adsabs/AstroCLIMB huggingface dataset:
Paper: Equatorial Waves and Superrotation in the Stratosphere of a Titan General Circulation Model
Authors: Neil T. Lewis, Nicholas A. Lombardo, Peter L. Read, Juan M. Lora
Figure caption: Spectra of eddy geopotential height and horizontal angular momentum flux convergence presented as a function of latitude and phase speed (panels (a) and (c)) and wavenumber and frequency (panels (b) and (d)), averaged between ±6° latitude. Analysis is shown for p = 1.5 hPa, L s = 226°–234°. The dashed cyan lines in panels (a) and (c) are curves of constant angular velocity (﹩{c}_{p}\times \cos \vartheta ﹩), and the solid blue lines show the zonal-mean zonal wind ﹩\overline{u}﹩. In panels (b) and (d), prograde modes are plotted with a positive wavenumber, and retrograde modes are plotted with a negative wavenumber. Blue in panel (b) indicates modes that are antisymmetric across the equator (only one is present, an MRG mode at ω + = 0.76 days and k  n  = 1; labeled in panel). The curves in panels (b) and (d) are dispersion curves for Kelvin waves (solid), MRG/n = 0 eastward inertio-gravity waves (dashed–dotted), n = 1 inertio-gravity waves (dotted), and n = 1 equatorial Rossby waves (dashed), where n is the meridional mode number. Curves are shown for vertical wavelengths λ v = 400 and 36 km for all waves, as well as λ v = 18 km for equatorial Rossby and Kelvin waves. These curves intersect with the c  p  = 170 m s−1 Kelvin wave, c  p  = 149 m s−1 Rossby–Kelvin wave, and c  p  = 73 m s−1 equatorial Rossby wave, shown in Figure 6, respectively (all k  n  = 1). The dispersion curves are calculated assuming a rotation rate ﹩{{\rm{\Omega }}}_{\mathrm{eff}}=\overline{u}/a﹩, which is the effective rotation rate moving with the superrotating jet. For details of the computation, see the Appendix.
Paper: Equatorial Waves and Superrotation in the Stratosphere of a Titan General Circulation Model
Authors: Neil T. Lewis, Nicholas A. Lombardo, Peter L. Read, Juan M. Lora
Figure caption: Composites of the horizontal structure for various waves identified at p = 1.5 hPa during the period L s = 226°–234°. Eddy velocity components (﹩u^{\prime} ﹩,﹩v^{\prime} ﹩) are shown as quivers, and eddy geopotential height is shown as colored contours. The quiver scale is constant between panels. Each panel shows fields filtered for k  n  = 1 and frequencies corresponding to c  p  = c  p,wave ± c  p,diff. The c  p,wave for each wave is indicated above each panel and corresponds to one of the cyan lines in Figures 5(a) and (c); c  p,diff = 5 m s−1. The red line in each panel shows the horizontal angular momentum flux convergence computed directly from each wave’s filtered eddy velocity field. It has units of ρ 0 × 10−3 m2 s−2. Blue lines show the zonal-mean zonal wind ﹩\overline{u}﹩, and dashed cyan lines show ﹩{c}_{p}\times \cos \vartheta ﹩ (both with units m s−1).
Paper: Equatorial Waves and Superrotation in the Stratosphere of a Titan General Circulation Model
Authors: Neil T. Lewis, Nicholas A. Lombardo, Peter L. Read, Juan M. Lora
Figure caption: Composites showing the filtered geopotential height anomaly averaged between ±20° latitude for selected waves. Red dashed lines in panels (b) and (c) indicate the pressure where ﹩{c}_{p}=\overline{u}﹩ for the selected phase speed. Above these lines, the waves are retrograde, and below them, they are prograde. As in Figures 6 and 8, the fields are filtered for frequencies corresponding to a range of phase speeds c  p  = c  p,wave ± c  p,diff, with c  p,diff = 5 m s−1.
Paper: Equatorial Waves and Superrotation in the Stratosphere of a Titan General Circulation Model
Authors: Neil T. Lewis, Nicholas A. Lombardo, Peter L. Read, Juan M. Lora
Figure caption: Eddy geopotential height spectrum presented as a function of pressure and phase speed, averaged within ±10° latitude for L s = 226°–234°. Vertical dashed lines correspond to c  p  associated with waves whose spatial structure in the λ–p plane is shown in Figures 10 or 11. Cyan, blue, and pink crosses correspond to the locations of waves whose horizontal structures are shown in Figures 6, 8, and 11, respectively. The solid blue curve shows the zonal-mean zonal wind ﹩\overline{u}﹩. The solid red curve indicates the pressure below which waves should be evanescent for a given phase speed (see text). The dotted purple lines indicate the pressure range spanned in Figures 3 and 4.
Paper: Equatorial Waves and Superrotation in the Stratosphere of a Titan General Circulation Model
Authors: Neil T. Lewis, Nicholas A. Lombardo, Peter L. Read, Juan M. Lora
Figure caption: Seasonal cycle of ﹩\overline{u}﹩, Ψ*,  F , and ∇ ·  F  across the pressure range p = 0.04–40 hPa. Left column: zonal-mean zonal wind ﹩\overline{u}﹩ and TEM stream function Ψ*, as in Figure 1. Right column: EP flux  F  (quivers) and its divergence ∇ ·  F  (colored contours). The horizontal and vertical components of  F  are rescaled as (π a)−1 F (ϑ) and ﹩{({\rm{\Delta }}{z}^{* })}^{-1}{F}^{({z}^{* })}﹩, respectively, where ﹩{\rm{\Delta }}{z}^{* }=-H\mathrm{log}({p}_{{\rm{t}}}/{p}_{{\rm{b}}})﹩ with p t = 2 × 10−2 and p b = 20 hPa. The EP flux divergence has units of density × specific angular momentum per unit time. Red contours indicate acceleration.
Paper: Equatorial Waves and Superrotation in the Stratosphere of a Titan General Circulation Model
Authors: Neil T. Lewis, Nicholas A. Lombardo, Peter L. Read, Juan M. Lora
Figure caption: Composites showing the horizontal structure for various waves as in Figure 6 but for p = 16.1 hPa. For panels (b) and (d), the quiver scale is constant and the same as in Figure 6. For panels (a) and (c), the quiver length has been multiplied by a factor of 5. As before, the filtered frequencies correspond to c  p  = c  p,wave ± c  p,diff. The c  p,wave is indicated above each panel, and c  p,diff = 5 m s−1.
Paper: Equatorial Waves and Superrotation in the Stratosphere of a Titan General Circulation Model
Authors: Neil T. Lewis, Nicholas A. Lombardo, Peter L. Read, Juan M. Lora
Figure caption: The EP flux  F  (quivers) and its divergence ∇ ·  F  (colored contours) for prograde (left) and retrograde (right) waves during the period L s = 226°–234°. Here  F  is scaled as in Figure 3. Gray contours show the zonal-mean zonal wind ﹩\overline{u}﹩ with the same contour levels as in Figures 1 and 3. Purple contours show the contribution to ∇ ·  F  from ﹩\partial {F}^{({z}^{* })}/\partial {z}^{* }﹩ (using the same contour levels).
Paper: Equatorial Waves and Superrotation in the Stratosphere of a Titan General Circulation Model
Authors: Neil T. Lewis, Nicholas A. Lombardo, Peter L. Read, Juan M. Lora
Figure caption: Spectra of eddy geopotential height and horizontal angular momentum flux convergence presented as a function of latitude and phase speed as in Figures 5(a) and (c) but for p = 16.1 hPa. The dashed cyan lines are curves of constant angular velocity (﹩{c}_{p}\times \cos \vartheta ﹩), and the solid blue lines show the zonal-mean zonal wind ﹩\overline{u}﹩.
Paper: Equatorial Waves and Superrotation in the Stratosphere of a Titan General Circulation Model
Authors: Neil T. Lewis, Nicholas A. Lombardo, Peter L. Read, Juan M. Lora
Figure caption: Composites showing the horizontal and vertical structure of the retrograde disturbance identified in Figure 9 at p = 0.1 hPa and c  p  = 125 m s−1. As with other composites, the frequencies were filtered using a window of width 5 m s−1 in phase speed space.
Paper: Evidence for Nitrogen-bearing Species on Umbriel: Sourced from a Subsurface Ocean, Undifferentiated Crust, or Impactors?
Authors: Richard J. Cartwright, Riley A. DeColibus, Julie C. Castillo-Rogez, Chloe B. Beddingfield, William M. Grundy, Tom A. Nordheim
Figure caption: Comparison between the four grand average Umbriel spectra shown in Figure 3 (black, A–D) compared to laboratory spectra (LS) and synthetic spectra (SS) (gray, numbered 1–20) of different candidate constituents. The candidate constituents shown here are summarized in Table 3 using the same numerical sequence (1–20): (1) LS of mixed NH3-hydrates, (2) LS of flash-frozen NH3–H2O solutions, (3) SS including amorphous NH3, (4, 5) SS including crystalline NH3 ice, (6-8) LS of NH4 carbonate, (9, 10) LS of NH4 bicarbonate, (11, 12) LS of NH4 chloride, (13) LS of thermonatrite, (14) SS including kaolinite, (15) SS including methylamine, (16) SS including ethylamine, (17) SS including propionitrile, (18) SS including ethylene, (19) SS including propyne, and (20) SS including methanol. The band centers of the 2.14 μm, 2.2 μm, 2.22 μm, and 2.24 μm bands (Tables A2–A5) are highlighted by the purple, blue, green, and red zones, respectively. All spectra were normalized to unity between 1.74 and 1.77 μm and offset vertically for clarity. Some of the laboratory spectra were vertically scaled for easier presentation in panels II and III. The synthetic spectra were generated with the previously described Hapke-Mie modeling program (model components, grain sizes, and mixing ratios are summarized in Table 4).
Paper: Evidence for Nitrogen-bearing Species on Umbriel: Sourced from a Subsurface Ocean, Undifferentiated Crust, or Impactors?
Authors: Richard J. Cartwright, Riley A. DeColibus, Julie C. Castillo-Rogez, Chloe B. Beddingfield, William M. Grundy, Tom A. Nordheim
Figure caption: Comparison between continuum-divided absorption features in the four grand average spectra (black, A–D) and representative laboratory and synthetic spectra (gray). The number to the right of each spectrum corresponds to the same number shown in Figure 4 and Tables 3 and 4. All continuum-divided bands are offset vertically for clarity. The wavelength range in band centers displayed by the 2.14 μm, 2.2 μm, 2.22 μm, and 2.24 μm bands (Tables A2–A5) are highlighted by the purple, blue, green, and red zones, respectively. The laboratory and synthetic spectra shown here represent the best matches to these four bands, based on comparison of their band centers: (A) 2.14 μm band compared to methylamine (15); (B) 2.2 μm band compared to NH4 chloride (11*), NH4 carbonate (7*), flash-frozen NH3–H2O solution (2), mixed NH3-hydrates (1), kaolinite (14), and thermonatrite (13); (C) 2.22 μm band compared to amorphous NH3 (3) and methylamine (15); and (D) 2.24 μm band compared to NH3 ice (4 and 5). Continuum-divided bands 7* and 11* only represent the central portion of the broad absorption features present in these spectra (Figure 4).
Paper: Evidence for Nitrogen-bearing Species on Umbriel: Sourced from a Subsurface Ocean, Undifferentiated Crust, or Impactors?
Authors: Richard J. Cartwright, Riley A. DeColibus, Julie C. Castillo-Rogez, Chloe B. Beddingfield, William M. Grundy, Tom A. Nordheim
Figure caption: Synthetic spectra for end-member species, offset vertically for clarity. The range in band centers for Umbriel’s 2.14 μm, 2.2 μm, 2.22 μm, and 2.24 μm bands (Tables A2–A5) are highlighted by the purple, blue, green, and red zones, respectively. Putative features at shorter wavelengths in the Umbriel spectra are highlighted by pairs of dotted lines spanning 1.583–1.597, 1.622–1.637, and 1.691–1.731 μm (close-up view shown in Figure 6). The gray-toned zones show the wavelength regions with prominent telluric features that contaminate the Umbriel data. The end-member species shown are amorphous C, 7 μm grain diameter (1; Rouleau & Martin 1991), CO2 ice (∼150 K), 10 μm grain diameter (2; Hansen 1997), H2O ice (80 K), 20 μm grain diameter (3; Mastrapa et al. 2008), H2O ice (80 K), 0.3 μm grain diameter (4; Mastrapa et al. 2008), kaolinite (room temperature), 7 μm grain diameter (5; Clark et al. 1990), amorphous NH3 (40 K), 10 μm grain diameter (6; Roser et al. 2021), NH3 ice (88 K), 10 μm grain diameter (7; Sill et al. 1980), NH3 ice (100 K), 10 μm grain diameter (8; Hudson et al. 2022a), methylamine (110 K), 10 μm grain diameter (9; Hudson et al. 2022b), ethylamine (100 K), 10 μm grain diameter (10; Hudson et al. 2022b), propionitrile (95 K), 10 μm grain diameter (11; Moore et al. 2010), ethylene (60 K), 10 μm grain diameter (12; Hudson et al. 2014), propyne (80 K), 10 μm grain diameter (13; Hudson et al. 2021), and methanol (120 K), 10 μm grain diameter (14; Gerakines & Hudson 2020). The grain sizes for each end-member constituent matches the grain sizes included in the particulate mixtures (Figure 4 and Table 4).
Paper: Evidence for Nitrogen-bearing Species on Umbriel: Sourced from a Subsurface Ocean, Undifferentiated Crust, or Impactors?
Authors: Richard J. Cartwright, Riley A. DeColibus, Julie C. Castillo-Rogez, Chloe B. Beddingfield, William M. Grundy, Tom A. Nordheim
Figure caption: Comparison between the four grand average spectra (black, A–D) and some representative laboratory and synthetic spectra shown in Figure 4 (gray). The number above each spectrum corresponds to the same spectrum number as shown in Figure 4 and Tables 5 and 6. All spectra were normalized to unity between 1.74 and 1.77 μm and offset vertically for clarity. Wavelength regions that show subtle features in the Umbriel spectra are highlighted by pairs of dotted lines spanning 1.583–1.597, 1.622–1.637, and 1.691–1.731 μm. The laboratory spectra shown in Panel I are NH4 chloride (11), NH4 bicarbonate (10), and thermonatrite (13). The synthetic spectra shown in Panel II include kaolinite (14), amorphous NH3 (3), NH3 ice (4), methylamine (15), and ethylamine (16).
Paper: Evidence for Nitrogen-bearing Species on Umbriel: Sourced from a Subsurface Ocean, Undifferentiated Crust, or Impactors?
Authors: Richard J. Cartwright, Riley A. DeColibus, Julie C. Castillo-Rogez, Chloe B. Beddingfield, William M. Grundy, Tom A. Nordheim
Figure caption: Grand average spectra (black) and 1σ uncertainties (light gray error bars) calculated using all individual spectra with band area and depth measurements >2σ for the 2.14 μm band (A, spectra b, c, f, g, i, l, m, and pin Figure 1), the 2.2 μm band (B, spectra b, c, e, f, h, i, j, l, and s in Figure 1), the 2.22 μm band (C, spectra a, d, g, i, j, m, n, and r in Figure 1), and the 2.24 μm band (D, spectra c, d, e, k, o, and q in Figure 1). All four grand average spectra are normalized to unity between 1.74 and 1.77 μm and offset vertically for clarity. The spectra have been smoothed using a 10–14 pixel wide boxcar function, whereas the 1σ uncertainties are shown at their native resolutions. The light purple zone highlights the wavelength range of the 2.14 μm band centers, the light blue zone shows the 2.2 μm band centers, the light green zone shows the 2.22 μm band centers, and the light red zone shows the range of 2.24 μm band centers (summarized in Figure 1 and the penultimate column of Tables A2, A3, A4, and A5, respectively). The dark gray line at the top of the plot is an atmospheric transmission model for Maunakea at zenith with 1.6 mm of precipitable water (50th percentile conditions), binned to simulate the spectral resolution of SpeX in SXD mode (R ∼ 750 at 2.2 μm, 0.″8 slit). This atmospheric spectrum demonstrates that Earth’s atmosphere is mostly transparent between 2.12 and 2.27 μm, with only a narrow CH4 gas feature overlapping the 2.2 μm band. Subpixel shifting routines used during data reduction help minimize residual telluric features. Thus, telluric contamination of the 2.2 μm band should be negligible.
Paper: Evidence for Nitrogen-bearing Species on Umbriel: Sourced from a Subsurface Ocean, Undifferentiated Crust, or Impactors?
Authors: Richard J. Cartwright, Riley A. DeColibus, Julie C. Castillo-Rogez, Chloe B. Beddingfield, William M. Grundy, Tom A. Nordheim
Figure caption: Scaled laboratory spectra for three different salts (gray) linearly combined with a synthetic spectrum (SS, black) that simulates the composition of Umbriel’s regolith, composed of a particulate mixture of crystalline H2O ice (0.3 and 20 μm grain sizes, 0.8 and 53.6%, respectively), amorphous C (8 μm grain size, 27.5%), and crystalline CO2 ice (10 μm grain size, 18.1%). Spectra have been offset vertically for clarity. The range in band centers for Umbriel’s 2.14 μm, 2.2 μm, 2.22 μm, and 2.24 μm bands (Tables A2–A5) is highlighted by the purple, blue, green, and red zones, respectively (shown in Figures 3 and 4). Additional putative features in the Umbriel spectra that may indicate the presence of NH3, salts, and organics are highlighted by pairs of dotted lines spanning 1.583–1.597, 1.622–1.637, and 1.691–1.731 μm (shown in Figure 6). The spectra shown in Panel I are NH4 carbonate (80 K) scaled by a factor of 0.012 (1a) and combined with spectrum SS (1b); NH4 carbonate (80 K) scaled by a factor of 0.007 (2a) and combined with spectrum SS (2b). The spectra shown in Panel II are NH4 chloride (90 K) scaled by a factor of 0.004 (3a) and combined with spectrum SS (3b); NH4 chloride (90 K) scaled by a factor of 0.002 (4a) and combined with spectrum SS (4b). The spectra shown in Panel III are thermonatrite (93 K) scaled by a factor of 0.016 (5a) and combined with spectrum SS (5b); thermonatrite (93 K) scaled by a factor of 0.008 (6a) and combined with spectrum SS (6b). Unscaled versions of these laboratory spectra are shown in Figures 4 and 6.
Paper: Evidence for Nitrogen-bearing Species on Umbriel: Sourced from a Subsurface Ocean, Undifferentiated Crust, or Impactors?
Authors: Richard J. Cartwright, Riley A. DeColibus, Julie C. Castillo-Rogez, Chloe B. Beddingfield, William M. Grundy, Tom A. Nordheim
Figure caption: Band area (left column) and band depth (right column) measurements and 1σ uncertainties for Umbriel’s 2.14 μm, 2.2 μm, 2.22 μm, and 2.24 μm bands, displayed as a function of subobserver longitude (measurements reported in Tables A2–A5). The solid blue lines show the mean area and depth measurements for each band, and the dashed orange lines show sinusoidal fits to the data. Gray-toned zones represent duplicated subobserver longitudes. We compared the fits provided by the mean and sinusoidal models using an F-test (results reported in Table 6). Several data points on the 2.22 μm and 2.24 μm band measurement plots are notably larger than the mean band area or depth values, suggesting that the constituents contributing to these bands might be concentrated in specific geologic features or regions on Umbriel’s surface. Spatially resolved spectra are required to further investigate this possibility.
Paper: Evidence for Nitrogen-bearing Species on Umbriel: Sourced from a Subsurface Ocean, Undifferentiated Crust, or Impactors?
Authors: Richard J. Cartwright, Riley A. DeColibus, Julie C. Castillo-Rogez, Chloe B. Beddingfield, William M. Grundy, Tom A. Nordheim
Figure caption: Umbriel grand average spectra (black, A–D) and 1σ uncertainties (light gray error bars) compared to a grand average spectrum and 1σ uncertainties (light gray error bars) of Ariel (black, E). The grand average Ariel spectrum was generate using the five IRTF/SpeX spectra that display >3σ band area and depth measurements for Ariel’s 2.2 μm band (reported in Cartwright et al. 2020c). All five spectra are normalized to unity between 1.74 and 1.77 μm and offset vertically for clarity. Each spectrum has been smoothed using a 10–14 pixel wide boxcar function, whereas the 1σ uncertainties are shown at their native resolutions. The range in band centers for Umbriel’s 2.14 μm, 2.2 μm, 2.22 μm, and 2.24 μm bands (Tables A2–A5) is highlighted by the purple, blue, green, and red zones, respectively.
Paper: Evidence for Nitrogen-bearing Species on Umbriel: Sourced from a Subsurface Ocean, Undifferentiated Crust, or Impactors?
Authors: Richard J. Cartwright, Riley A. DeColibus, Julie C. Castillo-Rogez, Chloe B. Beddingfield, William M. Grundy, Tom A. Nordheim
Figure caption: Eight reflectance spectra of Umbriel (continued below).
Paper: Origin-of-life Molecules in the Atmosphere after Big Impacts on the Early Earth
Authors: Nicholas F. Wogan, David C. Catling, Kevin J. Zahnle, Roxana Lupu
Figure caption: Outgoing longwave radiation of a 2 bar CO2 atmosphere on Mars with a 250 K surface temperature, computed with Clima (this work) and SMART (Meadows & Crisp 1996). The agreement between the two codes validates Clima.
Paper: Interstellar Comets from Post-main-sequence Systems as Tracers of Extrasolar Oort Clouds
Authors: W. Garrett Levine, Aster G. Taylor, Darryl Z. Seligman, Devin J. Hoover, Robert Jedicke, Jennifer B. Bergner, Gregory P. Laughlin
Figure caption: Maximum T eff during the AGB phase as a function of stellar mass and astrocentric distance. Contours at 6 K, 28 K, 86 K, and 144 K indicate representative values for which H2, CO, CO2, and H2O can be destroyed, respectively. All contour levels come from Gasc et al. (2017) except for H2, which comes from Seligman & Laughlin (2020).
Paper: Interstellar Comets from Post-main-sequence Systems as Tracers of Extrasolar Oort Clouds
Authors: W. Garrett Levine, Aster G. Taylor, Darryl Z. Seligman, Devin J. Hoover, Robert Jedicke, Jennifer B. Bergner, Gregory P. Laughlin
Figure caption: Fraction of test particles that became unbound during rebound simulations of a late-AGB thermal pulse, shown on a 25 × 25 grid in (e J,0, a J,0). Each cell represents approximately 6400 points. The dotted orange line shows the analytic prediction for the Ψ ≫ 1 regime from Equation (9): the maximum e J,0 value for which test particles are guaranteed to become unbound during post-main-sequence mass loss. The solid black line shows the contour where half of the test particles become unbound.
Paper: Interstellar Comets from Post-main-sequence Systems as Tracers of Extrasolar Oort Clouds
Authors: W. Garrett Levine, Aster G. Taylor, Darryl Z. Seligman, Devin J. Hoover, Robert Jedicke, Jennifer B. Bergner, Gregory P. Laughlin
Figure caption: Total number of Jurads ejected during post-main-sequence stellar evolution vs. the assumed power-law slope q in Equation (23). Our results are normalized to a 1  M ⊙ star, consistent with the scaling relation in Equation (22). These solutions were computed by summing over all size bins in each SFD. We display ejection numbers for different values of ﹩{r}_{\min }﹩, the smallest size included in the population, as curves of different colors.
Paper: Interstellar Comets from Post-main-sequence Systems as Tracers of Extrasolar Oort Clouds
Authors: W. Garrett Levine, Aster G. Taylor, Darryl Z. Seligman, Devin J. Hoover, Robert Jedicke, Jennifer B. Bergner, Gregory P. Laughlin
Figure caption: Comparison of our three methods of calculating the LSST’s search volume in which the Survey could detect Jurads. The upper panel shows values of instantaneous search volume V inst(H), while the lower panel shows the total volume V LSST over the 10 yr survey. “Model #1” corresponds to the representative quarter-sphere formulation, “Model #2” shows the result of numerically integrating the LSST search volume, and “Model #3” shows the application of simulations based on those by Hoover et al. (2022) to this situation. Only Model #1 and Model #2 return values for instantaneous volume. For reference, the size of ‘Oumuamua is marked by the vertical dotted line.
Paper: Interstellar Comets from Post-main-sequence Systems as Tracers of Extrasolar Oort Clouds
Authors: W. Garrett Levine, Aster G. Taylor, Darryl Z. Seligman, Devin J. Hoover, Robert Jedicke, Jennifer B. Bergner, Gregory P. Laughlin
Figure caption: Output of a numerical thermal penetration simulation for an object orbiting a 7.2 M ⊙-mass star at 1000 au. The temperature is initialized as T eff at the end of the RGB and is evolved through the early- and thermally pulsing–AGB. The temperature spike in the upper-right corner is the increase in stellar luminosity during the first thermal pulse. Of all stellar masses under consideration, this one precipitates the steepest temperature gradient across the minor planet. With only ΔT ∼ 10 K from the surface to the center, our use of effective temperature and isothermality for the exocomet’s temperature is justified.