adsabs/AstroCLIMB huggingface dataset:
Paper: The Disappearance of the Blue and Luminous Progenitor of the Type IIn SN 2010jl
Authors: Zexi Niu, Ning-Chen Sun, Jifeng Liu
Figure caption: Left: photometry decomposition of the preexplosion source s0, which is a blend of the progenitor of SN 2010jl (i.e., s1; blue) and the nearby field cluster s2 (orange). The black data points are based on HST observations as derived in this work, while the gray data points are based on Spizter/IRAC observations as reported in Fox et al. (2017). The progenitor is consistent with a blackbody of log(T eff/K) = 4.26﹩{}_{-0.09}^{+0.11}﹩ and log(L/L ⊙) = 6.52﹩{}_{-0.16}^{+0.20}﹩. Right: position of SN 2010jl’s progenitor on the HR diagram (red star with error bars). The other directly detected Type IIn SN progenitors are also displayed, including SN 2005gl (Gal-Yam et al. 2007), SN 2009ip (Smith et al. 2010b), SN 2010bt (Elias-Rosa et al. 2018), SN 2015bh (Elias-Rosa et al. 2016), and SN 2016jbu (Kilpatrick et al. 2018). For the last two SNe (2015bh and 2016jbu), the progenitors are observed at multiple epochs and exhibit significant variability; we show their positions at all the epochs as reported in the references. For the progenitors of the first three SNe (2005gl, 2009ip, and 2010bt), the effective temperatures are not well constrained by the detection (often in a single band), so we conservatively leave effective temperature as a free parameter and refit the reported photometry with a blackbody SED; the results are shown by the hatched regions. For comparison, We also plot single-star isochrones of M ini = 30, 50, 80 M ⊙ provided by MIST (black lines; Dotter 2016), standard locations of the hot/cool phases for LBVs (gray-shaded regions; Smith et al. 2004), the HD limit (gray broken line; Humphreys & Davidson 1994), and the position of the Galactic LBV η Car (black dotted line; Groh et al. 2012; Mehner et al. 2019).
Paper: The Disappearance of the Blue and Luminous Progenitor of the Type IIn SN 2010jl
Authors: Zexi Niu, Ning-Chen Sun, Jifeng Liu
Figure caption: HST photometry of s1 (i.e., SN 2010jl; black circles) and s2 (gray circles) at late times. Their composite magnitudes are also calculated and displayed as the red or blue diamonds. The gray horizontal lines correspond to the inverse-variance-weighted average magnitudes of s2 at different epochs, and the red/blue lines are the preexplosion brightness of s0 observed in 2001. The photometric uncertainties are reflected by the error bars associated with the data points and the widths of the horizontal lines.
Paper: The Disappearance of the Blue and Luminous Progenitor of the Type IIn SN 2010jl
Authors: Zexi Niu, Ning-Chen Sun, Jifeng Liu
Figure caption: HST images centered at SN 2010jl. All stamps have the same dimension of 0.″8 × 0.″8, and are aligned with north up and east to the left. The crosses mark the positions of sources near the SN position, i.e., the preexplosion source s0 detected on the WFPC2 images (blue), and the postexplosion sources s1 and s2 detected on the WFC3 images (red). For comparison, we have astrometrically aligned the images and overplot the positions of all three sources on each image.
Paper: Stellar Black Holes Can “Stretch” Supermassive Black Hole Accretion Disks
Authors: Shuying Zhou, Mouyuan Sun, Tong Liu, Jian-Min Wang, Jun-Xian Wang, Yongquan Xue
Figure caption: The left panel is same as the bottom panel of Figure 1, and the right panel is same as Figure 3 but with all sBHs distributed at R sBHs = 1000 R S. For this sBHs distribution, the effects of sBHs are on the same radius, and only the effective temperature at 1000 R S is changed. This distribution of sBHs allows the AGN accretion disk to have large half-light radii even at short wavelengths (i.e., 2000 Å).
Paper: Stellar Black Holes Can “Stretch” Supermassive Black Hole Accretion Disks
Authors: Shuying Zhou, Mouyuan Sun, Tong Liu, Jian-Min Wang, Jun-Xian Wang, Yongquan Xue
Figure caption: The effective temperature (T eff) distributions from R in = 3R S to R out = 3000R S for M • = 108 M ⊙ and ﹩{\dot{m}}_{\mathrm{tot}}={\dot{M}}_{\mathrm{tot}}/{\dot{M}}_{\bullet ,\mathrm{Edd}}=0.3﹩. The top left panel is for a pure SSD; the top right panel is for an SSD with sBHs for f sBHs = 0.1 and M sBH = 50 M ⊙ (Equation (6)). The bottom panel compares the effective temperature profiles for the two cases. The red curve is the effective temperature profile for a pure SSD; the blue curve is the azimuthal averaged effective temperature profile for an SSD embedded with sBHs; the gray dashed line indicates the T eff ∝ R −3/4 scaling relation. The accreting sBHs in an SSD heating up gas in the outer regions, resulting in an effective temperature profile significantly shallower than a pure SSD. Microlensing observations can distinguish the two temperature profiles.
Paper: Stellar Black Holes Can “Stretch” Supermassive Black Hole Accretion Disks
Authors: Shuying Zhou, Mouyuan Sun, Tong Liu, Jian-Min Wang, Jun-Xian Wang, Yongquan Xue
Figure caption: Half-light radii at different wavelengths for M • = 108 M ⊙. The x-axis is the rest-frame wavelength in units of 4000 Å. The y-axis is the half-light radius for an SSD embedded with sBHs (R half,sBHs) and a pure SSD in units of R S. The purple curves represent the results with different f sBHs. The blue and red dashed curves are the half-light radius of a pure SSD (R half,SSD) and 3R half,SSD, respectively. The colorful arrows indicate the rest-frame wavelengths of LSST bands at a redshift of 0.658, i.e., the redshift of a low-redshift lensed quasar, RXS J113155.5-123155 (Sluse et al. 2003). The presence of accreting sBHs significantly alters the half-light radius–wavelength relation by increasing the half-light radius of the long-wavelength emission.
Paper: Stellar Black Holes Can “Stretch” Supermassive Black Hole Accretion Disks
Authors: Shuying Zhou, Mouyuan Sun, Tong Liu, Jian-Min Wang, Jun-Xian Wang, Yongquan Xue
Figure caption: SEDs for the models and comparisons with composite quasar spectra. In each panel, the red curve is the SED for a pure SSD, the blue curve is the SED for an SSD embedded with a population of sBHs, and the purple curve is the composite quasar spectrum (normalized at 1450 Å). The top panel is for M • = 108 M ⊙ with f sBHs = 0.1 (for a pure SSD, f sBHs ≡ 0) and the composite quasar spectrum from Vanden Berk et al. (2001). When the wavelength is approximately larger than 4700 Å, the SED of the SSD with sBHs is significantly larger than that of the pure SSD, and the spectral slope in this wavelength range is almost consistent with the composite spectrum. The bottom panel is for M • = 109 M ⊙ with f sBHs = 0.1 and the composite quasar spectrum from Selsing et al. (2016). In this case, the sBHs have weak effects on the SED.
Paper: Stellar Black Holes Can “Stretch” Supermassive Black Hole Accretion Disks
Authors: Shuying Zhou, Mouyuan Sun, Tong Liu, Jian-Min Wang, Jun-Xian Wang, Yongquan Xue
Figure caption: Same as Figure 3 but for M • = 107 M ⊙. The wavelength ranges affected by accreting sBHs increase with decreasing SMBH mass.
Paper: Energetic Neutral Atoms Detected in the 2022 February 15 Solar Energetic Particle Event
Authors: C. M. S. Cohen, R. A. Leske, O. C. St. Cyr, G. M. Mason
Figure caption: Height as a function of time for the leading edges of the CME (black points) and the prominence (red points). For comparison, the release time profile of the ENAs is overplotted. The time for light to travel from the Sun to STEREO-A is added to enable direct comparison to remote-sensing data.
Paper: Energetic Neutral Atoms Detected in the 2022 February 15 Solar Energetic Particle Event
Authors: C. M. S. Cohen, R. A. Leske, O. C. St. Cyr, G. M. Mason
Figure caption: Energy deposited in detector L1 vs. energy deposited in detector L2 for all protons (red) and ENAs (blue). The upper portion of the trace is due to protons stopping in the L2 detector; the lower portion is from protons passing through both L1 and L2.
Paper: Energetic Neutral Atoms Detected in the 2022 February 15 Solar Energetic Particle Event
Authors: C. M. S. Cohen, R. A. Leske, O. C. St. Cyr, G. M. Mason
Figure caption: Average intensity spectrum for the ENAs averaged over the time period 2022 February 15 22:48 UT to 2022 February 16 01:12 UT (green solid circles) and for the Mewaldt et al. (2009) event (blue open squares) averaged over the period 2006 December 5 11:30 UT to 13:50 UT. A power law with index of −2.46 is shown for comparison to that reported by Mewaldt et al. (2009).
Paper: Energetic Neutral Atoms Detected in the 2022 February 15 Solar Energetic Particle Event
Authors: C. M. S. Cohen, R. A. Leske, O. C. St. Cyr, G. M. Mason
Figure caption: Angular distribution of the ENAs and protons for the ENA time period (blue line) and an earlier time period (red line). To increase statistical accuracy, the selected earlier time is 5 times longer; thus, for quantitative comparison, the red histogram is scaled by a factor of 5. The range of the IMF angles for the ENA time period, as indicated by the black arrow, was 21.8°–78° (and primarily varying between 40° and 70°).
Paper: Energetic Neutral Atoms Detected in the 2022 February 15 Solar Energetic Particle Event
Authors: C. M. S. Cohen, R. A. Leske, O. C. St. Cyr, G. M. Mason
Figure caption: (Left) Intensities of 1.8–3.6 MeV protons as a function of time for three sectors. Ranges of angles (relative to the spacecraft–Sun line) for each sector are given in the legend; note that sector 7 includes directions radially from the Sun. (Right) Zoom-in on the sector 7 increase around 2022 February 16 00:00 UT (day 47) with statistical uncertainties shown.
Paper: Energetic Neutral Atoms Detected in the 2022 February 15 Solar Energetic Particle Event
Authors: C. M. S. Cohen, R. A. Leske, O. C. St. Cyr, G. M. Mason
Figure caption: (Left) Images from STEREO-A/EUVI, COR1, and COR2 at different times, showing the leading edge of the erupting CME. To enhance the visibility of the CME, a background frame a few minutes earlier was subtracted from each image. (Right) Positions of various spacecraft at the time of the eruption (Gieseler et al. 2023). The black arrow indicates the approximate direction of the eruption.
Paper: Energetic Neutral Atoms Detected in the 2022 February 15 Solar Energetic Particle Event
Authors: C. M. S. Cohen, R. A. Leske, O. C. St. Cyr, G. M. Mason
Figure caption: (Left) Inverse velocity vs. time for all protons (red points) and the ENAs (blue). Dashed lines show expected velocity dispersion for path lengths of 0.967 au (the distance to STEREO-A) and 6 au (the latter also has a later release time to better correspond to the apparent SEP onset). (Right) The same plot for 8 hr of 2022 February 15–16, illustrating the good agreement between the expected velocity dispersion for a release time of 21:55 UT and path length of 0.967 au and the leading edge of the ENAs. Energy equivalents are shown on the right y-axes.
Paper: Energetic Neutral Atoms Detected in the 2022 February 15 Solar Energetic Particle Event
Authors: C. M. S. Cohen, R. A. Leske, O. C. St. Cyr, G. M. Mason
Figure caption: Red circles: arrival angle from the spacecraft–Sun line for protons as a function of time; in blue filled circles are the sector 7 particles during the time period of 46.95–47.05. The variability of the magnetic field direction during the ENA time period is indicated by the vertical arrow to the left of the y-axis and extends to 78°.
Paper: Energetic Neutral Atoms Detected in the 2022 February 15 Solar Energetic Particle Event
Authors: C. M. S. Cohen, R. A. Leske, O. C. St. Cyr, G. M. Mason
Figure caption: Positions and labels of the detectors for STEREO/LET. Adapted from Mewaldt et al. (2008).
Paper: JWST/MIRI Detection of Suprathermal OH Rotational Emissions: Probing the Dissociation of the Water by Lyα Photons near the Protostar HOPS 370
Authors: David A. Neufeld, P. Manoj, Himanshu Tyagi, Mayank Narang, Dan M. Watson, S. Thomas Megeath, Ewine F. Van Dishoeck, Robert A. Gutermuth, Thomas Stanke, Yao-Lun Yang, Adam E. Rubinstein, Guillem Anglada, Henrik Beuther, Alessio Caratti o Garatti, Neal J. Evans, Samuel Federman, William J. Fischer, Joel Green, Pamela Klaassen, Leslie W. Looney, Mayra Osorio, Pooneh Nazari, John J. Tobin, Łukasz Tychoniec, Scott Wolk
Figure caption: Spectral line maps obtained toward HOPS 370, shown with a logarithmic stretch. R.A. and decl. offsets are given in arcseconds relative to the ALMA source position (green star). The white circle demarks a 0.″8 radius region centered on the shocked knot. The maps are masked near a bright continuum source in the south where the line fits are unreliable. The red circles show the beam size (HPBW).
Paper: JWST/MIRI Detection of Suprathermal OH Rotational Emissions: Probing the Dissociation of the Water by Lyα Photons near the Protostar HOPS 370
Authors: David A. Neufeld, P. Manoj, Himanshu Tyagi, Mayank Narang, Dan M. Watson, S. Thomas Megeath, Ewine F. Van Dishoeck, Robert A. Gutermuth, Thomas Stanke, Yao-Lun Yang, Adam E. Rubinstein, Guillem Anglada, Henrik Beuther, Alessio Caratti o Garatti, Neal J. Evans, Samuel Federman, William J. Fischer, Joel Green, Pamela Klaassen, Leslie W. Looney, Mayra Osorio, Pooneh Nazari, John J. Tobin, Łukasz Tychoniec, Scott Wolk
Figure caption: The 8.8–13.4 μm spectra obtained toward the shocked knots. From top to bottom: Band 2B spectrum with continuum fit in blue; continuum-subtracted Band 2B, 2C, and 3A spectra. Red numbers above the OH lines indicate the value of N  U .
Paper: JWST/MIRI Detection of Suprathermal OH Rotational Emissions: Probing the Dissociation of the Water by Lyα Photons near the Protostar HOPS 370
Authors: David A. Neufeld, P. Manoj, Himanshu Tyagi, Mayank Narang, Dan M. Watson, S. Thomas Megeath, Ewine F. Van Dishoeck, Robert A. Gutermuth, Thomas Stanke, Yao-Lun Yang, Adam E. Rubinstein, Guillem Anglada, Henrik Beuther, Alessio Caratti o Garatti, Neal J. Evans, Samuel Federman, William J. Fischer, Joel Green, Pamela Klaassen, Leslie W. Looney, Mayra Osorio, Pooneh Nazari, John J. Tobin, Łukasz Tychoniec, Scott Wolk
Figure caption: Spectra of suprathermal OH lines observed toward the shocked knots. Yellow: observed spectrum. Line positions are marked with vertical lines for each component of the OH quartet, with the same color coding as in Figure 2. Black histogram: Gaussian fit to the ﹩{\rm{A}}^{\prime} ﹩ components (see text).
Paper: JWST/MIRI Detection of Suprathermal OH Rotational Emissions: Probing the Dissociation of the Water by Lyα Photons near the Protostar HOPS 370
Authors: David A. Neufeld, P. Manoj, Himanshu Tyagi, Mayank Narang, Dan M. Watson, S. Thomas Megeath, Ewine F. Van Dishoeck, Robert A. Gutermuth, Thomas Stanke, Yao-Lun Yang, Adam E. Rubinstein, Guillem Anglada, Henrik Beuther, Alessio Caratti o Garatti, Neal J. Evans, Samuel Federman, William J. Fischer, Joel Green, Pamela Klaassen, Leslie W. Looney, Mayra Osorio, Pooneh Nazari, John J. Tobin, Łukasz Tychoniec, Scott Wolk
Figure caption: H2 rotational diagram obtained toward the shocked knots. Black points: no reddening correction. Blue and red points: reddening correction applied. Blue and red dashed lines: best fits to the rotational diagram for ortho- and para-H2.
Paper: JWST/MIRI Detection of Suprathermal OH Rotational Emissions: Probing the Dissociation of the Water by Lyα Photons near the Protostar HOPS 370
Authors: David A. Neufeld, P. Manoj, Himanshu Tyagi, Mayank Narang, Dan M. Watson, S. Thomas Megeath, Ewine F. Van Dishoeck, Robert A. Gutermuth, Thomas Stanke, Yao-Lun Yang, Adam E. Rubinstein, Guillem Anglada, Henrik Beuther, Alessio Caratti o Garatti, Neal J. Evans, Samuel Federman, William J. Fischer, Joel Green, Pamela Klaassen, Leslie W. Looney, Mayra Osorio, Pooneh Nazari, John J. Tobin, Łukasz Tychoniec, Scott Wolk
Figure caption: Contours of the predicted Lyα/Brα luminosity ratio in the plane of v  s  and log10 n 0. Red, cyan, and blue contours: Lyα/Brα = 1000, 1500, and 2000. Green band: region where the predicted [Ne III] 15.6 μm to [Ne II] 12.8 μm flux ratio lies within a factor of 1.5 of that observed. Magenta band: region where the predicted [Fe II] 17.94 μm to [Fe II] 5.34 μm flux ratio lies within a factor of 1.5 of that observed.
Paper: JWST/MIRI Detection of Suprathermal OH Rotational Emissions: Probing the Dissociation of the Water by Lyα Photons near the Protostar HOPS 370
Authors: David A. Neufeld, P. Manoj, Himanshu Tyagi, Mayank Narang, Dan M. Watson, S. Thomas Megeath, Ewine F. Van Dishoeck, Robert A. Gutermuth, Thomas Stanke, Yao-Lun Yang, Adam E. Rubinstein, Guillem Anglada, Henrik Beuther, Alessio Caratti o Garatti, Neal J. Evans, Samuel Federman, William J. Fischer, Joel Green, Pamela Klaassen, Leslie W. Looney, Mayra Osorio, Pooneh Nazari, John J. Tobin, Łukasz Tychoniec, Scott Wolk
Figure caption: OH photon intensity as a function of N  U . Black points: observed intensities. Also shown are the T21 predictions for H2O photodissociation by Lyα radiation (blue) and by a 104 K blackbody (red).
Paper: JWST/MIRI Detection of Suprathermal OH Rotational Emissions: Probing the Dissociation of the Water by Lyα Photons near the Protostar HOPS 370
Authors: David A. Neufeld, P. Manoj, Himanshu Tyagi, Mayank Narang, Dan M. Watson, S. Thomas Megeath, Ewine F. Van Dishoeck, Robert A. Gutermuth, Thomas Stanke, Yao-Lun Yang, Adam E. Rubinstein, Guillem Anglada, Henrik Beuther, Alessio Caratti o Garatti, Neal J. Evans, Samuel Federman, William J. Fischer, Joel Green, Pamela Klaassen, Leslie W. Looney, Mayra Osorio, Pooneh Nazari, John J. Tobin, Łukasz Tychoniec, Scott Wolk
Figure caption: Average 5.8–7.0 μm spectrum obtained toward the shocked knots, with rovibrational transitions of ortho- and para-water marked with stars and plus signs.
Paper: “Extended Emission” from Fallback Accretion onto Merger Remnants
Authors: Carlo Musolino, Raphaël Duqué, Luciano Rezzolla
Figure caption: Mass ejection history of the four simulations. All times are measured from the merger time, and the mass flux is separated into bound (red), unbound (blue), and total mass flux (black). For all binaries, the vertical gray dashed lines mark the moments where the snapshots of Figures 1 and 2 are taken. For the two SFHO binaries (upper panels), the time of black hole formation is also marked with a black dotted line.
Paper: “Extended Emission” from Fallback Accretion onto Merger Remnants
Authors: Carlo Musolino, Raphaël Duqué, Luciano Rezzolla
Figure caption: Snapshots of the material flowing through the detector surface at R  d  = 300 M ⊙ at various times of the simulation. Upper panels: SFHO-q1.0 system. Lower panels: SFHO-q.75 system. Upper hemispheres: mass flux per unit solid angle. Lower hemispheres: u  t  of the flowing material. The three columns correspond to different times during the evolution, as reported in Figure 3.
Paper: “Extended Emission” from Fallback Accretion onto Merger Remnants
Authors: Carlo Musolino, Raphaël Duqué, Luciano Rezzolla
Figure caption: Fallback accretion rate for the bound material. We present the four simulated binaries as solid lines and an accretion rate with ﹩\dot{{m}_{\mathrm{FB}}}\propto {t}_{\mathrm{FB}}^{-5/3}﹩ to guide the eye (dashed line).
Paper: “Extended Emission” from Fallback Accretion onto Merger Remnants
Authors: Carlo Musolino, Raphaël Duqué, Luciano Rezzolla
Figure caption: Two-dimensional mass histogram of bound matter as per its ejection time (x-axis) and fallback time (y-axis) for all four binaries studied. These histograms evidence the fallback time of the bound material ejected at different stages of the merger and postmerger phases. For the two SFHO binaries (top panels), we also indicate the time of formation of the black hole (vertical black line). For the TNTYST-q1.0 system (lower left panel), we show the 10 ms segment that is reproduced in sequence to study the consequences of very long-term ejection (gray shaded area; see discussion in Section A.1).
Paper: “Extended Emission” from Fallback Accretion onto Merger Remnants
Authors: Carlo Musolino, Raphaël Duqué, Luciano Rezzolla
Figure caption: Same as Figure 1 but for the two TNTYST binaries.
Paper: “Extended Emission” from Fallback Accretion onto Merger Remnants
Authors: Carlo Musolino, Raphaël Duqué, Luciano Rezzolla
Figure caption: Mass histogram of the orbital energy in the bound ejecta counted over the entire simulation. For explanations on the lower bounds of these histograms, see Section 2.1.
Paper: “Extended Emission” from Fallback Accretion onto Merger Remnants
Authors: Carlo Musolino, Raphaël Duqué, Luciano Rezzolla
Figure caption: Comparison of mass distributions of orbital energy as measured for different detector positions in the domain. The histogram is calculated as in Figure 4, by placing the detector at different radii, as per the legend. Left: SFHO-q1.0 system. Right: SFHO-q.75 system.
Paper: “Extended Emission” from Fallback Accretion onto Merger Remnants
Authors: Carlo Musolino, Raphaël Duqué, Luciano Rezzolla
Figure caption: Radiation arising from the fallback flow as per our model of blackbody emission from the photosphere heated up by r-process nucleosynthesis (Section 3.2). In each panel, the temperature evolution was determined from the r-process heating starting from a Y  e  value measured at different latitudes in the fallback flow, as indicated above the panels. We present the luminosity in the Swift/BAT and Swift/XRT bands (colored solid and dashed lines, respectively) and the bolometric luminosity (black solid line). We also present the luminosity derived from the accretion rate (gray dotted line). In the panels corresponding to near-polar views (θ = 15°), we present the best-fit model of a flat power-law light curve to the XRT luminosity (gray dashed line; Equation (25)). For these panels, the best-fit parameters are reported in the figures. Finally, we show the XRT data for some GRBs with extended emission in the source frame, arbitrarily scaled in flux to compare with our model (colored points).
Paper: “Extended Emission” from Fallback Accretion onto Merger Remnants
Authors: Carlo Musolino, Raphaël Duqué, Luciano Rezzolla
Figure caption: Spacetime distribution of the density in the fallback outflow–inflow as determined by our semianalytical model (Section 3.1). The white part in the lower right corner is empty, because the bound material has not reached that altitude above the central object (Equation (20)). We present some fluid lines of the flow (white lines) and the photosphere used in the emission model (orange line). We show the surface of the detector sphere, where the fallback rate of ﹩{\dot{m}}_{\mathrm{FB}}\propto {t}^{-5/3}﹩ is enforced (gray segment; Equation (18)), and the leading edge of the outflow (gray dashed line).
Paper: “Extended Emission” from Fallback Accretion onto Merger Remnants
Authors: Carlo Musolino, Raphaël Duqué, Luciano Rezzolla
Figure caption: A schematic view of our model for the EM signature of the fallback flow. The fallback outflow–inflow (blue) is ejected underneath the unbound material (purple), where the kilonova signal is emitted (red photons). The fallback material emits X-rays (blue photons) that can either be absorbed and reprocessed in the kilonova ejecta (equatorial direction) or reach a distant observer by passing through the free way opened by the passing of the jet launched postmerger (polar direction). In this case, the fallback radiation appears as high-energy extended emission.
Paper: “Extended Emission” from Fallback Accretion onto Merger Remnants
Authors: Carlo Musolino, Raphaël Duqué, Luciano Rezzolla
Figure caption: Fallback accretion luminosity obtained by extending the ejection history of the TNTYST-q1.0 system. The solid lines represent the fallback accretion luminosity for different lengths of the ejection extension. The ejection segment that is reproduced to make up the extension is presented in Figure 7 (gray shaded region).
Paper: “Extended Emission” from Fallback Accretion onto Merger Remnants
Authors: Carlo Musolino, Raphaël Duqué, Luciano Rezzolla
Figure caption: Comparison between the fallback time estimated by a Newtonian description of the fallback orbits (t FB, N) and that estimated by a relativistic integration of the orbits in a Kerr spacetime (t FB, K). This comparison serves to justify our use of the Newtonian estimate throughout our study.