles/P. The time evolution of the spark pattern is reflected in the phase behavior across the profile (top window).
Paper: Two-dimensional Configuration and Temporal Evolution of Spark Discharges in Pulsars
Authors: Rahul Basu, George I. Melikidze, Dipanjan Mitra
Figure caption: Single pulse simulations demonstrating the coherent subpulse drifting. (a) Pulse stack with 128 simulated single pulses and (b) LRFS across the pulse window. The drifting periodicity, P 3 = 4.9P, is seen as a peak frequency, f  p  ∼ 0.2 cycles/P. The time evolution of the spark pattern is reflected in the phase behavior across the profile (top window).
Paper: Overview of the Remote Sensing Observations from PSP Solar Encounter 10 with Perihelion at 13.3 R ⊙ 
Authors: Russell A. Howard, Guillermo Stenborg, Angelos Vourlidas, Brendan M. Gallagher, Mark G. Linton, Phillip Hess, Nathan B. Rich, Paulett C. Liewer
Figure caption: Top three panels: j-maps along the three radial directions in the WISPR-I FOV indicated in Figure 2. The inclined features reveal the outward flow of plasma, with the curved tracks indicating the existence of acceleration (or deceleration) relative to the S/C. Bottom panel: lat-map for slit at column #320, which covers elongations (HPLN-ZPN) between ∼21.0° and ∼28.2° depending on the date and position along the slit (i.e., latitude HPLT-ZPN; see the top panels of Figure 1 and Figure 2). The projection of the solar equatorial plane is at zero degrees. The start of each day (vertical dashed lines) and the corresponding S/C heliocentric distance in R ⊙ are indicated at the top of each panel. The wide, vertical feature at the end of November 18 is an artifact due to a 4 hr data gap in the synoptic observing program.
Paper: Overview of the Remote Sensing Observations from PSP Solar Encounter 10 with Perihelion at 13.3 R ⊙ 
Authors: Russell A. Howard, Guillermo Stenborg, Angelos Vourlidas, Brendan M. Gallagher, Mark G. Linton, Phillip Hess, Nathan B. Rich, Paulett C. Liewer
Figure caption: Top row: FOV of the WISPR telescopes. The grid depicts the fixed angular FOV in HPC coordinates for the perihelion date in orbit 10. The HPC coordinate grid reveals the roll of each instrument frame, as well as the optical distortion on the detector. Bottom left: exposure times (ET) during the synoptic observing program in E10. The ET during the inbound and outbound segments (both telescopes) of the encounter have a similar profile. The increase of the ET for WISPR-I below 0.157 au is due to the different gain setting used for the WISPR-I images below that S/C distance. Bottom right: top-down view of the TS at the start of the science encounter (black dashed circle) and at perihelion (blue dashed circle) of orbit 10. The two positions of PSP are depicted by the black and blue circles, respectively. The Sun is represented by the yellow circle at [0,0]. The orbits of Mercury and PSP are marked with the black and blue solid lines, respectively.
Paper: Overview of the Remote Sensing Observations from PSP Solar Encounter 10 with Perihelion at 13.3 R ⊙ 
Authors: Russell A. Howard, Guillermo Stenborg, Angelos Vourlidas, Brendan M. Gallagher, Mark G. Linton, Phillip Hess, Nathan B. Rich, Paulett C. Liewer
Figure caption: Coronal activity on 2021 November 19 recorded by WISPR-I at three different time instances. Top row: LW-processed snapshots. Bottom row: LT-processed snapshots. For details see Section 3.2.
Paper: Overview of the Remote Sensing Observations from PSP Solar Encounter 10 with Perihelion at 13.3 R ⊙ 
Authors: Russell A. Howard, Guillermo Stenborg, Angelos Vourlidas, Brendan M. Gallagher, Mark G. Linton, Phillip Hess, Nathan B. Rich, Paulett C. Liewer
Figure caption: WISPR-I/WISPR-O composite of the main event on 2021 November 19 at two time instances. The images have been projected onto the HPC grid to show the physical FOVs of both detectors together. The curvature of the images is due to a combination of the optical distortion of the lens and the spherical basis of the coordinate system.
Paper: Overview of the Remote Sensing Observations from PSP Solar Encounter 10 with Perihelion at 13.3 R ⊙ 
Authors: Russell A. Howard, Guillermo Stenborg, Angelos Vourlidas, Brendan M. Gallagher, Mark G. Linton, Phillip Hess, Nathan B. Rich, Paulett C. Liewer
Figure caption: Coronal activity on 2021 November 20 recorded by WISPR-I at three different time instances. Top row: LW-processed snapshots. Bottom row: LT-processed snapshots. For details see Section 3.3.
Paper: Overview of the Remote Sensing Observations from PSP Solar Encounter 10 with Perihelion at 13.3 R ⊙ 
Authors: Russell A. Howard, Guillermo Stenborg, Angelos Vourlidas, Brendan M. Gallagher, Mark G. Linton, Phillip Hess, Nathan B. Rich, Paulett C. Liewer
Figure caption: STEREO-A COR2 snapshots of the November 19 event observed by WISPR (see Figure 5).
Paper: Overview of the Remote Sensing Observations from PSP Solar Encounter 10 with Perihelion at 13.3 R ⊙ 
Authors: Russell A. Howard, Guillermo Stenborg, Angelos Vourlidas, Brendan M. Gallagher, Mark G. Linton, Phillip Hess, Nathan B. Rich, Paulett C. Liewer
Figure caption: Slits for the height−time and latitude−time maps shown in Figure 3 in a WISPR detector frame. The three radial slits were placed to encompass the FOV and capture the three regions where most of the activity was occurring (they converge at the Sun’s center). The vertical slit is intended to capture the latitudinal extent of the coronal transients, as well as the latitudinal evolution of pseudostationary structures in the FOV, e.g., streamers.
Paper: Overview of the Remote Sensing Observations from PSP Solar Encounter 10 with Perihelion at 13.3 R ⊙ 
Authors: Russell A. Howard, Guillermo Stenborg, Angelos Vourlidas, Brendan M. Gallagher, Mark G. Linton, Phillip Hess, Nathan B. Rich, Paulett C. Liewer
Figure caption: Development in the upper half of the WISPR-I FOV of a small CME on 2021 November 16. The axis labels are given in pixels and are intended to indicate explicitly the portion of the images selected for display.
Paper: Insight-HXMT Observation of 4U 1608–52: Evidence of Interplay between a Thermonuclear Burst and Accretion Environment
Authors: Yu-Peng Chen, Shu Zhang, Long Ji, Shuang-Nan Zhang, Ling-Da Kong, Peng-Ju Wang, Zhi Chang, Jing-Qiang Peng, Jin-Lu Qu, Jian Li
Figure caption: Spectral fitting result of the burst with time bin 0.25 s with a pure blackbody model (black), f  a  model (the left panel, red), and convolution thermal-Comptonization model (the right panel, red), including the time evolution of the blackbody bolometric flux F bb, the temperature kT bb, the observed radius R of the NS surface at 4 kpc, the goodness of fit ﹩{\chi }_{v}^{2}﹩. The bolometric flux of the blackbody model F bb is in units of 10−8 erg cm−2 s−1.
Paper: Insight-HXMT Observation of 4U 1608–52: Evidence of Interplay between a Thermonuclear Burst and Accretion Environment
Authors: Yu-Peng Chen, Shu Zhang, Long Ji, Shuang-Nan Zhang, Ling-Da Kong, Peng-Ju Wang, Zhi Chang, Jing-Qiang Peng, Jin-Lu Qu, Jian Li
Figure caption: Top panel: the spectral fit results for LE (black), ME (red)m and HE (green) when the burst reaches the maximum emission area in the f  a  model; the blackbody model and enhancement of the persistent emission are labeled. The three lower panels: residuals of the spectral fit results with an absorbed blackbody model (the second panel), f  a  model (the third panel), and convolution thermal-Comptonization model (the bottom panel).
Paper: Insight-HXMT Observation of 4U 1608–52: Evidence of Interplay between a Thermonuclear Burst and Accretion Environment
Authors: Yu-Peng Chen, Shu Zhang, Long Ji, Shuang-Nan Zhang, Ling-Da Kong, Peng-Ju Wang, Zhi Chang, Jing-Qiang Peng, Jin-Lu Qu, Jian Li
Figure caption: The spectral fit results of the persistent emission by LE (black), ME (red), and NICER (green) with model cons*tbabs*thcomp*diskbb. The embedded panel shows the background level for ME (red) and HE (blue).
Paper: Insight-HXMT Observation of 4U 1608–52: Evidence of Interplay between a Thermonuclear Burst and Accretion Environment
Authors: Yu-Peng Chen, Shu Zhang, Long Ji, Shuang-Nan Zhang, Ling-Da Kong, Peng-Ju Wang, Zhi Chang, Jing-Qiang Peng, Jin-Lu Qu, Jian Li
Figure caption: Illustration of the central region of an NS XRB before the PRE phase (left), in the PRE phase (middle), and after the PRE phase (right) during a burst, in which the inner part of the disk is swept away by the burst in the PRE phase.
Paper: The Radial Evolution of the Solar Wind as Organized by Electron Distribution Parameters
Authors: J. S. Halekas, P. Whittlesey, D. E. Larson, M. Maksimovic, R. Livi, M. Berthomier, J. C. Kasper, A. W. Case, M. L. Stevens, S. D. Bale, R. J. MacDowall, M. P. Pulupa
Figure caption: Radial evolution of the local solar wind proton speed (v  p ) measured by SPAN-Ion (same as Figures 4 and 8), with curves showing the predicted speed profiles from Parker solar wind models for a polytropic index of γ = 5/4 (Parker 1960), with coronal temperatures set to the corresponding strahl parallel temperatures (T  S∣∣). The diamonds show the critical points for the two solutions.
Paper: Insight-HXMT Observation of 4U 1608–52: Evidence of Interplay between a Thermonuclear Burst and Accretion Environment
Authors: Yu-Peng Chen, Shu Zhang, Long Ji, Shuang-Nan Zhang, Ling-Da Kong, Peng-Ju Wang, Zhi Chang, Jing-Qiang Peng, Jin-Lu Qu, Jian Li
Figure caption: Bolometric flux evolution of the bursts detected by Insight-HXMT with the f  a  model (left) and convolution thermal-Comptonization model (right). The bolometric flux (in units of 10−8 erg cm−2 s−1) evolution of the enhanced persistent emission is in green, the burst emission in red, and the sum of the previous two components in blue.
Paper: Insight-HXMT Observation of 4U 1608–52: Evidence of Interplay between a Thermonuclear Burst and Accretion Environment
Authors: Yu-Peng Chen, Shu Zhang, Long Ji, Shuang-Nan Zhang, Ling-Da Kong, Peng-Ju Wang, Zhi Chang, Jing-Qiang Peng, Jin-Lu Qu, Jian Li
Figure caption: The flux‒temperature diagram for the burst spectra in the rising (blue) and decaying (red) phase from 4U 1608–52. The diagonal blue and red lines correspond to constant radius in the rising and decaying phases. The time sequence is that the burst starts at the lower right, stays at the PRE phase (black) at the upper left, and decays at the lower left.
Paper: Insight-HXMT Observation of 4U 1608–52: Evidence of Interplay between a Thermonuclear Burst and Accretion Environment
Authors: Yu-Peng Chen, Shu Zhang, Long Ji, Shuang-Nan Zhang, Ling-Da Kong, Peng-Ju Wang, Zhi Chang, Jing-Qiang Peng, Jin-Lu Qu, Jian Li
Figure caption: Net lightcurves of the Type I X-ray burst detected in the Insight-HXMT observation of 4U 1608–52 with a time bin of 0.1 s. The top, second, third, and bottom panels are the LE, ME, and HE results in their full energy band and HE in 30–50 keV, respectively. The red lines indicates the PRE phase. The arrows indicates the hard X-ray excess during the PRE phase.
Paper: On the Impact of Relativistic Gravity on the Rate of Tidal Disruption Events
Authors: Eric R. Coughlin, C. J. Nixon
Figure caption: Distribution function of the pericenter distance (left) and β of the encounter (right), where β = r t/r p, normalized by N, which is the total number of stars scattered within distances ≤ r t. In the left panel the value of r p ranges from the direct capture radius r p = 4 to the tidal radius r p = r t. Note that the integral under each of these curves is less than N, the number of stars that enter the tidal radius, because the fraction of stars with r p < 4 is directly captured. The Newtonian result is plotted in the right panel as a dashed line with f  β  ∝ β −2; on the left panel the Newtonian result would be a horizontal line with ﹩{f}_{{r}_{{\rm{p}}}}=﹩ constant, to which the solutions clearly tend in the large-r p limit.
Paper: On the Impact of Relativistic Gravity on the Rate of Tidal Disruption Events
Authors: Eric R. Coughlin, C. J. Nixon
Figure caption: Fraction of TDEs (blue) and DCEs (red) as a function of the tidal radius (in gravitational radii; r g = GM/c 2) of the SMBH. The solid lines account for relativistic effects (Equations (13) and (14)), while the dashed lines are in the Newtonian limit (Equation (15)). The relation between the SMBH mass (top axis) and the tidal radius is given in Equation (11) and is for a solar-like star.