adsabs/AstroCLIMB huggingface dataset:
Paper: Polyaromatic Units Set the Albedo of Dark Extraterrestrial Materials
Authors: Romain Maupin, Zahia Djouadi, Rosario Brunetto, Obadias Mivumbi, Christophe Sandt, and Ferenc Borondics
Figure caption: Panels (a) and (b) show the spectra of the silicon oil (black), the uncontaminated Tagish Lake grain (green) and the contaminated Tagish Lake (red) in the aliphatic and silicate regions, respectively. In panels (c) and (d) we compare the uncontaminated Tagish Lake spectrum (green) to the one obtained after a linear correction of the contaminated grain spectrum from the silicon oil contribution in the aliphatic and silicate bands, respectively.
Paper: Extreme-ultraviolet- and X-Ray-driven Photochemistry of Gaseous Exoplanets
Authors: Daniele Locci, Antonino Petralia, Giuseppina Micela, Antonio Maggio, Angela Ciaravella, and Cesare Cecchi-Pestellini
Figure caption: The geometry of the radiation transfer in our model, with the incoming radiation traveling horizontally. The zenith angle θ identifies the radial path along which the chemistry is computed. The vertical black arrows indicate the pressures sampled along the photon path.
Paper: Extreme-ultraviolet- and X-Ray-driven Photochemistry of Gaseous Exoplanets
Authors: Daniele Locci, Antonino Petralia, Giuseppina Micela, Antonio Maggio, Angela Ciaravella, and Cesare Cecchi-Pestellini
Figure caption: Stellar emission F in the energy range between 3 eV and 10 keV. Red line: LX = 1 × 1027 erg s−1, TX = 0.3 keV; green line: LX = 1 × 1028 erg s−1, TX = 0.5 keV; blue line: LX = 1 × 1030 erg s−1, TX = 1 keV. In the EUV band, we assume a flat spectral shape related to the X-ray luminosity by the Sanz-Forcada et al. (2011) relation. In the inset, we report the portion encompassing the Lyα line, which is also related to LX (Linsky et al. 2020); the asymmetry in the line profile stems out of the resolution with which we sample the spectrum.
Paper: Extreme-ultraviolet- and X-Ray-driven Photochemistry of Gaseous Exoplanets
Authors: Daniele Locci, Antonino Petralia, Giuseppina Micela, Antonio Maggio, Angela Ciaravella, and Cesare Cecchi-Pestellini
Figure caption: Total photoionization cross section (cm2) as a function of the energy (eV) of the incoming photon. Red solid line: neutrals; green solid line: cations; blue solid line: Compton ionization cross section (Locci et al. 2018); black dashed line: straight-line approximation, ∼ E−2.8.
Paper: Extreme-ultraviolet- and X-Ray-driven Photochemistry of Gaseous Exoplanets
Authors: Daniele Locci, Antonino Petralia, Giuseppina Micela, Antonio Maggio, Angela Ciaravella, and Cesare Cecchi-Pestellini
Figure caption: Photochemical rates, and ion and electron profiles in the RF model. Top panel: trends of different radiation-induced exit rates; bottom panel: vertical distribution of normalized volume mixing ratios of atomic ions and electrons.
Paper: Extreme-ultraviolet- and X-Ray-driven Photochemistry of Gaseous Exoplanets
Authors: Daniele Locci, Antonino Petralia, Giuseppina Micela, Antonio Maggio, Angela Ciaravella, and Cesare Cecchi-Pestellini
Figure caption: Optical depths of photons of different energies. Top panel: distribution along the vertical pressure profile; bottom panel: pressure level at which τ(E) = 1 (blue line), 10 (green line), and 100 (red line). Labels indicate the set of photon energies (eV) exploited in the top panel.
Paper: Extreme-ultraviolet- and X-Ray-driven Photochemistry of Gaseous Exoplanets
Authors: Daniele Locci, Antonino Petralia, Giuseppina Micela, Antonio Maggio, Angela Ciaravella, and Cesare Cecchi-Pestellini
Figure caption: Atomic (left panel) and molecular (right panel) vertical number density profiles for a selected set of species under the conditions of the RF model.
Paper: Extreme-ultraviolet- and X-Ray-driven Photochemistry of Gaseous Exoplanets
Authors: Daniele Locci, Antonino Petralia, Giuseppina Micela, Antonio Maggio, Angela Ciaravella, and Cesare Cecchi-Pestellini
Figure caption: The C+/C/CO transition.
Paper: Extreme-ultraviolet- and X-Ray-driven Photochemistry of Gaseous Exoplanets
Authors: Daniele Locci, Antonino Petralia, Giuseppina Micela, Antonio Maggio, Angela Ciaravella, and Cesare Cecchi-Pestellini
Figure caption: Vertical density profiles of electrons and their major contributors under the conditions of the RF model (solid lines). Black symbols indicate the distribution of the electron density suppressing X-rays (NX model).
Paper: Extreme-ultraviolet- and X-Ray-driven Photochemistry of Gaseous Exoplanets
Authors: Daniele Locci, Antonino Petralia, Giuseppina Micela, Antonio Maggio, Angela Ciaravella, and Cesare Cecchi-Pestellini
Figure caption: The vertical distribution of some C–H-bearing species including hydrogen cyanide (HCN) in the RF (solid line) and NX (dashed lines) models.
Paper: Extreme-ultraviolet- and X-Ray-driven Photochemistry of Gaseous Exoplanets
Authors: Daniele Locci, Antonino Petralia, Giuseppina Micela, Antonio Maggio, Angela Ciaravella, and Cesare Cecchi-Pestellini
Figure caption: Atmospheric concentrations arising from different assumptions on the illuminating stellar high-energy flux. RF model (LX = 1 × 1028 erg s−1, TX = 0.5 keV): red lines; LA model (LX = 1 × 1027 erg s−1, TX = 0.3 keV): purple lines; HA model (LX = 1 × 1030 erg s−1, TX = 1 keV): pale blue lines; NX model (no X-rays): blue lines; UV model (no radiation with energy higher than the Lyman continuum): green symbols; NE model (no EUV radiation): black symbols.
Paper: Extreme-ultraviolet- and X-Ray-driven Photochemistry of Gaseous Exoplanets
Authors: Daniele Locci, Antonino Petralia, Giuseppina Micela, Antonio Maggio, Angela Ciaravella, and Cesare Cecchi-Pestellini
Figure caption: Metallicity-dependent electron density profiles in the atmosphere. RF model: red line; LM model: green line; HM model: blue line.
Paper: Extreme-ultraviolet- and X-Ray-driven Photochemistry of Gaseous Exoplanets
Authors: Daniele Locci, Antonino Petralia, Giuseppina Micela, Antonio Maggio, Angela Ciaravella, and Cesare Cecchi-Pestellini
Figure caption: Water (left) and carbon monoxide (right) vertical profiles. LM model: green lines; RF model: red lines; HM model: blue lines. Dashed lines refer to the electron profiles; colors indicate the same models as in the case of molecular species.
Paper: Bistability of the Atmospheric Circulation on TRAPPIST-1e
Authors: Denis E. Sergeev, Neil T. Lewis, F. Hugo Lambert, Nathan J. Mayne, Ian A. Boutle, James Manners, Krisztian Kohary
Figure caption: Steady-state atmospheric circulation in the (left) Base (SJ regime) and (right) T0_280 (DJ regime) simulations. Panels (a) and (b) show 500 hPa temperature (shading, K) with 300 hPa wind vectors; panels (c) and (d) show 300 hPa eddy geopotential height (shading, m) and eddy wind vectors. The cyan lines in the bottom panels show the longitude of the planetary wave crest, defined as the maximum of the geopotential height anomaly. Thin cyan lines show the 50 day mean longitude for several time periods of the steady-state climate, while the thick cyan line shows the overall time mean longitude. The geopotential height anomaly is defined as the deviation from the zonal mean of the height of the 300 hPa isobaric surface.
Paper: Bistability of the Atmospheric Circulation on TRAPPIST-1e
Authors: Denis E. Sergeev, Neil T. Lewis, F. Hugo Lambert, Nathan J. Mayne, Ian A. Boutle, James Manners, Krisztian Kohary
Figure caption: Time series of diagnostics for the night-side cold traps, defined as the region bounded by 45° and 55° in the latitude and 160°–140°W in the longitude. The panels for the (left) SJ and (right) DJ regime show: (purple, solid) water vapor path in kilograms per meter squared, (purple, dashed) cloud water path in 10 kg m−2, (red, solid) water vapor radiative effect WVRELW sfc in watts per meter squared, (red, dashed) cloud radiative effect CRELW sfc in watts per meter squared, and (blue) surface temperature in kelvin. The WVRELW sfc is defined as the difference between the radiative fluxes at the surface calculated with and without the water vapor opacity. Likewise, the CRELW sfc is defined as the difference between the “clear-sky” and “cloudy” radiative fluxes at the surface.
Paper: Bistability of the Atmospheric Circulation on TRAPPIST-1e
Authors: Denis E. Sergeev, Neil T. Lewis, F. Hugo Lambert, Nathan J. Mayne, Ian A. Boutle, James Manners, Krisztian Kohary
Figure caption: Steady-state thermodynamic conditions in the (left) Base (SJ regime) and (right) T0_280 (DJ regime) simulations. Panels (a) and (b) show surface temperature (shading; kelvin) with 10 m wind vectors; panels (c) and (d) show water vapor path (shading; kilograms per meter squared); and panels (e) and (f) show cloud water path (shading; kilograms per meter squared).
Paper: Bistability of the Atmospheric Circulation on TRAPPIST-1e
Authors: Denis E. Sergeev, Neil T. Lewis, F. Hugo Lambert, Nathan J. Mayne, Ian A. Boutle, James Manners, Krisztian Kohary
Figure caption: Time-mean vertical profiles at the (solid lines) western and (dashed lines) eastern terminators in the (blue) SJ and (orange) DJ. The variables shown are (a) air temperature, (b) specific humidity, (c) cloud liquid water mixing ratio, and (d) cloud ice mixing ratio.
Paper: Bistability of the Atmospheric Circulation on TRAPPIST-1e
Authors: Denis E. Sergeev, Neil T. Lewis, F. Hugo Lambert, Nathan J. Mayne, Ian A. Boutle, James Manners, Krisztian Kohary
Figure caption: Helmholtz decomposition of the horizontal wind at 300 hPa in the (left) Base (SJ regime) and (right) T0_280 (DJ regime) simulations, corresponding to the wind field shown in Figures 7(a), (b). Panels (a) and (b) show the zonal mean rotational component; panels (c) and (d) show the eddy rotational component; panels (e) and (f) show the divergent component. Note the different scaling of the each of the components. Also shown is the upward wind velocity (shading; 10−2 meters per second).
Paper: Bistability of the Atmospheric Circulation on TRAPPIST-1e
Authors: Denis E. Sergeev, Neil T. Lewis, F. Hugo Lambert, Nathan J. Mayne, Ian A. Boutle, James Manners, Krisztian Kohary
Figure caption: Time series of diagnostics for the night-side cold traps, defined as the region bounded by 45° and 55° in the latitude and 160°–140°W in the longitude. The panels for the (left) SJ and (right) DJ regime show: (orange) downward longwave radiation flux, (green, solid) net longwave radiation flux, (green, dashed) sensible heat flux in watts per meter squared, (green, dotted) latent heat flux, and (blue) time derivative of the surface temperature in kelvin per day.
Paper: Bistability of the Atmospheric Circulation on TRAPPIST-1e
Authors: Denis E. Sergeev, Neil T. Lewis, F. Hugo Lambert, Nathan J. Mayne, Ian A. Boutle, James Manners, Krisztian Kohary
Figure caption: Differences in the transmission depth (ppm) between terminators (eastern minus western) in the (a) SJ and (b) DJ cases. Different lines show spectral differences assuming (pink) cloudy, (cyan) clear-sky, and (olive) dry atmosphere.
Paper: Bistability of the Atmospheric Circulation on TRAPPIST-1e
Authors: Denis E. Sergeev, Neil T. Lewis, F. Hugo Lambert, Nathan J. Mayne, Ian A. Boutle, James Manners, Krisztian Kohary
Figure caption: The steady-state moist static energy (MSE) budget for the (a) Base (SJ regime) and (b) T0_280 (DJ regime) simulations. See the text for details.
Paper: Bistability of the Atmospheric Circulation on TRAPPIST-1e
Authors: Denis E. Sergeev, Neil T. Lewis, F. Hugo Lambert, Nathan J. Mayne, Ian A. Boutle, James Manners, Krisztian Kohary
Figure caption: Simulated transmission spectra for the (blue) SJ and (orange) DJ cases. The transmission spectra are calculated using fluxes (a) with and (b) without the effect of clouds included. Panel (c) shows the difference, SJ minus DJ, for (solid lines) cloudy and (dashed lines) clear-sky calculations.
Paper: The TRAPPIST-1 Habitable Atmosphere Intercomparison (THAI). II. Moist Cases—The Two Waterworlds
Authors: Denis E. Sergeev, Thomas J. Fauchez, Martin Turbet, Ian A. Boutle, Kostas Tsigaridis, Michael J. Way, Eric T. Wolf, Shawn D. Domagal-Goldman, François Forget, Jacob Haqq-Misra, Ravi K. Kopparapu, F. Hugo Lambert, James Manners, Nathan J. Mayne
Figure caption: Hab 2 results: time variability of (a)–(c) surface temperature (K), (d) ice-free ocean area fraction, (e)–(h) cloud water path (kg m−2), and (i)–(l) the altitude of the cloud content maximum (km). Each column shows ((a), (d), (e), (i)) global mean, ((b), (f), (j)) day-side mean, ((c), (g), (k)) night-side mean, and ((h), (l)) terminator mean. Thin lines show the raw data, and thick lines show a five-orbit rolling mean.
Paper: The TRAPPIST-1 Habitable Atmosphere Intercomparison (THAI). II. Moist Cases—The Two Waterworlds
Authors: Denis E. Sergeev, Thomas J. Fauchez, Martin Turbet, Ian A. Boutle, Kostas Tsigaridis, Michael J. Way, Eric T. Wolf, Shawn D. Domagal-Goldman, François Forget, Jacob Haqq-Misra, Ravi K. Kopparapu, F. Hugo Lambert, James Manners, Nathan J. Mayne
Figure caption: Hab 2 results: (a)–(d) cloud water path (vertically integrated cloud condensate content, kg m−2), and (e)–(h) cloud fraction (%).
Paper: The TRAPPIST-1 Habitable Atmosphere Intercomparison (THAI). II. Moist Cases—The Two Waterworlds
Authors: Denis E. Sergeev, Thomas J. Fauchez, Martin Turbet, Ian A. Boutle, Kostas Tsigaridis, Michael J. Way, Eric T. Wolf, Shawn D. Domagal-Goldman, François Forget, Jacob Haqq-Misra, Ravi K. Kopparapu, F. Hugo Lambert, James Manners, Nathan J. Mayne
Figure caption: Hab 2 results: substellar vertical profiles of (a) air temperature (K), (b) lapse rate (K km−1), (c) SW heating rate (K d−1), and (d) LW heating rate (K d−1). Time-mean values are shown by solid lines, the 1σ deviation is shown by shading.
Paper: The TRAPPIST-1 Habitable Atmosphere Intercomparison (THAI). II. Moist Cases—The Two Waterworlds
Authors: Denis E. Sergeev, Thomas J. Fauchez, Martin Turbet, Ian A. Boutle, Kostas Tsigaridis, Michael J. Way, Eric T. Wolf, Shawn D. Domagal-Goldman, François Forget, Jacob Haqq-Misra, Ravi K. Kopparapu, F. Hugo Lambert, James Manners, Nathan J. Mayne
Figure caption: Hab 2 results: meridional-mean profiles of (a) the mass-weighted tropospheric mean of air temperature (K), (b) water vapor path (kg m−2), (c) cloud water path (kg m−2): total (solid lines), liquid (dashed lines), and ice (dotted lines), and (d) cloud area fraction (%). Here, the troposphere’s boundary is defined by the lapse rate decreasing below 2 K km−1 in the upper atmosphere. Note the different y-axis limits compared to Figure 6.