adsabs/AstroCLIMB huggingface dataset:
Paper: The Hubble Space Telescope Survey of M31 Satellite Galaxies. I. RR Lyrae–based Distances and Refined 3D Geometric Structure
Authors: Alessandro Savino, Daniel R. Weisz, Evan D. Skillman, Andrew Dolphin, Nitya Kallivayalil, Andrew Wetzel, Jay Anderson, Gurtina Besla, Michael Boylan-Kolchin, James S. Bullock, Andrew A. Cole, Michelle L. M. Collins, M. C. Cooper, Alis J. Deason, Aaron L. Dotter, Mark Fardal, Annette M. N. Ferguson, Tobias K. Fritz, Marla C. Geha, Karoline M. Gilbert, Puragra Guhathakurta, Rodrigo Ibata, Michael J. Irwin, Myoungwon Jeon, Evan Kirby, Geraint F. Lewis, Dougal Mackey, Steven R. Majewski, Nicolas Martin, Alan McConnachie, Ekta Patel, R. Michael Rich, Joshua D. Simon, Sangmo Tony Sohn, Erik J. Tollerud, Roeland P. van der Marel
Figure caption: (a) Sky projection (in the galactic coordinate system of Conn et al. 2012) of the M31 satellites, color-coded by absolute luminosity, as seen from the center of M31, using the distance data of Conn et al. (2012). The gray lines represent the uncertainties in the sky position. The direction of the MW is also reported. (b) The same as panel (a), but using the distances calculated in this paper. The comparison illustrates the improvement in sample size and distance precision of our compilation. The few remaining galaxies with large positional uncertainties are those that lie in close proximity to M31 (D 31 ≲ 60 kpc).
Paper: The Hubble Space Telescope Survey of M31 Satellite Galaxies. I. RR Lyrae–based Distances and Refined 3D Geometric Structure
Authors: Alessandro Savino, Daniel R. Weisz, Evan D. Skillman, Andrew Dolphin, Nitya Kallivayalil, Andrew Wetzel, Jay Anderson, Gurtina Besla, Michael Boylan-Kolchin, James S. Bullock, Andrew A. Cole, Michelle L. M. Collins, M. C. Cooper, Alis J. Deason, Aaron L. Dotter, Mark Fardal, Annette M. N. Ferguson, Tobias K. Fritz, Marla C. Geha, Karoline M. Gilbert, Puragra Guhathakurta, Rodrigo Ibata, Michael J. Irwin, Myoungwon Jeon, Evan Kirby, Geraint F. Lewis, Dougal Mackey, Steven R. Majewski, Nicolas Martin, Alan McConnachie, Ekta Patel, R. Michael Rich, Joshua D. Simon, Sangmo Tony Sohn, Erik J. Tollerud, Roeland P. van der Marel
Figure caption: Difference between the distance modulus calculated in this paper and literature values from the compilations of McConnachie et al. (2005; purple circles), Conn et al. (2012; orange diamonds), and Weisz et al. (2019b; cyan triangles). The thick colored portion of the error bar shows the contribution to the total error budget coming from our distance measurements. The galaxies are ordered in descending order of absolute luminosity. The vertical dotted line marks M  V  = −9.5.
Paper: The Hubble Space Telescope Survey of M31 Satellite Galaxies. I. RR Lyrae–based Distances and Refined 3D Geometric Structure
Authors: Alessandro Savino, Daniel R. Weisz, Evan D. Skillman, Andrew Dolphin, Nitya Kallivayalil, Andrew Wetzel, Jay Anderson, Gurtina Besla, Michael Boylan-Kolchin, James S. Bullock, Andrew A. Cole, Michelle L. M. Collins, M. C. Cooper, Alis J. Deason, Aaron L. Dotter, Mark Fardal, Annette M. N. Ferguson, Tobias K. Fritz, Marla C. Geha, Karoline M. Gilbert, Puragra Guhathakurta, Rodrigo Ibata, Michael J. Irwin, Myoungwon Jeon, Evan Kirby, Geraint F. Lewis, Dougal Mackey, Steven R. Majewski, Nicolas Martin, Alan McConnachie, Ekta Patel, R. Michael Rich, Joshua D. Simon, Sangmo Tony Sohn, Erik J. Tollerud, Roeland P. van der Marel
Figure caption: Difference in the distance modulus (top panel) and in the distance to M31 (bottom panel) resulting from the inclusion of RRc variables in our fits. Purple circles and cyan diamonds represent galaxies with F606W/F814W and F475W/F814W data, respectively.
Paper: The Hubble Space Telescope Survey of M31 Satellite Galaxies. I. RR Lyrae–based Distances and Refined 3D Geometric Structure
Authors: Alessandro Savino, Daniel R. Weisz, Evan D. Skillman, Andrew Dolphin, Nitya Kallivayalil, Andrew Wetzel, Jay Anderson, Gurtina Besla, Michael Boylan-Kolchin, James S. Bullock, Andrew A. Cole, Michelle L. M. Collins, M. C. Cooper, Alis J. Deason, Aaron L. Dotter, Mark Fardal, Annette M. N. Ferguson, Tobias K. Fritz, Marla C. Geha, Karoline M. Gilbert, Puragra Guhathakurta, Rodrigo Ibata, Michael J. Irwin, Myoungwon Jeon, Evan Kirby, Geraint F. Lewis, Dougal Mackey, Steven R. Majewski, Nicolas Martin, Alan McConnachie, Ekta Patel, R. Michael Rich, Joshua D. Simon, Sangmo Tony Sohn, Erik J. Tollerud, Roeland P. van der Marel
Figure caption: Difference in the distance modulus (top panel) and in the distance to M31 (bottom panel) resulting from the omission of the empirical correction term (Equation (3)). Purple circles and cyan diamonds represent galaxies with F606W/F814W and F475W/F814W data, respectively.
Paper: Greater Climate Sensitivity and Variability on TRAPPIST-1e than Earth
Authors: Assaf Hochman, Paolo De Luca, Thaddeus D. Komacek
Figure caption: Phase plane diagrams of the dynamical systems metrics d (local dimension) and θ (inverse persistence) with varying pCO2 (“LOW,” blue; “MID,” green; “HIGH,” red; see Section 3.1) for TRAPPIST-1e (left column), EARTH analog (middle column; note reduced y-axis scale), and ERA5 reanalysis as reference (right column; note extended x-axis scale). The regions used to compute the dynamical systems metrics are displayed in Figure 1(a). The dynamical systems metrics are computed for the T max variable.
Paper: Greater Climate Sensitivity and Variability on TRAPPIST-1e than Earth
Authors: Assaf Hochman, Paolo De Luca, Thaddeus D. Komacek
Figure caption: Difference (Δ) between Earth analog and TRAPPIST-1e (a, d, g) spatial extremes for maximum temperature at the surface (T max in °C). (b, e, h) are the same as (a, d, g) but for ERA5 reanalysis and TRAPPIST-1e, and (c, f, i) for ERA5 reanalysis and the Earth analog. The different pCO2 scenarios are described in Section 3.1 and are referred to as “Low” (10−2 Bar), “Mid” (10−1 Bar), and “High” (1 Bar). White regions represent areas without extremes and nonstatistically significant values (p-value ≥ 0.01) following a two-tailed Wilcoxon rank-sum test and a Bonferroni correction (see Section 3.4).
Paper: Greater Climate Sensitivity and Variability on TRAPPIST-1e than Earth
Authors: Assaf Hochman, Paolo De Luca, Thaddeus D. Komacek
Figure caption: Box plots of daily maximum temperature (°C) of mean extreme anomalies computed with respect to ERA5 reanalysis climatology (1979–2020) for Earth analog (blue), TRAPPIST-1e (red), and ERA5 (gray). (b–g) Regions described in Figure 1(a). The different pCO2 scenarios are described in Section 3.1 and are referred to as “Low” (10−2 Bar), “Mid” (10−1 Bar), and “High” (1 Bar). Extremes are computed for each grid box as daily values exceeding the 95th percentile. The box plots show the 25th quantile, median, and 75th quantile. Black dots are outliers.
Paper: Greater Climate Sensitivity and Variability on TRAPPIST-1e than Earth
Authors: Assaf Hochman, Paolo De Luca, Thaddeus D. Komacek
Figure caption: Cumulative distribution functions of median daily maximum temperature (T max in °C) for Earth analog (solid blue lines), TRAPPIST-1e (solid red lines), and ERA5 (dashed black lines). (b–g) Regions described in Figure 1(a). The different pCO2 scenarios are described in Section 3.1 and are referred to as “Low” (–10−2 Bar), “Mid” (10−1 Bar), and “High” (1 Bar).
Paper: Greater Climate Sensitivity and Variability on TRAPPIST-1e than Earth
Authors: Assaf Hochman, Paolo De Luca, Thaddeus D. Komacek
Figure caption: Same as Figure 3 but for precipitation (Prec in mm d−1).
Paper: Greater Climate Sensitivity and Variability on TRAPPIST-1e than Earth
Authors: Assaf Hochman, Paolo De Luca, Thaddeus D. Komacek
Figure caption: Same as Figure 8 but for daily total precipitation (Prec in mm d−1).
Paper: Greater Climate Sensitivity and Variability on TRAPPIST-1e than Earth
Authors: Assaf Hochman, Paolo De Luca, Thaddeus D. Komacek
Figure caption: Time series for annual global means and extreme (95th percentile, Q95) of daily maximum temperature (a, b; T max in °C) and precipitation (c, d; Prec in mm d−1) for Earth analog (solid blue lines), TRAPPIST-1e (solid red lines), and ERA5 (dashed black lines). The different pCO2 scenarios are described in Section 3.1 and are referred to as “Low” (10−2 Bar), “Mid” (10−1 Bar), and “High” (1 Bar).
Paper: Greater Climate Sensitivity and Variability on TRAPPIST-1e than Earth
Authors: Assaf Hochman, Paolo De Luca, Thaddeus D. Komacek
Figure caption: Same as Figure 5 but for precipitation (Prec in mm d−1).
Paper: Greater Climate Sensitivity and Variability on TRAPPIST-1e than Earth
Authors: Assaf Hochman, Paolo De Luca, Thaddeus D. Komacek
Figure caption: Same as Figure 7 but for daily total precipitation (Prec in mm d−1).
Paper: Thermal Evolution and Magnetic History of Rocky Planets
Authors: Jisheng Zhang, Leslie A. Rogers
Figure caption: Time evolution of the fraction of the total mantle mass in liquid phase (x  m ) in planets with CMF = 0.326 (top row), CMF = 0.7 (bottom row), T eq = 255 K (left column), T eq = 1350 K (middle column), and T eq = 2500 K (right column). Blue and red curves indicate planets with 1 and 3 M ⊕, respectively. T eq has the major influence on the evolution of the magma ocean. The lifetime and the depth of the magma ocean have a slight dependence on the planetary mass and CMF, which together determine the mass of the mantle.
Paper: Thermal Evolution and Magnetic History of Rocky Planets
Authors: Jisheng Zhang, Leslie A. Rogers
Figure caption: Evolution of (a) surface heat flow (F surf) and (b) fraction of total mantle mass in the liquid phase (x  m ) for a 1 M ⊕ planet with CMF = 0.326 and T eq = 255 K. The melting curve is taken to be Earth’s mantle solidus (Hirschmann 2000; Andrault et al. 2011) instead of Equation (3). Brown curves are for the case with no atmosphere and blue curves are for the case with a degassed gray atmosphere with an initial water content of 4.3 × 10−2 wt% and CO2 content of 1.4 × 10−2 wt%. Dotted, dashed–dotted, and solid curves represent the fully molten stage, the partially molten stage, and the mush stage.
Paper: Thermal Evolution and Magnetic History of Rocky Planets
Authors: Jisheng Zhang, Leslie A. Rogers
Figure caption: Evolution of (a) surface heat flow, (b) radial temperature profiles, (c) heat flux at the CMB, and (d) solid inner core size for a 1 M ⊕ planet with CMF = 0.326 and T eq = 255 K. Melting temperature of iron is reduced by 20% artificially to mimic the influence of impurities in the iron core (see text in Section 3.2). The surface heat flow reduces to ∼0.07 W/m2 (corresponding to ∼36.5 TW) and the solid inner core size increases to ∼1300 km at 4.5 Gyr.
Paper: Thermal Evolution and Magnetic History of Rocky Planets
Authors: Jisheng Zhang, Leslie A. Rogers
Figure caption: Time evolution of (a) dynamo source region and (b) magnetic Reynolds number profiles of the magma ocean for a 1 M ⊕ planet with CMF = 0.326. The dotted line in (b) indicates the threshold above which the region can potentially support a dynamo. The dynamo source region starts off as the entire fully molten mantle and is confined to the subsurface magma ocean only ∼150 yr after the start. The size of the region while confined to the subsurface magma ocean reaches its maximum of 890 km at ∼1 Myr and vanishes ∼40 million years.
Paper: Thermal Evolution and Magnetic History of Rocky Planets
Authors: Jisheng Zhang, Leslie A. Rogers
Figure caption: Evolution of (a) surface heat flow, (b) melt fraction distribution, (c) fraction of the total mantle mass in the liquid phase, and (d) heat flux at the CMB for a 1 M ⊕ planet with CMF = 0.326 and T eq = 255 K. The planetary radius and core radius start off at 6600 km and 3424 km, and decrease to 6400 km and 3409 km, respectively. The subsurface magma ocean reaches its maximum size of 1277 km at an age of ∼1 million years and fully solidifies by ∼150 million years
Paper: Milky Way Zero-point Calibration of the JAGB Method: Using Thermally Pulsing AGB Stars in Galactic Open Clusters
Authors: Barry F. Madore, Wendy L. Freedman, Abigail J. Lee, Kayla Owens
Figure caption: The J-band luminosity function (blue line) for the JAGB stars (blue points) seen in Figure 1. The mean absolute magnitude (M ☉ = −6.40 mag) is shown by the vertical red line. The bold, dashed black vertical line to the right is the absolute J-band mean magnitude for the MW carbon stars individually calibrated by Lee et al. (2021) using Gaia EDR3 parallaxes. The black curve is a Gaussian with 1σ of ±0.35 mag and a modal magnitude of −6.35 mag, fit to the centrally located data between −7.0 and −5.5 mag only.
Paper: Thermal Evolution and Magnetic History of Rocky Planets
Authors: Jisheng Zhang, Leslie A. Rogers
Figure caption: Model predicted radial density profile at 4.5 Gyr and comparison to the result from PREM (Dziewonski & Anderson 1981). Our model predicted a higher density in the iron core due to the lack of light impurities, which results in a slightly smaller iron core size. The model predicted planetary radius is in excellent agreement with the PREM result.
Paper: Thermal Evolution and Magnetic History of Rocky Planets
Authors: Jisheng Zhang, Leslie A. Rogers
Figure caption: Algorithm of the model. Initial profiles are prepared step 1. Subsequent updates in temperature, melt fraction and structural profiles are carried out by iterating steps 2 and 3.
Paper: The Solar Probe ANalyzer—Ions on the Parker Solar Probe
Authors: Roberto Livi, Davin E. Larson, Justin C. Kasper, Robert Abiad, A. W. Case, Kristopher G. Klein, David W. Curtis, Gregory Dalton, Michael Stevens, Kelly E. Korreck, George Ho, Miles Robinson, Chris Tiu, Phyllis L. Whittlesey, Jaye L. Verniero, Jasper Halekas, James McFadden, Mario Marckwordt, Amanda Slagle, Mamuda Abatcha, Ali Rahmati, Michael D. McManus
Figure caption: Left: Parker Solar Probe spacecraft with the SPAN-A sensor highlighted in the red box. Right: Mollweide projection of the SPAN-I field of view, including partial obstruction of the spacecraft and its TPS (red). The projection is based on the look direction of the anodes in ϕ and the deflector angles in θ.
Paper: The Solar Probe ANalyzer—Ions on the Parker Solar Probe
Authors: Roberto Livi, Davin E. Larson, Justin C. Kasper, Robert Abiad, A. W. Case, Kristopher G. Klein, David W. Curtis, Gregory Dalton, Michael Stevens, Kelly E. Korreck, George Ho, Miles Robinson, Chris Tiu, Phyllis L. Whittlesey, Jaye L. Verniero, Jasper Halekas, James McFadden, Mario Marckwordt, Amanda Slagle, Mamuda Abatcha, Ali Rahmati, Michael D. McManus
Figure caption: Left: SPAN-A flight module with the right (SPAN-I) and left (SPAN-E) ESA. SPAN-I consists of an ESA with deflectors followed by a titanium TOF section for mass-per-charge discrimination. Right: SPAN-I separated from the main SPAN-A unit.
Paper: Breaking Correlation in the Inflow Parameters of Interstellar Neutral Gas in Direct-sampling Observations
Authors: M. Bzowski, M. A. Kubiak, E. Möbius, N. A. Schwadron
Figure caption: Simulated and actual correlation tube for the ISN He observation conditions for IBEX-Lo. A projection of the tube in the longitude–speed plane in the four-dimensional parameter space is shown. The gray-shaded region bound by the dashed and dashed–dotted lines marks the simulated correlation lines for DOYs 22 and 57, which represent the typical time interval of ISN He observations by IBEX-Lo each year. The maximum of the observed flux occurs at DOY 37 (gray solid line, IBEX max). The gray ellipse represents the uncertainty of the flow parameters typically obtained for IBEX-Lo observations collected during one observation season (a 3σ uncertainty). The blue line represents the correlation tube actually obtained from analysis of IBEX observations by Bzowski et al. (2015). The gray dots represent the speed and ecliptic longitude from the correlated parameter sets listed in the first two rows in Table 1 (the speed–direction correlation). The black dots illustrate a projection on the (speed–longitude) parameter-space subspace of the parameter sets from the last two rows in Table 1, corresponding to the parameter correlation by the Mach number. Clearly, the latter two points are selected to be far away from the correlation tube for the speed–direction correlation tube.
Paper: Breaking Correlation in the Inflow Parameters of Interstellar Neutral Gas in Direct-sampling Observations
Authors: M. Bzowski, M. A. Kubiak, E. Möbius, N. A. Schwadron
Figure caption: Left panel: simulated correlation tubes projected on the longitude–speed plane for uniformly spaced DOYs during the first half of the calendar year. The IBEX max correlation line, copied from Figure 2, is drawn in blue. The gray ellipses are cartoon illustrations of the correlation tubes for individual correlation lines. The intersection of these regions, visible as the dark region near the center, illustrates the reduction of the parameter uncertainties, expected when observations taken during several well-separated time intervals during the year are available. Right panel: correlation tubes projected on the longitude-latitude plane, with identical color coding to that in the left panel. Additionally, the broken line, almost coincident with the line for DOY 127, connects the longitude and latitude of the flow directions of the primary ISN He and the Warm Breeze, i.e., the secondary population of interstellar He.
Paper: Breaking Correlation in the Inflow Parameters of Interstellar Neutral Gas in Direct-sampling Observations
Authors: M. Bzowski, M. A. Kubiak, E. Möbius, N. A. Schwadron
Figure caption: Two series of the normalized flux of ISN He for selected DOYs, illustrating the feasibility of breaking the correlation of the ISN flow parameters. The capability of adjusting the elongation angle of the instrument boresight to the spacecraft spin axis is used. (1) Dots: the elongation angle set always follows the peak of the primary population of ISN gas. (2) Squares: the elongation is changed stepwise with time and maintained to be constant during prolonged intervals. The color code and the format of the figure are identical to those used in Figure 5. Dots are scaled upward by a factor of two to improve the visibility. The DOYs and elongations are listed in the panels.
Paper: Breaking Correlation in the Inflow Parameters of Interstellar Neutral Gas in Direct-sampling Observations
Authors: M. Bzowski, M. A. Kubiak, E. Möbius, N. A. Schwadron
Figure caption: Two series of simulated normalized fluxes of ISN He for selected DOYs, corresponding to the IBEX ISN observation season: (1) for the boresight adjusted daily to follow the peak of ISN He (dots, upper set of lines), and (2) simulated for an IBEX-like viewing geometry (squares, bottom set of lines), i.e., with the boresight inclined at 90° to the spin axis (ε = 90). Three cases of the degenerate inflow parameters taken from Table 1 are drawn: the baseline (black), degen 1 (blue), and degen 2 (green). The horizontal axis represents the spacecraft spin angle. The vertical axis is dimensionless. The variable-elongation case is scaled upward by a factor of two to improve the visibility. Discerning the three lines for a given ε requires a strong magnification of the figure because the normalized fluxes are almost identical between the three degenerate parameter sets. Note that the two line sets drawn for DOY 29 are identical. The DOYs of the simulations are listed in the blue color at the bottom of the panels, and the elongation angles of the boresight from the spacecraft spin axis ε used for the two groups of simulations in each panels are listed at the corresponding line groups.
Paper: Breaking Correlation in the Inflow Parameters of Interstellar Neutral Gas in Direct-sampling Observations
Authors: M. Bzowski, M. A. Kubiak, E. Möbius, N. A. Schwadron
Figure caption: Example plots of orbits that impact at an instrument moving with Earth from identical directions but with different speeds. The black circle represents Earth’s orbit; Earth is moving counterclockwise. When the instrument is at the locations indicated by the dotted radius-vectors and the DOY labels, it is hit by three atoms approaching from the same direction but with different speeds. The plot is drawn assuming that one of these atoms has the velocity vector far away from the Sun identical to the inflow velocity of ISN gas. The other two orbits impact the instrument with a speed greater (black) or smaller (green) by 2 km s−1 than that of the former atom. Their orbits, and thus the directions of motion ahead of the Sun clearly differ. The observer location for DOY 37 is selected so that it corresponds to the viewing geometry of IBEX-Lo, with the atoms impacting the instrument at the directions perpendicular to the radius vector. The blue, orange, and brown lines mark detection geometry at an alternative location, when the instrument is at the upwind longitude (DOY 160); viewing of these atoms is impossible for IBEX. For these two locations, direct orbits are shown. For DOY 305, three indirect orbits are presented; these are also inaccessible for IBEX, but will be accessible for IMAP.
Paper: The Solar Probe ANalyzer—Ions on the Parker Solar Probe
Authors: Roberto Livi, Davin E. Larson, Justin C. Kasper, Robert Abiad, A. W. Case, Kristopher G. Klein, David W. Curtis, Gregory Dalton, Michael Stevens, Kelly E. Korreck, George Ho, Miles Robinson, Chris Tiu, Phyllis L. Whittlesey, Jaye L. Verniero, Jasper Halekas, James McFadden, Mario Marckwordt, Amanda Slagle, Mamuda Abatcha, Ali Rahmati, Michael D. McManus
Figure caption: VDFs from 2019-04-05/19:54:31 showing the core at 350 km s−1 and the beam 600 km s−1, without any interference from He++. Left: phase-space density of H+ for all look directions. Middle: contour elevations showing a 2D slice through the ϕ plane. Right: contour elevations showing a 2D slice through the θ plane. The black arrow represents the magnetic field direction in SPAN-I coordinates, where the head is at the solar-wind velocity (measured by SPC), and the length is the Alfvén speed.
Paper: Breaking Correlation in the Inflow Parameters of Interstellar Neutral Gas in Direct-sampling Observations
Authors: M. Bzowski, M. A. Kubiak, E. Möbius, N. A. Schwadron
Figure caption: Temperature–speed correlation lines obtained from IBEX-Lo observations (blue) and simulated using the speed values from the simulated longitude–speed correlation line for DOY 37 (see Figure 2) and the Mach number as obtained from IBEX-Lo observations using Equation (1) (gray). The observed Mach number is equal to 5.075. The thick black dots represent the temperature–speed pairs of the parameter sets correlated by the Mach number, listed in the last two rows in Table 1.
Paper: The Solar Probe ANalyzer—Ions on the Parker Solar Probe
Authors: Roberto Livi, Davin E. Larson, Justin C. Kasper, Robert Abiad, A. W. Case, Kristopher G. Klein, David W. Curtis, Gregory Dalton, Michael Stevens, Kelly E. Korreck, George Ho, Miles Robinson, Chris Tiu, Phyllis L. Whittlesey, Jaye L. Verniero, Jasper Halekas, James McFadden, Mario Marckwordt, Amanda Slagle, Mamuda Abatcha, Ali Rahmati, Michael D. McManus
Figure caption: Energy spectrogram of protons (top), alphas (middle), and alphas corrected for proton bleeding (bottom). Separation between protons and alphas allows for the first individual measurements of the 3D distribution functions of H+ and He++ in the inner heliosphere.
Paper: Light-curve Model for Luminous Red Novae and Inferences about the Ejecta of Stellar Mergers
Authors: Tatsuya Matsumoto, Brian D. Metzger
Figure caption: (Left) Progenitor star R ⋆ vs. progenitor star mass M ⋆ as inferred from pretransient observations for a sample of LRNe (Table 1). For comparison, we show the TAMS (black line) and contours of surface escape velocity ﹩{v}_{\mathrm{esc},\star }={(2{{GM}}_{\star }/{R}_{\star })}^{1/2}﹩ (gray lines). (Right) Ratio of the ejecta velocity v obs inferred from spectroscopy of the transient emission to progenitor donor surface escape speed v esc,⋆. As expected, v obs/v esc,⋆ is larger for more evolved progenitors (R ⋆ > R TAMS) with well-developed core–envelope structure, for which the ejecta launching radius R 0 can be ≪ R ⋆.