adsabs/AstroCLIMB huggingface dataset:
Paper: Cloud–Cloud Collision: Formation of Hub-filament Systems and Associated Gas Kinematics. Mass-collecting Cone—A New Signature of Cloud–Cloud Collision
Authors: A. K. Maity, T. Inoue, Y. Fukui, L. K. Dewangan, H. Sano, R. I. Yamada, K. Tachihara, N. K. Bhadari, O. R. Jadhav
Figure caption:                         The PV diagrams for the regions highlighted in Figure 2(i). The left and right panels are oriented along the x- and y-axes, respectively. Progressing from top to bottom, it covers t = 0, 0.2, 0.4, 0.5, and 0.7 Myr. Three velocity ranges are highlighted with shaded regions in blue, gray, and red on the PV diagram along the y-axis at t = 0.2 Myr. Similarly, two velocity ranges are indicated with shaded regions in gray and red on the PV diagram along the y-axis at t = 0.5 Myr. These velocity ranges are utilized to generate integrated density maps, which are presented in Figure 12.
Paper: Cloud–Cloud Collision: Formation of Hub-filament Systems and Associated Gas Kinematics. Mass-collecting Cone—A New Signature of Cloud–Cloud Collision
Authors: A. K. Maity, T. Inoue, Y. Fukui, L. K. Dewangan, H. Sano, R. I. Yamada, K. Tachihara, N. K. Bhadari, O. R. Jadhav
Figure caption: The spatial distribution of different velocity components in the x–y plane at t = 0.2 and 0.5 Myr. (a) The redshifted integrated density image at t = 0.2 Myr is displayed for the velocity range v  z : [4.25, 5.75] km s−1. The spatial distributions of the blueshifted component (for v  z : [−6.75, −3.75] km s−1) and the compressed layer (for v  z : [−2.25, 3.75] km s−1) are overlaid on the image using blue and black contours, respectively. A total of 20 equispaced contours ranging from 103 to 105 cm−3 km s−1 are shown for the blueshifted component. Similarly, 10 equispaced contours from 104 to 105 cm−3 km s−1 are shown for the compressed layer. (b) The redshifted integrated density image at t = 0.5 Myr is presented for the velocity range v  z : [5.25, 7.25] km s−1. The spatial distribution of the compressed layer (for v  z : [−3.25, 4.25] km s−1) is overlaid on the image using 10 equispaced black contours from 8 × 102 to 4 × 105 cm−3 km s−1.
Paper: Cloud–Cloud Collision: Formation of Hub-filament Systems and Associated Gas Kinematics. Mass-collecting Cone—A New Signature of Cloud–Cloud Collision
Authors: A. K. Maity, T. Inoue, Y. Fukui, L. K. Dewangan, H. Sano, R. I. Yamada, K. Tachihara, N. K. Bhadari, O. R. Jadhav
Figure caption:                         The magnetic field streamlines are shown over the (a) x–z and (b) y–z projected column density maps at t = 0.7 Myr. The plus symbols are sink particles, identical to Figures 2(s) and (t), respectively. (c) The y–z projected mass-weighted average gas velocity vectors for the compressed layer are displayed over the column density map for an integration range of x: [−0.1, 0.1] pc. The horizontal cuts, L1–L6 (having a width, ΔL                                               z                       = 0.25 pc), are used to extract the PV diagrams shown in Figure 14. The pair of white dashed lines show a cone (with θ  ∼ 52°). Panels (d), (e), and (f) show the changes in dynamic pressure, gravitational acceleration, and the magnetic fields in the compressed layer at t = 0.7 Myr. The regions, L1–L6, are marked in the last three panels with gray dotted lines.
Paper: Cloud–Cloud Collision: Formation of Hub-filament Systems and Associated Gas Kinematics. Mass-collecting Cone—A New Signature of Cloud–Cloud Collision
Authors: A. K. Maity, T. Inoue, Y. Fukui, L. K. Dewangan, H. Sano, R. I. Yamada, K. Tachihara, N. K. Bhadari, O. R. Jadhav
Figure caption: The distributions of (a) velocity magnitude (﹩|{\boldsymbol{V}}|﹩), (b) angle between ﹩{\boldsymbol{V}}﹩ and the z-axis, (c) density, (d) dynamic pressure, and (e) magnitude of the magnetic field (﹩|{\boldsymbol{B}}|﹩) in the compressed layer at t = 0.4 Myr, corresponding to the conical region shown in Figure 4(c). The contours in each panel represent 30%, 60%, and 90% of the total number of pixels, excluding contributions from the initial gas distribution and gravitationally accelerated gas (﹩|{\boldsymbol{V}}|\geqslant 5﹩ km s−1 and angle between ﹩{\boldsymbol{V}}﹩ and the z-axis ≤5°).
Paper: Cloud–Cloud Collision: Formation of Hub-filament Systems and Associated Gas Kinematics. Mass-collecting Cone—A New Signature of Cloud–Cloud Collision
Authors: A. K. Maity, T. Inoue, Y. Fukui, L. K. Dewangan, H. Sano, R. I. Yamada, K. Tachihara, N. K. Bhadari, O. R. Jadhav
Figure caption:                         Normalized histograms of the relative orientations among the filament skeleton, projected magnetic field, gas velocity, and gravitational field vectors at t = 0.7 Myr. The top row depicts pairs between high-density filament skeletons and the magnetic field, gas velocity, and gravitational field vectors. The bottom row illustrates the relative orientations among the magnetic field, gas velocity, and gravitational field vectors for both the skeletons (in light-slate blue) and their surroundings (in red). The total number of pixels in the filament skeletons (N                      ske) and their surroundings (N                      sur) are mentioned at each time step. Figure A1 in the Appendix contains similar plots for t = 0.3–0.6 Myr.
Paper: Cloud–Cloud Collision: Formation of Hub-filament Systems and Associated Gas Kinematics. Mass-collecting Cone—A New Signature of Cloud–Cloud Collision
Authors: A. K. Maity, T. Inoue, Y. Fukui, L. K. Dewangan, H. Sano, R. I. Yamada, K. Tachihara, N. K. Bhadari, O. R. Jadhav
Figure caption: Panels (a)–(f) present the PV diagrams extracted for the regions, L1–L6, which are highlighted in Figure 13(c). The gray curves on the PV diagrams present a cone (with θ  ∼ 52°) with a constant gas velocity of about 4.25 km s−1 directed toward its vertex. The cone is shown by white dashed lines in Figure 13(c).
Paper: Radio Afterglows from Tidal Disruption Events: An Unbiased Sample from ASKAP RACS
Authors: Akash Anumarlapudi, Dougal Dobie, David L. Kaplan, Tara Murphy, Assaf Horesh, Emil Lenc, Laura Driessen, Stefan W. Duchesne, Hannah Dykaar, B. M. Gaensler, Timothy J. Galvin, Joe Grundy, George Heald, Aidan W. Hotan, Minh Huynh, James K. Leung, David McConnell, Vanessa A. Moss, Joshua Pritchard, Wasim Raja, Kovi Rose, Gregory Sivakoff, Yuanming Wang, Ziteng Wang, Mark H. Wieringa, Matthew T. Whiting
Figure caption: Light curve of the TDE ASASSN-15oi using RACS, VLASS, and archival data. In all the figures in this article, RACS-low data are shown as black stars, RACS-mid as open black squares, RACS-high as open black diamonds, and VLASS data as filled black diamonds. RACS data combined with the data from the VAST full survey, shown as red stars, reveal the rise and decline of the 888 MHz light curve. Shown as multicolored dots is the archival light curve, from 3 to 15 GHz, adapted from Horesh et al. (2021). The green stripe shows the data used to estimate the electron distribution index. The inset shows this spectrum, and the dashed line in the inset shows the best-fit power law to these data (see text for more details). Shown as dashed–dotted lines are the visual guides for different power-law declines.
Paper: Radio Afterglows from Tidal Disruption Events: An Unbiased Sample from ASKAP RACS
Authors: Akash Anumarlapudi, Dougal Dobie, David L. Kaplan, Tara Murphy, Assaf Horesh, Emil Lenc, Laura Driessen, Stefan W. Duchesne, Hannah Dykaar, B. M. Gaensler, Timothy J. Galvin, Joe Grundy, George Heald, Aidan W. Hotan, Minh Huynh, James K. Leung, David McConnell, Vanessa A. Moss, Joshua Pritchard, Wasim Raja, Kovi Rose, Gregory Sivakoff, Yuanming Wang, Ziteng Wang, Mark H. Wieringa, Matthew T. Whiting
Figure caption: Top panel: the light curve using archival data (from Goodwin et al. 2022b; Sfaradi et al. 2022) is shown at four different frequencies (1.35, 2.25, 5.5, and 9 GHz). The yellow curve is the best-fit model for the 1.4 GHz data (see text for the model), with the dashed lines representing the individual components and the solid line indicating their sum. Bottom panel: 15.5 GHz light curve for reference using the data from Sfaradi et al. (2022). The red curve is the two-component model proposed by Sfaradi et al. (2022), with the dashed line representing the individual components and the solid line, their sum.
Paper: Radio Afterglows from Tidal Disruption Events: An Unbiased Sample from ASKAP RACS
Authors: Akash Anumarlapudi, Dougal Dobie, David L. Kaplan, Tara Murphy, Assaf Horesh, Emil Lenc, Laura Driessen, Stefan W. Duchesne, Hannah Dykaar, B. M. Gaensler, Timothy J. Galvin, Joe Grundy, George Heald, Aidan W. Hotan, Minh Huynh, James K. Leung, David McConnell, Vanessa A. Moss, Joshua Pritchard, Wasim Raja, Kovi Rose, Gregory Sivakoff, Yuanming Wang, Ziteng Wang, Mark H. Wieringa, Matthew T. Whiting
Figure caption: Light curve of TDE AT 2018hyz using RACS/VAST data, VLASS data, and archival data (from Cendes et al. 2022). The archival light curve, at five different frequencies from 1.3 to 19 GHz, adapted from Cendes et al. (2022), is shown as multicolored dots for reference.
Paper: Radio Afterglows from Tidal Disruption Events: An Unbiased Sample from ASKAP RACS
Authors: Akash Anumarlapudi, Dougal Dobie, David L. Kaplan, Tara Murphy, Assaf Horesh, Emil Lenc, Laura Driessen, Stefan W. Duchesne, Hannah Dykaar, B. M. Gaensler, Timothy J. Galvin, Joe Grundy, George Heald, Aidan W. Hotan, Minh Huynh, James K. Leung, David McConnell, Vanessa A. Moss, Joshua Pritchard, Wasim Raja, Kovi Rose, Gregory Sivakoff, Yuanming Wang, Ziteng Wang, Mark H. Wieringa, Matthew T. Whiting
Figure caption: Light curve of the TDE AT 2019ahk confirming the late-time rise of the radio light curve at all the RACS observing frequencies. Also shown are the contemporary data at 1.3 and 1.6 GHz adapted from Christy et al. (2024), showing the continued rise of the 0.8–0.9 GHz light curve and the turnover of the 1.6 GHz light curve. This source is too far south for VLASS.
Paper: Photometric White Dwarf Rotation
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, L. T. T. Soethe, Alejandra D. Romero, Keaton J. Bell
Figure caption: Observational data of the surface rotation of WD stars (orange crosses for the complete sample and black dots for the likely single sample) are compared against evolutionary models showing the rotation period in the WD cooling track. We compare models with the six mechanisms of angular momentum transport turned off (solid lines) and on (dotted lines) during the whole evolution. For an initial rotational velocity of v i = 10 km s−1, we present models with metallicities of Z = 0.02 (purple), 0.002 (dark green), and 0.001 (light blue). We also compare two models where the Tayler–Spruit dynamo is the only mechanism that is turned off during the computations (dark blue and light green dotted–dashed lines). For an initial rotational velocity of v i = 50 km s−1, we compare two models with Z = 0.02 (red lines). All model sequences have an initial mass of 1.5 M ⊙.
Paper: Photometric White Dwarf Rotation
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, L. T. T. Soethe, Alejandra D. Romero, Keaton J. Bell
Figure caption: Internal magnetic field at T eff = 25,000 K and 11,000 K, generated by the Tayler–Spruit dynamo during the evolution due to differential rotation caused by angular momentum transfer throughout the stellar evolution. B  r  is the radial field and B  ϕ  is the azimuthal one. The properties of the initial model in ZAMS are M  i  = 1.5 M ⊙, Z = 0.001, and v  i  = 10 km s−1. For T eff = 25,000 K, the solid red line shows the radial component and the dotted blue line represents the azimuthal one. For T eff = 11,000 K, the dashed green line shows the azimuthal component and the radial component does not have enough intensity to appear in the plot. The six angular momentum transfer mechanisms operate throughout the evolution. Magnetic field values are negligible beyond 1.3 on the x-axis, i.e., toward the surface.
Paper: Photometric White Dwarf Rotation
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, L. T. T. Soethe, Alejandra D. Romero, Keaton J. Bell
Figure caption: FT of the 20 s data for G226-29 from Sectors 40 to 41 and 47 to 60. The inset plot zooms into the FT at low frequencies. The red dashed line indicates the FAP. The large peak on the right is the pulsation triplet at 109.47235s@1.81mma, 109.27929s@0.57mma, and 109.08690s@1.62mma, while the region around 200 μHz corresponds to the wandering peak around 4500 s.
Paper: Photometric White Dwarf Rotation
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, L. T. T. Soethe, Alejandra D. Romero, Keaton J. Bell
Figure caption: FT of TESS data of star TIC 262548040. The horizontal red line indicates FAP = 1/1000 and the vertical dotted lines indicate the peak of 0.106 hr and its double.
Paper: Photometric White Dwarf Rotation
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, L. T. T. Soethe, Alejandra D. Romero, Keaton J. Bell
Figure caption: Running FT of G226-29 20 s data from Sector 51. The tall peak on the right is the pulsation triplet around 109 s, while the region around 200 μHz corresponds to the peaks around 4500 s.
Paper: Photometric White Dwarf Rotation
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, L. T. T. Soethe, Alejandra D. Romero, Keaton J. Bell
Figure caption: Rotational period distribution up to 30 hr for the likely single WDs excluding periods shorter than 0.3 hr. The red bins indicate the magnetic stars of the sample.
Paper: Photometric White Dwarf Rotation
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, L. T. T. Soethe, Alejandra D. Romero, Keaton J. Bell
Figure caption: FT of NGC 1501 data at low frequencies.
Paper: Photometric White Dwarf Rotation
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, L. T. T. Soethe, Alejandra D. Romero, Keaton J. Bell
Figure caption: FT of TIC 7675859 data from sectors 52 to 54.
Paper: Photometric White Dwarf Rotation
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, L. T. T. Soethe, Alejandra D. Romero, Keaton J. Bell
Figure caption: BPM 24754 light curve from Sectors 12, 39, and 66.
Paper: Unveiling the Multifaceted GRB 200613A: Prompt Emission Dynamics, Afterglow Evolution, and the Host Galaxy’s Properties
Authors: Shao-Yu Fu, Dong Xu, Wei-Hua Lei, Antonio de Ugarte Postigo, D. Alexander Kann, Christina C. Thöne, José Feliciano Agüí Fernández, Yi Shuang-Xi, Wei Xie, Yuan-Chuan Zou, Xing Liu, Shuai-Qing Jiang, Tian-Hua Lu, Jie An, Zi-Pei Zhu, Jie Zheng, Qing-Wen Tang, Peng-Wei Zhao, Li-Ping Xin, Jian-Yan Wei
Figure caption: Constraint on the central engine parameters, i.e., the accretion rate ﹩\dot{m}﹩ and BH spin a •, for GRB 200613A. The shaded region is obtained by equating ﹩{\dot{E}}_{{\rm{B}}}{\eta }_{\gamma }/{f}_{{\rm{b}}}=3.5\times {10}^{52}\ \mathrm{erg}\ {{\rm{s}}}^{-1}﹩ (the upper boundary, the solid black line) and ﹩{\dot{E}}_{{\rm{B}}}{\eta }_{\gamma }/{f}_{{\rm{b}}}=1\times {10}^{52}\ \mathrm{erg}\ {{\rm{s}}}^{-1}﹩ (lower boundary, the dashed black line). The blue triangles are the ones obtained by assuming the upper limit of BB component as ﹩{L}_{\gamma ,\mathrm{iso}}^{\mathrm{BB}}\leqslant {L}_{\gamma ,\mathrm{iso}}^{\mathrm{Band}}/100﹩. The true value is shown with blue triangles in the shaded region. The BH mass m • = 3, efficiency η  γ  ≃ 0.45, and beaming factor f b = 0.09 are adopted when producing this figure.
Paper: Unveiling the Multifaceted GRB 200613A: Prompt Emission Dynamics, Afterglow Evolution, and the Host Galaxy’s Properties
Authors: Shao-Yu Fu, Dong Xu, Wei-Hua Lei, Antonio de Ugarte Postigo, D. Alexander Kann, Christina C. Thöne, José Feliciano Agüí Fernández, Yi Shuang-Xi, Wei Xie, Yuan-Chuan Zou, Xing Liu, Shuai-Qing Jiang, Tian-Hua Lu, Jie An, Zi-Pei Zhu, Jie Zheng, Qing-Wen Tang, Peng-Wei Zhao, Li-Ping Xin, Jian-Yan Wei
Figure caption: Comparison between the observations and the predictions from the neutrino annihilation mechanism (red dashed lines) and the BZ mechanism (blue dashed lines), reproduced by Yi et al. (2017). The blue dots indicate GRBs with the beaming corrected luminosity, whereas magenta triangles are the ones with only a lower limit. The red dashed lines show ﹩\eta (\dot{m})-{\dot{E}}_{\nu \bar{\nu }}(\dot{m})﹩ relation for θ  j  = 0.022 (top), 0.04 (middle) and 0.12 (bottom), respectively. The blue dashed line shows the ﹩{{\rm{\Gamma }}}_{\max }(\dot{m})﹩–﹩{\dot{E}}_{{\rm{B}}}(\dot{m})﹩ relation. The ﹩{{\rm{\Gamma }}}_{\min }(\dot{m})﹩–﹩{\dot{E}}_{{\rm{B}}}(\dot{m})﹩ is plotted with the blue dotted line. The best fits to the data ﹩{{\rm{\Gamma }}}_{0}\propto {L}_{\mathrm{tot}}^{0.14}﹩ are shown with a solid line (Yi et al. 2017). The green triangles indicate the GRB 200613A with a lower limit.
Paper: Unveiling the Multifaceted GRB 200613A: Prompt Emission Dynamics, Afterglow Evolution, and the Host Galaxy’s Properties
Authors: Shao-Yu Fu, Dong Xu, Wei-Hua Lei, Antonio de Ugarte Postigo, D. Alexander Kann, Christina C. Thöne, José Feliciano Agüí Fernández, Yi Shuang-Xi, Wei Xie, Yuan-Chuan Zou, Xing Liu, Shuai-Qing Jiang, Tian-Hua Lu, Jie An, Zi-Pei Zhu, Jie Zheng, Qing-Wen Tang, Peng-Wei Zhao, Li-Ping Xin, Jian-Yan Wei
Figure caption: Stellar mass of the host galaxies vs. SFR (left panel) and specific SFR (right panel) of our sample. Open squares represent parameters derived using Prospector, while solid circles represent those derived in other ways (e.g., via other numerical models or mass-to-light relations). The host galaxy of GRB 200613A is represented by a black open square. Notably, the most massive host galaxy in our sample is GRB 190829A.
Paper: Late-time X-Ray Observations of the Jetted Tidal Disruption Event AT2022cmc: The Relativistic Jet Shuts Off
Authors: T. Eftekhari, A. Tchekhovskoy, K. D. Alexander, E. Berger, R. Chornock, T. Laskar, R. Margutti, Y. Yao, Y. Cendes, S. Gomez, A. Hajela, D. R. Pasham
Figure caption: Allowed phase space of black holes masses as a function of both the jet efficiency (η jet = ϵ jet/ϵ disk) and the fraction of accreted matter (f in = f accr f circ f partial) for AT2022cmc, Sw J1644+57, and Sw J2058+05, where individual curves correspond to the ratio of intrinsic jet and disk luminosity (L jet/L disk with ﹩{L}_{\mathrm{jet}}={L}_{\mathrm{jet},\mathrm{off}}{f}_{\mathrm{beam},200}^{-1}{f}_{\mathrm{bol},3}﹩) at jet shut-off (blue curves) and the total accreted mass relative to a complete disruption (M accr/0.5 M ⊙; red curves). The width of each curve corresponds to the uncertainty in the X-ray luminosity and timescale of jet shut-off. For a given black hole mass, there exists a one-to-one mapping between f in and η jet. The gray shaded regions denote the upper limit constraints on M BH for each source from X-ray variability arguments.
Paper: Late-time X-Ray Observations of the Jetted Tidal Disruption Event AT2022cmc: The Relativistic Jet Shuts Off
Authors: T. Eftekhari, A. Tchekhovskoy, K. D. Alexander, E. Berger, R. Chornock, T. Laskar, R. Margutti, Y. Yao, Y. Cendes, S. Gomez, A. Hajela, D. R. Pasham
Figure caption: Stringent late-time upper limits on the X-ray emission of AT2022cmc obtained in this work place robust constraints on the shut-off time of the relativistic jet. Our late-time Chandra observations (large open triangles) and our merged Chandra epoch (large solid triangle) at t rest ≈ 182 days indicate a deviation from the earlier power-law decline (dashed maroon line) in the X-ray light curve based on Swift/XRT (t rest ∼ 5–86 days; Y. Yao et al. 2024) and XMM-Newton (t rest = 52 and 137 days; Y. Yao et al. 2024) data. Our best-fit broken power-law model is shown as a dark blue line, while light blue lines represent random samples from the MCMC chains. Also shown for comparison are the X-ray light curves of other jetted TDEs, including Sw J1644+57 (light gray circles; D. N. Burrows et al. 2011; B. A. Zauderer et al. 2013; T. Eftekhari et al. 2018), Sw J2058+05 (dark gray squares; D. R. Pasham et al. 2015), and Sw J1112-82 (yellow squares; G. C. Brown et al. 2015). Vertical dashed lines indicate the time of jet shut-off for each event.
Paper: The Wanderer: Charting WASP-77A b’s Formation and Migration Using a System-wide Inventory of Carbon and Oxygen Abundances
Authors: David R. Coria, Neda Hejazi, Ian J. M. Crossfield, Maleah Rhem
Figure caption: Pre- and post-renormalization for strong, isolated 13CH lines (top: line at 4231.412 Å in the HIRES spectrum; bottom: line at 4268.304 Å in the ESPRESSO spectrum). The area within the orange lines shows the χ 2 fit window dominated by 13CH line centered at 3982.247 Å, while the regions covered by the red and black lines (left plot) are excluded from the continuum/pseudo-continuum selection routine. The starred points are the selected continuum/pseudo-continuum points used for renormalization. The pink points represent the residuals R = O/M for the selected continuum/pseudo-continuum points and the black curve is the polynomial fit which, when divided out of the observed spectrum, provides a significantly better alignment to the target 13CH line. The figures on the right highlight the location of our selected 13CH lines and other nearby atomic lines.
Paper: Late-time X-Ray Observations of the Jetted Tidal Disruption Event AT2022cmc: The Relativistic Jet Shuts Off
Authors: T. Eftekhari, A. Tchekhovskoy, K. D. Alexander, E. Berger, R. Chornock, T. Laskar, R. Margutti, Y. Yao, Y. Cendes, S. Gomez, A. Hajela, D. R. Pasham
Figure caption: Left: X-ray light curve of Sw J2058+05 (D. R. Pasham et al. 2015; black squares) with our best-fit broken power-law model (dark blue curve), which indicates a jet shut-off time of ﹩{t}_{\mathrm{rest}}\approx {212}_{-35}^{+46}﹩ days. The X-ray light curve prior to the jet shut-off decays following t −2.1. Right: results from our MCMC parameter estimation for a broken power-law fit to the X-ray light curve of Sw J2058+05. Marginalized posterior distributions for each parameter are shown on the diagonal, where dashed lines indicate the median and 68% confidence interval.
Paper: Late-time X-Ray Observations of the Jetted Tidal Disruption Event AT2022cmc: The Relativistic Jet Shuts Off
Authors: T. Eftekhari, A. Tchekhovskoy, K. D. Alexander, E. Berger, R. Chornock, T. Laskar, R. Margutti, Y. Yao, Y. Cendes, S. Gomez, A. Hajela, D. R. Pasham
Figure caption: Results from our MCMC parameter estimation for a broken power-law fit to the X-ray light curve of AT2022cmc. Marginalized posterior distributions for each parameter are shown on the diagonal, where dashed lines indicate the median and 68% confidence interval.
Paper: Pre-peak Emission in Tidal Disruption Events
Authors: Xiaoshan Huang, 小珊 黄, Shane W. Davis, Yan-fei Jiang, 燕飞 姜
Figure caption: Top panel: the outflow rates ﹩{\dot{M}}_{\mathrm{out}}﹩ (dashed lines) and accretion rates (solid lines) in RSI50Edd10 (orange lines), RSI20Edd10 (blue lines), and RSI100Edd10 (red lines). The accretion rate is measured at 3r  s  in all three runs. The outflow rate is measured over spherical shells at radii of 100r SI, 150r SI, and 300r SI in RSI20Edd10, RSI50Edd10, and RSI100Edd10, respectively. These are relatively outer radii in each simulation where the mass flux and luminosity are not sensitive to measuring radius. Bottom panel: total luminosity L carried by radiation flux measured over the same spherical shell as ﹩{\dot{M}}_{\mathrm{out}}﹩, normalized to Eddington luminosity assuming 10% efficiency. The prompt rise on L/L Edd corresponds to the emission from stream–stream collision. We caution that such a short rise time is likely related to the fixed ﹩\dot{M}﹩ we assumed in our injected stream and likely underestimates the rise time of real TDEs, where the fallback accretion rate ramps up over time.