adsabs/AstroCLIMB huggingface dataset:
Paper: Early Stages of Galilean Moon Formation in a Water-depleted Environment
Authors: Olivier Mousis, A. Schneeberger, Jonathan I. Lunine, Christopher R. Glein, Alexis Bouquet, Steven D. Vance
Figure caption: Equilibrium dehydration curves of the serpentine polymorphs chrysotile and lizardite in the presence of solar composition material, where the carbon speciation is dominated by carbon monoxide. Water ice (Ih) condensation curves are shown for (blue curve) a solar composition case in which ∼33% of the water budget is in phyllosilicates, while the rest is present as water vapor; and for (orange curve) a case in which the water-vapor abundance has been enriched by a factor of 10 relative to the preceding case. The green curve depicts the P tot–T profile from our CPD model after 105 yr. At temperatures higher than the temperature of curve crossing, the dehydration of serpentine is thermodynamically favored. Water vapor will condense as water ice at disk temperatures below the SL temperature.
Paper: Hypervelocity Stars Track Back to the Galactic Center in Gaia DR3
Authors: Jiwei Liao, Cuihua Du, Hefan Li, Jun Ma, Jianrong Shi
Figure caption: The coordinate system of the figure is the positional angle of ascending node of the orbit vs. inclination of the orbit with respect to the line of sight. Filled blue circles identify orientation of orbital planes of S-stars around the GC from Gillessen et al. (2017), while the red curve shows a set of possible orientations of orbital planes consistent with Gaia DR3 6016819861087891456. The red curve also identifies the potential orbital plane of the secondary star of Gaia DR3 6016819861087891456 binary if it still orbits the SMBH and if it was ejected by Hills mechanism. The stars S83 and R44 are members of the clockwise stellar disk (Bartko et al. 2009; Yelda et al. 2014) at (104°, 126°) marked by the filled green circle and the dashed line, indicating a disk thickness of 16°.
Paper: Early Stages of Galilean Moon Formation in a Water-depleted Environment
Authors: Olivier Mousis, A. Schneeberger, Jonathan I. Lunine, Christopher R. Glein, Alexis Bouquet, Steven D. Vance
Figure caption: Equilibrium dehydration curves of the serpentine polymorphs chrysotile and lizardite, along with the vapor-pressure curve of water ice (Ih). Gray arrows represent examples of how changes in temperature and/or partial pressure of water vapor would make the indicated processes thermodynamically favorable.
Paper: Hypervelocity Stars Track Back to the Galactic Center in Gaia DR3
Authors: Jiwei Liao, Cuihua Du, Hefan Li, Jun Ma, Jianrong Shi
Figure caption: Panel (a) and panel (b) are the 3D backward orbits of Gaia DR3 6016819861087891456 and Gaia DR3 4094201527955913856 under four potential models, respectively. The orbits under each potential model overlap each other, and the points on the orbit closest to the GC are the same. The points on the orbit closest from the GC is the orbit turning points.
Paper: Astronomical Detection of the Interstellar Anion C10H− toward TMC-1 from the GOTHAM Large Program on the Green Bank Telescope
Authors: Anthony Remijan, Haley N. Scolati, Andrew M. Burkhardt, P. Bryan Changala, Steven B. Charnley, Ilsa R. Cooke, Martin A. Cordiner, Harshal Gupta, Eric Herbst, Kin Long Kelvin Lee, Ryan A. Loomis, Christopher N. Shingledecker, Mark A. Siebert, Ci Xue, Michael C. McCarthy, Brett A. McGuire
Figure caption: Individual lines of C10H− covered in the GOTHAM observations through 25 GHz (black). Both the spectra and the simulations have been smoothed to a resolution of 5.6 kHz (from the native 1.4 kHz full resolution) to better show potential features. The spectra for lines falling at higher frequencies are substantially noisier and have been omitted from the plot to reduce the number of panels. Simulations of C10H− emission using the parameters given in Table 2 are shown in colors, with the total simulation in red. The quantum numbers for each transition are given in the upper left of each panel, and the central frequency of the window (in the sky frame) is given in the top right. Each window is 6.0 km s−1 in total width.
Paper: Astronomical Detection of the Interstellar Anion C10H− toward TMC-1 from the GOTHAM Large Program on the Green Bank Telescope
Authors: Anthony Remijan, Haley N. Scolati, Andrew M. Burkhardt, P. Bryan Changala, Steven B. Charnley, Ilsa R. Cooke, Martin A. Cordiner, Harshal Gupta, Eric Herbst, Kin Long Kelvin Lee, Ryan A. Loomis, Christopher N. Shingledecker, Mark A. Siebert, Ci Xue, Michael C. McCarthy, Brett A. McGuire
Figure caption: Velocity stacked and matched filter spectra of C10H− from a jacknife analysis where the full catalog was split into two. The intensity scales are the S/Ns of the response functions when centered at a given velocity. The “zero” velocity corresponds to the channel with the highest intensity to account for blended spectroscopic transitions and variations in velocity component source sizes. (Left) The stacked spectra from the GOTHAM DR4 data are displayed in black, overlaid with the expected line profile in red from our MCMC fit to the data. The S/N is on a per-channel basis. (Right) Matched filter response obtained from cross correlating the simulated and observed velocity stacks in the left panel; the value annotated corresponds to the peak impulse response of the matched filter.
Paper: Astronomical Detection of the Interstellar Anion C10H− toward TMC-1 from the GOTHAM Large Program on the Green Bank Telescope
Authors: Anthony Remijan, Haley N. Scolati, Andrew M. Burkhardt, P. Bryan Changala, Steven B. Charnley, Ilsa R. Cooke, Martin A. Cordiner, Harshal Gupta, Eric Herbst, Kin Long Kelvin Lee, Ryan A. Loomis, Christopher N. Shingledecker, Mark A. Siebert, Ci Xue, Michael C. McCarthy, Brett A. McGuire
Figure caption: The abundance and column density of the C n H (left) and C n H− (right) families as observed by the GBT (black, solid, circles), simulated by NAUTILUS (blue, dashed, stars) at a model time of t = 2.5 × 105 yr, and predicted by machine learning (orange, dotted, ×s). The observed column density of C2H is taken from Pratap et al. (1997) with the Five College Radio Astronomical Observatory 14 m antenna.
Paper: Astronomical Detection of the Interstellar Anion C10H− toward TMC-1 from the GOTHAM Large Program on the Green Bank Telescope
Authors: Anthony Remijan, Haley N. Scolati, Andrew M. Burkhardt, P. Bryan Changala, Steven B. Charnley, Ilsa R. Cooke, Martin A. Cordiner, Harshal Gupta, Eric Herbst, Kin Long Kelvin Lee, Ryan A. Loomis, Christopher N. Shingledecker, Mark A. Siebert, Ci Xue, Michael C. McCarthy, Brett A. McGuire
Figure caption: Individual lines of C4H detected in the GOTHAM observations (black). Simulations of C4H emission using the parameters given in Table B1 are shown in colors, with the total simulation in red. The quantum numbers for each transition are given in the upper left of each panel, and the central frequency of the window (in the sky frame) is given in the top right. Each window is 4.0 km s−1 in total width.
Paper: Astronomical Detection of the Interstellar Anion C10H− toward TMC-1 from the GOTHAM Large Program on the Green Bank Telescope
Authors: Anthony Remijan, Haley N. Scolati, Andrew M. Burkhardt, P. Bryan Changala, Steven B. Charnley, Ilsa R. Cooke, Martin A. Cordiner, Harshal Gupta, Eric Herbst, Kin Long Kelvin Lee, Ryan A. Loomis, Christopher N. Shingledecker, Mark A. Siebert, Ci Xue, Michael C. McCarthy, Brett A. McGuire
Figure caption: Corner plot for C4H showing parameter covariances and marginalized posterior distributions for the C4H MCMC fit. The 16th, 50th, and 84th confidence intervals (corresponding to ±1σ for a Gaussian posterior distribution) are shown as vertical lines.
Paper: Astronomical Detection of the Interstellar Anion C10H− toward TMC-1 from the GOTHAM Large Program on the Green Bank Telescope
Authors: Anthony Remijan, Haley N. Scolati, Andrew M. Burkhardt, P. Bryan Changala, Steven B. Charnley, Ilsa R. Cooke, Martin A. Cordiner, Harshal Gupta, Eric Herbst, Kin Long Kelvin Lee, Ryan A. Loomis, Christopher N. Shingledecker, Mark A. Siebert, Ci Xue, Michael C. McCarthy, Brett A. McGuire
Figure caption: Corner plot for C10H− showing parameter covariances and marginalized posterior distributions for the C10H− MCMC fit. The 16th, 50th, and 84th confidence intervals (corresponding to ±1 sigma for a Gaussian posterior distribution) are shown as vertical lines.
Paper: Astronomical Detection of the Interstellar Anion C10H− toward TMC-1 from the GOTHAM Large Program on the Green Bank Telescope
Authors: Anthony Remijan, Haley N. Scolati, Andrew M. Burkhardt, P. Bryan Changala, Steven B. Charnley, Ilsa R. Cooke, Martin A. Cordiner, Harshal Gupta, Eric Herbst, Kin Long Kelvin Lee, Ryan A. Loomis, Christopher N. Shingledecker, Mark A. Siebert, Ci Xue, Michael C. McCarthy, Brett A. McGuire
Figure caption: Corner plot for C10H showing parameter covariances and marginalized posterior distributions for the C10H MCMC fit. The 16th, 50th, and 84th confidence intervals (corresponding to ±1σ for a Gaussian posterior distribution) are shown as vertical lines.
Paper: Astronomical Detection of the Interstellar Anion C10H− toward TMC-1 from the GOTHAM Large Program on the Green Bank Telescope
Authors: Anthony Remijan, Haley N. Scolati, Andrew M. Burkhardt, P. Bryan Changala, Steven B. Charnley, Ilsa R. Cooke, Martin A. Cordiner, Harshal Gupta, Eric Herbst, Kin Long Kelvin Lee, Ryan A. Loomis, Christopher N. Shingledecker, Mark A. Siebert, Ci Xue, Michael C. McCarthy, Brett A. McGuire
Figure caption: Simulated gas-phase abundance and column densities of the C n H (left) and C n H− (right) families from nautilus chemical models in comparison to the observed values with uncertainties shown as horizontal bars with hashed patterns. The time used in Figure 4 is shown as a vertical dashed gray line. The same hash and color scheme are used for molecules containing the same number of carbon atoms.
Paper: Astronomical Detection of the Interstellar Anion C10H− toward TMC-1 from the GOTHAM Large Program on the Green Bank Telescope
Authors: Anthony Remijan, Haley N. Scolati, Andrew M. Burkhardt, P. Bryan Changala, Steven B. Charnley, Ilsa R. Cooke, Martin A. Cordiner, Harshal Gupta, Eric Herbst, Kin Long Kelvin Lee, Ryan A. Loomis, Christopher N. Shingledecker, Mark A. Siebert, Ci Xue, Michael C. McCarthy, Brett A. McGuire
Figure caption: Individual lines of C8H− detected in the GOTHAM observations (black). Simulations of C8H− emission using the parameters given in Table G1 are shown in colors, with the total simulation in red. The quantum numbers for each transition are given in the upper left of each panel, and the central frequency of the window (in the sky frame) is given in the top right. Each window is 4.0 km s−1 in total width.
Paper: Astronomical Detection of the Interstellar Anion C10H− toward TMC-1 from the GOTHAM Large Program on the Green Bank Telescope
Authors: Anthony Remijan, Haley N. Scolati, Andrew M. Burkhardt, P. Bryan Changala, Steven B. Charnley, Ilsa R. Cooke, Martin A. Cordiner, Harshal Gupta, Eric Herbst, Kin Long Kelvin Lee, Ryan A. Loomis, Christopher N. Shingledecker, Mark A. Siebert, Ci Xue, Michael C. McCarthy, Brett A. McGuire
Figure caption: Corner plot for C8H− showing parameter covariances and marginalized posterior distributions for the C8H− MCMC fit. The 16th, 50th, and 84th confidence intervals (corresponding to ±1σ for a Gaussian posterior distribution) are shown as vertical lines.
Paper: Radiation Transport Two-temperature GRMHD Simulations of Warped Accretion Disks
Authors: M. T. P. Liska, N. Kaaz, G. Musoke, A. Tchekhovskoy, O. Porth
Figure caption: Panels (a) and (b): spacetime diagrams of the density, ρ, and warp amplitude, ψ. The warp amplitude peaks where the disk is about to tear or has already torn. Since dissipation is enhanced in warps, a maximum in the warp amplitude correspond to a minimum in the density. The main tearing event is denoted by black dotted lines. Panels (c) and (d): spacetime diagrams of the electron, T  e , and ion, T  i , temperatures. The ion and electron temperatures correlate with the warp amplitude and anticorrelate with the density. Close to the BH and in the tear the ions are significantly hotter than the electrons since Coulomb collisions are unable to equilibrate the ion and eletron temperatures. Panels (e) and (f): spacetime diagrams of the tilt, ﹩{ \mathcal T }﹩, and precession, ﹩{ \mathcal P }﹩, angle of the disk. Around t ∼ 36,500 r  g /c a disk tears off and precesses for ≲two periods, during which it gradually aligns with the BH spin axis.
Paper: Radiation Transport Two-temperature GRMHD Simulations of Warped Accretion Disks
Authors: M. T. P. Liska, N. Kaaz, G. Musoke, A. Tchekhovskoy, O. Porth
Figure caption: The first demonstration of disk tearing in a radiation-pressure-supported accretion disk, as seen through isocountour 3D renderings of the density at three different times. Left panel: the disk at t = 28,955 r  g /c forms a rigid body that is warped, but shows no differential precession. Middle panel: the disk tears off a precessing inner disk at t = 31,000 r  g  that precesses for two periods between t = 35,000 r  g /c and t = 37,000 r  g /c. While precessing, the inner disk aligns with the BH, shrinking in size until it fully disappears. Right pane: the disk forms a new tear at r ∼ 25 r  g /c around t ∼ 45,000 r  g /c, and the tearing process repeats.
Paper: Radiation Transport Two-temperature GRMHD Simulations of Warped Accretion Disks
Authors: M. T. P. Liska, N. Kaaz, G. Musoke, A. Tchekhovskoy, O. Porth
Figure caption: A volume rendering of the density during the main tearing event at t = 37,026 r  g /c. The red plane cuts the disk at the ϕ = 0 surface. Streamers from the outer disk (green) deposit low-angular-momentum gas onto the inner disk (blue). This causes the inner accretion disk to shrink in size (Kaaz et al. 2022).
Paper: SN 2019ewu: A Peculiar Supernova with Early Strong Carbon and Weak Oxygen Features from a New Sample of Young SN Ic Spectra
Authors: Marc Williamson, Christian Vogl, Maryam Modjaz, Wolfgang Kerzendorf, Jaladh Singhal, Teresa Boland, Jamison Burke, Zhihao Chen, Daichi Hiramatsu, Lluís Galbany, Estefania Padilla Gonzalez, D. Andrew Howell, Saurabh W. Jha, Lindsey A. Kwok, Curtis McCully, Megan Newsome, Craig Pellegrino, Jeonghee Rho, Giacomo Terreran, Xiaofeng Wang
Figure caption: (Left) The O I 7774 absorption line pseudo-equivalent width (pEW) as a function of time for the GSP SN Ic sample (colors) compared to the distribution of SNe Ic from the MGS (gray). SN 2019ewu has particularly weak oxygen absorption at early times. (Right) (B−V) colors calculated directly from the GSP spectra using the ST-mag system. All spectra are dereddened to correct for MW extinction but may be contaminated by host-galaxy extinction. SN 2019yz and SN 2021do are excluded because their spectra show narrow Na I D lines indicative of host-galaxy extinction. SN 2019ewu and SN 2020akf show particularly blue early-time spectra but different oxygen line strengths.(The data used to create this figure are available.)
Paper: SN 2019ewu: A Peculiar Supernova with Early Strong Carbon and Weak Oxygen Features from a New Sample of Young SN Ic Spectra
Authors: Marc Williamson, Christian Vogl, Maryam Modjaz, Wolfgang Kerzendorf, Jaladh Singhal, Teresa Boland, Jamison Burke, Zhihao Chen, Daichi Hiramatsu, Lluís Galbany, Estefania Padilla Gonzalez, D. Andrew Howell, Saurabh W. Jha, Lindsey A. Kwok, Curtis McCully, Megan Newsome, Craig Pellegrino, Jeonghee Rho, Giacomo Terreran, Xiaofeng Wang
Figure caption: A comparison of the first two spectra of SN 2019ewu (black) to SNe Ic from the MGS at a similar phase relative to the V-band maximum (colors), as well as spectra from SN Ic 2020oi (Rho et al. 2021). The spectra shown here are continuum removed by SNID to facilitate line-shape comparison. The left figure highlights the broad P Cygni feature in SN 2019ewu that has not been seen before in early-time SN Ic spectra, while the right figure shows how the feature evolves one week later to develop a doublet shape.
Paper: SN 2019ewu: A Peculiar Supernova with Early Strong Carbon and Weak Oxygen Features from a New Sample of Young SN Ic Spectra
Authors: Marc Williamson, Christian Vogl, Maryam Modjaz, Wolfgang Kerzendorf, Jaladh Singhal, Teresa Boland, Jamison Burke, Zhihao Chen, Daichi Hiramatsu, Lluís Galbany, Estefania Padilla Gonzalez, D. Andrew Howell, Saurabh W. Jha, Lindsey A. Kwok, Curtis McCully, Megan Newsome, Craig Pellegrino, Jeonghee Rho, Giacomo Terreran, Xiaofeng Wang
Figure caption: Fe II 5169 absorption velocities measured as a function of ﹩{t}_{{V}_{\max }}﹩ for the GSP SN Ic sample (colored lines) compared to the mean ±1 standard deviation velocity of the SN Ic sample from Liu et al. (2016) shown as the gray band. Velocities are calculated only when Fe II 5169 can be clearly identified from the Fe doublet. A clear identification of Fe II 5169 cannot be made for SN 2019yz after early times due to contamination from an emergent feature.(The data used to create this figure are available.)
Paper: SN 2019ewu: A Peculiar Supernova with Early Strong Carbon and Weak Oxygen Features from a New Sample of Young SN Ic Spectra
Authors: Marc Williamson, Christian Vogl, Maryam Modjaz, Wolfgang Kerzendorf, Jaladh Singhal, Teresa Boland, Jamison Burke, Zhihao Chen, Daichi Hiramatsu, Lluís Galbany, Estefania Padilla Gonzalez, D. Andrew Howell, Saurabh W. Jha, Lindsey A. Kwok, Curtis McCully, Megan Newsome, Craig Pellegrino, Jeonghee Rho, Giacomo Terreran, Xiaofeng Wang
Figure caption: Spectral time series for the six SNe Ic analyzed in this work (corrected for MW but not host-galaxy extinction). Dashed vertical lines mark the Na 5896 and O 7774 lines, and phases are relative to the date of the V-band maximum. All SNe with the exception of SN 2021do were discovered early enough to obtain spectra more than 1 week prior to maximum light. We note that SN 2019ewu and SN 2020akf have blue featureless spectra at very early times for SNe Ic, which may be related to their slow-developing and weak O 7774 feature compared to the other SNe.
Paper: SN 2019ewu: A Peculiar Supernova with Early Strong Carbon and Weak Oxygen Features from a New Sample of Young SN Ic Spectra
Authors: Marc Williamson, Christian Vogl, Maryam Modjaz, Wolfgang Kerzendorf, Jaladh Singhal, Teresa Boland, Jamison Burke, Zhihao Chen, Daichi Hiramatsu, Lluís Galbany, Estefania Padilla Gonzalez, D. Andrew Howell, Saurabh W. Jha, Lindsey A. Kwok, Curtis McCully, Megan Newsome, Craig Pellegrino, Jeonghee Rho, Giacomo Terreran, Xiaofeng Wang
Figure caption: (Left) A TARDIS model (blue) for the first spectrum of SN 2019ewu (black). The primary features of the model are labeled (O II, Si III, C II). (Right) A comparison of the model and observed spectrum from the left panel with continuum removed by SNID to highlight the ability of the model to reproduce the lines seen in the data. The P Cygni–shaped feature in the SN 2019ewu spectrum can be produced in the model without any hydrogen.
Paper: SN 2019ewu: A Peculiar Supernova with Early Strong Carbon and Weak Oxygen Features from a New Sample of Young SN Ic Spectra
Authors: Marc Williamson, Christian Vogl, Maryam Modjaz, Wolfgang Kerzendorf, Jaladh Singhal, Teresa Boland, Jamison Burke, Zhihao Chen, Daichi Hiramatsu, Lluís Galbany, Estefania Padilla Gonzalez, D. Andrew Howell, Saurabh W. Jha, Lindsey A. Kwok, Curtis McCully, Megan Newsome, Craig Pellegrino, Jeonghee Rho, Giacomo Terreran, Xiaofeng Wang
Figure caption: A subset of the SN 2019ewu spectral time series (black) at −12, −5, 0, and 16 days relative to the V-band maximum. Colored spectra show particularly good spectral matches identified by SNID at each phase. SN 2019ewu initially matches with SN II before developing broad lines typical of SN Ic-bl, before settling as an SN Ic.
Paper: A Potential Site for Wide-orbit Giant Planet Formation in the IM Lup Disk
Authors: Arthur D. Bosman, Johan Appelgren, Edwin A. Bergin, Michiel Lambrechts, Anders Johansen
Figure caption: Left: required dust mass to suppress the C18O in the inner 20 au of IM Lup as a function of the dust scale height. Crosses assume a dust size distribution from 0.005 μm to the listed size with a power-law slope of −3.5. Squares assume all the dust is a single size, 0.2 mm, which yields the highest opacity at 1.3 mm. Blue vertical line shows the maximal total refractory mass in the IM Lup disk. Right: same as on the left, but the H  d /H  g  converted into a vertical mixing α assuming the dust of 0.2 mm size is dominating the opacity and needs to be elevated to the listed Hd /Hg  (Johansen et al. 2014). Points with arrows take the mass for H  d /H  g  = 1, and show the α for H  d /H  g  = 0.99, as an infinite α is required for H  d /H  g  = 1. A high α > 0.001 is required when a full dust size distribution is assumed. Only under the assumption that the dust is 0.2 mm sized will α < 10−3 solutions be possible.
Paper: A Potential Site for Wide-orbit Giant Planet Formation in the IM Lup Disk
Authors: Arthur D. Bosman, Johan Appelgren, Edwin A. Bergin, Michiel Lambrechts, Anders Johansen
Figure caption: Surface densities of the gas and dust of IM Lup. The solid gray lines show the gas and dust from the model from Zhang et al. (2021), which is the baseline for our DALI models. The dashed–dotted gray line shows the minimal amount of dust required if purely 0.2 mm particles are responsible for the 1.3 mm dust emission. In the inner 40 au, the dust is optically thick and thus the derived surface density is uncertain. Dark and light blue lines show the predictions of our drift model for 1 mm, assuming a global gas-to-dust ratio of 100, and 0.2 mm grains, assuming a global gas-to-dust ratio of 1000, respectively (see Appendix B). Both models are taken at 0.6 Myr, the time at which the 1 mm grains have a large pileup in the inner 20 au. The dark red arrow shows the limit for 400 M ⊕ within 20 au, as derived previously (Bosman et al. 2021). Our dust model predicts that we can create an inner-disk pileup with significant mass in the inner disk with 1 mm grains, while just 10% of the total dust mass in 0.2 mm grains leaves enough opacity in the outer disk to explain the continuum emission further out in the disk.
Paper: A Potential Site for Wide-orbit Giant Planet Formation in the IM Lup Disk
Authors: Arthur D. Bosman, Johan Appelgren, Edwin A. Bergin, Michiel Lambrechts, Anders Johansen
Figure caption: Top: the dimensionless cooling time t coolΩk, assuming a VSI wavelength mode of λ/H = 0.1. Below a critical cooling time (red), the disk cools quickly enough that the VSI can become active. The sensitivity of the VSI-active region on opacity (κ KB) is illustrated by increasing (dashed) or decreasing (dotted) the opacity by a factor of 2. Bottom: the effect of VSI turbulence in the inner disk on the scale height of millimeter-sized particles. The gas scale height is shown in blue, while the millimeter-sized dust scale height is shown in black for our nominal opacity. Also, here the sensitivity on the opacity is shown with dashed and dotted curves.
Paper: A Cosmological Fireball with 16% Gamma-Ray Radiative Efficiency
Authors: Liang Li, Yu Wang, Felix Ryde, Asaf Pe'er, Bing Zhang, Sylvain Guiriec, Alberto J. Castro-Tirado, D. Alexander Kann, Magnus Axelsson, Kim Page, Péter Veres, P. N. Bhat
Figure caption: Pulse-wise properties of GRB 190114C. (a) Temporal evolutions of the photospheric radius r ph (violet), the saturation radius r s (orange), and the nozzle radius r 0 (cyan). (b) Temporal evolution of the parameter ﹩{\mathfrak{R}}﹩. (c) Temporal evolutions of the blackbody energy flux (F BB) and the total energy flux (F tot). (d) The total energy flux (F tot) vs. the blackbody energy flux (F BB). The color notations are the same as in Figure 6.