adsabs/AstroCLIMB huggingface dataset:
Paper: Pre-impact Thermophysical Properties and the Yarkovsky Effect of NASA DART Target (65803) Didymos
Authors: Benjamin Rozitis, Simon F. Green, Samuel L. Jackson, Colin Snodgrass, Cyrielle Opitom, Thomas G. Müller, Ulrich C. Kolb, Steven R. Chesley, R. Terik Daly, Cristina A. Thomas, Andrew S. Rivkin
Figure caption: Reduced-χ 2 contour plot showing the best-fit solutions when the thermal inertia of Dimorphos is also introduced as an additional free parameter to that of Didymos. Here, the diameters of Didymos and Dimorphos have been held constant at their central values. As demonstrated, the mid-infrared data do not provide any constraints on the thermal inertia of Dimorphos.
Paper: Pre-impact Thermophysical Properties and the Yarkovsky Effect of NASA DART Target (65803) Didymos
Authors: Benjamin Rozitis, Simon F. Green, Samuel L. Jackson, Colin Snodgrass, Cyrielle Opitom, Thomas G. Müller, Ulrich C. Kolb, Steven R. Chesley, R. Terik Daly, Cristina A. Thomas, Andrew S. Rivkin
Figure caption: Spectral emissivity of the Didymos system derived by the (a) ATPM and (b) NEATM. The emissivity spectra of the S-type asteroids (6) Hebe (Green et al. 1985) and (951) Gaspra (Vernazza et al. 2010) are shown for comparison, as they also exhibit a sharp drop-off in spectral emissivity at wavelengths <9 μm. The shaded gray area indicates a region of strong telluric absorption, which introduces additional noise into the derived spectra. The error bars give the standard errors for the mean spectral emissivity values derived from the infrared photometry.
Paper: Orbital and Physical Characterization of Asteroid Dimorphos Following the DART Impact
Authors: Shantanu P. Naidu, Steven R. Chesley, Nicholas Moskovitz, Cristina Thomas, Alex J. Meyer, Petr Pravec, Peter Scheirich, Davide Farnocchia, Daniel J. Scheeres, Marina Brozovic, Lance A. M. Benner, Andrew S. Rivkin, Nancy L. Chabot
Figure caption: The planar full two-body problem from Scheeres (2009).
Paper: Orbital and Physical Characterization of Asteroid Dimorphos Following the DART Impact
Authors: Shantanu P. Naidu, Steven R. Chesley, Nicholas Moskovitz, Cristina Thomas, Alex J. Meyer, Petr Pravec, Peter Scheirich, Davide Farnocchia, Daniel J. Scheeres, Marina Brozovic, Lance A. M. Benner, Andrew S. Rivkin, Nancy L. Chabot
Figure caption: Postimpact orbital period (top), geometric eccentricity (middle), and libration angle (bottom) derived from the best-fit orbit of Dimorphos as a function of time, beginning at the time of the DART impact. We measure orbital period as the time between consecutive crossings of an inertial reference direction in the orbit plane. Orange curves show the best-fit exponential curve to the orbital period and the mean geometric eccentricity.
Paper: Orbital and Physical Characterization of Asteroid Dimorphos Following the DART Impact
Authors: Shantanu P. Naidu, Steven R. Chesley, Nicholas Moskovitz, Cristina Thomas, Alex J. Meyer, Petr Pravec, Peter Scheirich, Davide Farnocchia, Daniel J. Scheeres, Marina Brozovic, Lance A. M. Benner, Andrew S. Rivkin, Nancy L. Chabot
Figure caption: Residuals of mutual event times using the best-fit model described in Section 2, neglecting an exponential decay term ﹩{\ddot{\theta }}_{\mathrm{drag}}﹩. The dotted line (not a fit) highlights the approximate trend in the residuals. The plot contains six groups of data points, each group taken within a single lunation. The lunations are labeled as L 0 to L 5.
Paper: Orbital and Physical Characterization of Asteroid Dimorphos Following the DART Impact
Authors: Shantanu P. Naidu, Steven R. Chesley, Nicholas Moskovitz, Cristina Thomas, Alex J. Meyer, Petr Pravec, Peter Scheirich, Davide Farnocchia, Daniel J. Scheeres, Marina Brozovic, Lance A. M. Benner, Andrew S. Rivkin, Nancy L. Chabot
Figure caption: Photometric measurements (dots) from Moskovitz et al. (2024) of a primary occultation (left minimum) and primary eclipse (right minimum) overlaid with our photometric model (black curve) described in Section 4. Red circles (squares) show the times when the COM of Dimorphos, or the COM shadow, entered (exited) the mutual event. Inset figures show the system configuration corresponding to these event start and stop times.
Paper: Orbital and Physical Characterization of Asteroid Dimorphos Following the DART Impact
Authors: Shantanu P. Naidu, Steven R. Chesley, Nicholas Moskovitz, Cristina Thomas, Alex J. Meyer, Petr Pravec, Peter Scheirich, Davide Farnocchia, Daniel J. Scheeres, Marina Brozovic, Lance A. M. Benner, Andrew S. Rivkin, Nancy L. Chabot
Figure caption: Postimpact libration angle vs. libration velocity of the best-fit orbit of Dimorphos. The star shows the state at impact, which corresponds to ϕ  B  = −1.2 × 10−5 rad s−1 listed in Table 1. The libration amplitude is about 30°.
Paper: Orbital and Physical Characterization of Asteroid Dimorphos Following the DART Impact
Authors: Shantanu P. Naidu, Steven R. Chesley, Nicholas Moskovitz, Cristina Thomas, Alex J. Meyer, Petr Pravec, Peter Scheirich, Davide Farnocchia, Daniel J. Scheeres, Marina Brozovic, Lance A. M. Benner, Andrew S. Rivkin, Nancy L. Chabot
Figure caption: Estimated ΔP as a function of mid-time of data arc. Uncertainties are 1σ. The corresponding data arc is noted next to each data point. The best-fit constant ΔP (orange), linearly changing ΔP (green), and exponentially decaying ΔP (red) are overlaid.
Paper: Orbital and Physical Characterization of Asteroid Dimorphos Following the DART Impact
Authors: Shantanu P. Naidu, Steven R. Chesley, Nicholas Moskovitz, Cristina Thomas, Alex J. Meyer, Petr Pravec, Peter Scheirich, Davide Farnocchia, Daniel J. Scheeres, Marina Brozovic, Lance A. M. Benner, Andrew S. Rivkin, Nancy L. Chabot
Figure caption: Residuals of mutual event times from the best-fit solution in Table 1. The notable trend in the residuals seen in Figure 3 has been removed by adopting the draglike dissipation ﹩{\ddot{\theta }}_{\mathrm{drag}}﹩.
Paper: Orbital and Physical Characterization of Asteroid Dimorphos Following the DART Impact
Authors: Shantanu P. Naidu, Steven R. Chesley, Nicholas Moskovitz, Cristina Thomas, Alex J. Meyer, Petr Pravec, Peter Scheirich, Davide Farnocchia, Daniel J. Scheeres, Marina Brozovic, Lance A. M. Benner, Andrew S. Rivkin, Nancy L. Chabot
Figure caption:  χ 2s as a function of the primary equatorial radius of Didymos. “All data” refers to all the data (lightcurve + radar + spacecraft/DRACO) used in the orbit fit.
Paper: Orbital and Physical Characterization of Asteroid Dimorphos Following the DART Impact
Authors: Shantanu P. Naidu, Steven R. Chesley, Nicholas Moskovitz, Cristina Thomas, Alex J. Meyer, Petr Pravec, Peter Scheirich, Davide Farnocchia, Daniel J. Scheeres, Marina Brozovic, Lance A. M. Benner, Andrew S. Rivkin, Nancy L. Chabot
Figure caption: Histogram of the residuals for each type of event time. PE and PO stand for primary eclipse and primary occultation. SE and SO stand for secondary eclipse and secondary occultation.
Paper: The Population of Young Craters on the Moon: New Catalog and Spatial and Temporal Analysis
Authors: Rebecca R. Ghent, Emily S. Costello, A. H. Parker
Figure caption: Byrgius A (24.°55 S, 296.°2 E, d = 18.2 km), showing prominent rays. (a) Albedo rays (LROC WAC Hapke-norm 689 nm mosaic; I/F 0.07 (black) to 0.21 (white)); (b) Maturity rays (Kaguya MI derived OMAT mosaic; high OMAT value denotes immature material; dimensionless values 0.11–0.38); (c) thermophysical rays (Diviner global regolith temperature anomaly map; −5 to +5 K); and (d) rocks (Diviner global slope-adjusted rock abundance; 0–0.03). All frames shown at the same scale.
Paper: The Population of Young Craters on the Moon: New Catalog and Spatial and Temporal Analysis
Authors: Rebecca R. Ghent, Emily S. Costello, A. H. Parker
Figure caption: Crater 03-1-070791 (24.06 S, 239.41 E, d = 7.3 km; OMAT and RA color scales as in Figure 1). (a) Kaguya OMAT, showing a diffuse halo of low-maturity material (arrows) but no clear ray morphology. (b) Diviner SAM rock abundance overlaid on the LROC WAC morphology mosaic. Slightly elevated RA values are associated with individual large rocks or clusters of rocks. (c) LROC NAC images of a portion of the northern crater rim and surrounding region. Rocks likely to have been ejected during the impact that formed the crater are clearly visible (arrows).
Paper: The Population of Young Craters on the Moon: New Catalog and Spatial and Temporal Analysis
Authors: Rebecca R. Ghent, Emily S. Costello, A. H. Parker
Figure caption: Venn diagrams depicting the fractional overlaps between rocky and rayed craters of all types (left) and between rocky and albedo-rayed craters (right). Circle areas are proportional to the number of craters in each category.
Paper: The Population of Young Craters on the Moon: New Catalog and Spatial and Temporal Analysis
Authors: Rebecca R. Ghent, Emily S. Costello, A. H. Parker
Figure caption: Small (300 m) crater near Ulugh Beigh B (32.67 N, 280.86 E) showing elevated RA values (overlaid on LROC NAC; color bar as in Figure 1) associated with a small superimposed crater that has likely excavated rocks from a subsurface layer such as a buried melt deposit.
Paper: The Population of Young Craters on the Moon: New Catalog and Spatial and Temporal Analysis
Authors: Rebecca R. Ghent, Emily S. Costello, A. H. Parker
Figure caption: Cumulative histograms by diameter for craters with both rocks and rays vs. rays or rocks only. All histograms normalized by total count and bin width (histogram areas integrate to unity).
Paper: The Population of Young Craters on the Moon: New Catalog and Spatial and Temporal Analysis
Authors: Rebecca R. Ghent, Emily S. Costello, A. H. Parker
Figure caption: Global LROC WAC morphology mosaic (Speyerer et al. 2011) in Robinson projection showing locations of rays and rocks. Top: rayed craters (green); bottom: rocky craters (yellow).
Paper: The Population of Young Craters on the Moon: New Catalog and Spatial and Temporal Analysis
Authors: Rebecca R. Ghent, Emily S. Costello, A. H. Parker
Figure caption: Cumulative (top) and differential (bottom) size–frequency plots of the 187 craters from Morota & Furumoto (2003b) that we positively identified (red), and the albedo-rayed craters from our database that reside in the MF2003 study region. D−1.8 curve plotted for comparison to Morota & Furumoto (2003a, 2003b).
Paper: Probing the Oxidation State of Ocean Worlds with SUDA: Fe (II) and Fe (III) in Ice Grains
Authors: Maryse Napoleoni, Lucía Hortal Sánchez, Nozair Khawaja, Bernd Abel, Christopher R. Glein, Jon K. Hillier, Frank Postberg
Figure caption: LILBID cation mass spectra of iron (III) sulfate (Fe3+ 2[SO4]3), recorded with a delay time of 5.0 μs.
Paper: Probing the Oxidation State of Ocean Worlds with SUDA: Fe (II) and Fe (III) in Ice Grains
Authors: Maryse Napoleoni, Lucía Hortal Sánchez, Nozair Khawaja, Bernd Abel, Christopher R. Glein, Jon K. Hillier, Frank Postberg
Figure caption: LILBID anion mass spectra of iron (II) chloride (FeCl2), recorded with a delay time of 5.3 μs.
Paper: Probing the Oxidation State of Ocean Worlds with SUDA: Fe (II) and Fe (III) in Ice Grains
Authors: Maryse Napoleoni, Lucía Hortal Sánchez, Nozair Khawaja, Bernd Abel, Christopher R. Glein, Jon K. Hillier, Frank Postberg
Figure caption: LILBID cation mass spectra of iron (II) sulfate (FeSO4), recorded with a delay time of 5.0 μs.
Paper: Three-dimensional Atmospheric Dynamics of Jupiter from Ground-based Doppler Imaging Spectroscopy in the Visible
Authors: Francois-Xavier Schmider, Patrick Gaulme, Raúl Morales-Juberías, Jason Jackiewicz, Ivan Gonçalves, Tristan Guillot, Amy A. Simon, Michael H. Wong, Thomas Underwood, David Voelz, Cristo Sanchez, Riley DeColibus, Sarah A. Kovac, Sean Sellers, Doug Gilliam, Patrick Boumier, Thierry Appourchaux, Julien Dejonghe, Jean Pierre Rivet, Steve Markham, Saburo Howard, Lyu Abe, Djamel Mekarnia, Masahiro Ikoma, Hidekazu Hanayama, Bun'ei Sato, Masanobu Kunitomo, Hideyuki Izumiura
Figure caption: Top panel: photometric map of Jupiter from the JIVE campaign. Middle panels: inferred vertical (top) and meridional (bottom) from deprojected dopplergrams (in m s−1) derived from the 2018 JIVE campaign at DST. Vertical (resp. meridional) velocities are obtained by assuming that meridional (resp. vertical) velocities are null. The deprojected meridional velocity field is discarded in the equatorial region to avoid the plot being dominated by noise. Bottom panel: meridional velocity field component (in m s−1) derived from HST observations. Positive meridional velocity is northward, and positive vertical velocity is upward.
Paper: Three-dimensional Atmospheric Dynamics of Jupiter from Ground-based Doppler Imaging Spectroscopy in the Visible
Authors: Francois-Xavier Schmider, Patrick Gaulme, Raúl Morales-Juberías, Jason Jackiewicz, Ivan Gonçalves, Tristan Guillot, Amy A. Simon, Michael H. Wong, Thomas Underwood, David Voelz, Cristo Sanchez, Riley DeColibus, Sarah A. Kovac, Sean Sellers, Doug Gilliam, Patrick Boumier, Thierry Appourchaux, Julien Dejonghe, Jean Pierre Rivet, Steve Markham, Saburo Howard, Lyu Abe, Djamel Mekarnia, Masahiro Ikoma, Hidekazu Hanayama, Bun'ei Sato, Masanobu Kunitomo, Hideyuki Izumiura
Figure caption: Left panel: mean zonal wind profile from Doppler measurements (in blue) compared to the simulated Doppler wind profile (in crimson). As in Gonçalves et al. (2019), the width of the dark blue line represents the theoretical noise level estimated from the known photon noise and the sensitivity, while the light blue bars represent the dispersion of all the measurements, which could include actual velocity variations, so it is an upper limit of the true noise level. Right panel: comparison between the wind profile obtained with the cloud-tracking technique on the 2018 HST OPAL data (black line) and the JIVE profile to which we added the difference between the HST profile and the simulated profile based on the HST profile (red line) The light gray area around the black line represents the error on the HST profile.
Paper: Three-dimensional Atmospheric Dynamics of Jupiter from Ground-based Doppler Imaging Spectroscopy in the Visible
Authors: Francois-Xavier Schmider, Patrick Gaulme, Raúl Morales-Juberías, Jason Jackiewicz, Ivan Gonçalves, Tristan Guillot, Amy A. Simon, Michael H. Wong, Thomas Underwood, David Voelz, Cristo Sanchez, Riley DeColibus, Sarah A. Kovac, Sean Sellers, Doug Gilliam, Patrick Boumier, Thierry Appourchaux, Julien Dejonghe, Jean Pierre Rivet, Steve Markham, Saburo Howard, Lyu Abe, Djamel Mekarnia, Masahiro Ikoma, Hidekazu Hanayama, Bun'ei Sato, Masanobu Kunitomo, Hideyuki Izumiura
Figure caption: Comparison between the photometric and inferred velocity profiles from the JIVE data. The flux F(λ) is the photometric map from Figure 6 (top panel) averaged over the longitudes. Its derivative ∂F/∂λ is displayed as the second line. The three bottom lines show the same for the projected zonal, vertical, and meridional maps displayed in Figure 6. The background gray and white areas indicate the location of the belts (gray) and zones (white). From left to right, the acronyms correspond to the usual nomenclature: SPR for South Polar Region, SSTe (Z or B) for South-South Temperate (Zone or Belt), STe (Z or B) for South Temperate (Zone or Belt), STr (Z or B) for South Tropical (Zone or Belt), SEB for South Equatorial Belt, and EZ for Equatorial Zone. The nomenclature is the same in the northern hemisphere, with N in place of S.
Paper: Three-dimensional Atmospheric Dynamics of Jupiter from Ground-based Doppler Imaging Spectroscopy in the Visible
Authors: Francois-Xavier Schmider, Patrick Gaulme, Raúl Morales-Juberías, Jason Jackiewicz, Ivan Gonçalves, Tristan Guillot, Amy A. Simon, Michael H. Wong, Thomas Underwood, David Voelz, Cristo Sanchez, Riley DeColibus, Sarah A. Kovac, Sean Sellers, Doug Gilliam, Patrick Boumier, Thierry Appourchaux, Julien Dejonghe, Jean Pierre Rivet, Steve Markham, Saburo Howard, Lyu Abe, Djamel Mekarnia, Masahiro Ikoma, Hidekazu Hanayama, Bun'ei Sato, Masanobu Kunitomo, Hideyuki Izumiura
Figure caption: Jupiter observed by JIVE on 2018 May 17 at the DST. Left panel: image of Jupiter that corresponds with an exposure time of 30 s, where the flux is expressed in photons pixel−1. Right panel: line-of-sight velocity map corresponding to the same acquisition, aka dopplergram, where the velocity is expressed in km s−1. The x- and y-axes are expressed in pixels, and the seeing was estimated to be about 1.″4.
Paper: Three-dimensional Atmospheric Dynamics of Jupiter from Ground-based Doppler Imaging Spectroscopy in the Visible
Authors: Francois-Xavier Schmider, Patrick Gaulme, Raúl Morales-Juberías, Jason Jackiewicz, Ivan Gonçalves, Tristan Guillot, Amy A. Simon, Michael H. Wong, Thomas Underwood, David Voelz, Cristo Sanchez, Riley DeColibus, Sarah A. Kovac, Sean Sellers, Doug Gilliam, Patrick Boumier, Thierry Appourchaux, Julien Dejonghe, Jean Pierre Rivet, Steve Markham, Saburo Howard, Lyu Abe, Djamel Mekarnia, Masahiro Ikoma, Hidekazu Hanayama, Bun'ei Sato, Masanobu Kunitomo, Hideyuki Izumiura
Figure caption: Simulation of the difference of velocity between a solid rotation model and its corresponding Doppler map that includes the degradation of the velocity signal by the PSF. The PSF is assumed to be Gaussian with an FWHM of 2″. The flux model employed to simulate the data is based on an actual high-resolution image of Jupiter. The color scale indicates the velocity in m s−1.
Paper: Three-dimensional Atmospheric Dynamics of Jupiter from Ground-based Doppler Imaging Spectroscopy in the Visible
Authors: Francois-Xavier Schmider, Patrick Gaulme, Raúl Morales-Juberías, Jason Jackiewicz, Ivan Gonçalves, Tristan Guillot, Amy A. Simon, Michael H. Wong, Thomas Underwood, David Voelz, Cristo Sanchez, Riley DeColibus, Sarah A. Kovac, Sean Sellers, Doug Gilliam, Patrick Boumier, Thierry Appourchaux, Julien Dejonghe, Jean Pierre Rivet, Steve Markham, Saburo Howard, Lyu Abe, Djamel Mekarnia, Masahiro Ikoma, Hidekazu Hanayama, Bun'ei Sato, Masanobu Kunitomo, Hideyuki Izumiura
Figure caption: (A) Legendre decomposition of the HST profile for n > 23 (orange line) and n < 23 (magenta line). (B) Comparison between the JIVE profile and the n < 23 Legendre decomposition. (C) Comparison of the HST profile and the sum of the JOVIAL profile and the n > 23 Legendre decomposition.
Paper: Three-dimensional Atmospheric Dynamics of Jupiter from Ground-based Doppler Imaging Spectroscopy in the Visible
Authors: Francois-Xavier Schmider, Patrick Gaulme, Raúl Morales-Juberías, Jason Jackiewicz, Ivan Gonçalves, Tristan Guillot, Amy A. Simon, Michael H. Wong, Thomas Underwood, David Voelz, Cristo Sanchez, Riley DeColibus, Sarah A. Kovac, Sean Sellers, Doug Gilliam, Patrick Boumier, Thierry Appourchaux, Julien Dejonghe, Jean Pierre Rivet, Steve Markham, Saburo Howard, Lyu Abe, Djamel Mekarnia, Masahiro Ikoma, Hidekazu Hanayama, Bun'ei Sato, Masanobu Kunitomo, Hideyuki Izumiura
Figure caption: Jupiter zonal circulation from Doppler spectroscopy and cloud tracking. Top panel: deprojected velocity maps of Jupiter based on the 2018 JIVE campaign at DST. Bottom: zonal velocity map retrieved from cloud tracking based on HST OPAL data. Color scales indicate the velocity expressed in m s−1. Longitudes and latitudes are planetocentric. Positive zonal velocity is prograde, that is, eastward.
Paper: Three-dimensional Atmospheric Dynamics of Jupiter from Ground-based Doppler Imaging Spectroscopy in the Visible
Authors: Francois-Xavier Schmider, Patrick Gaulme, Raúl Morales-Juberías, Jason Jackiewicz, Ivan Gonçalves, Tristan Guillot, Amy A. Simon, Michael H. Wong, Thomas Underwood, David Voelz, Cristo Sanchez, Riley DeColibus, Sarah A. Kovac, Sean Sellers, Doug Gilliam, Patrick Boumier, Thierry Appourchaux, Julien Dejonghe, Jean Pierre Rivet, Steve Markham, Saburo Howard, Lyu Abe, Djamel Mekarnia, Masahiro Ikoma, Hidekazu Hanayama, Bun'ei Sato, Masanobu Kunitomo, Hideyuki Izumiura
Figure caption: Comparison of the meridional circulation of the GRS from JIVE (left) and HST/OPAL (right). Velocities are expressed in m s−1.
Paper: Heat-flux-limited Cloud Activity and Vertical Mixing in Giant Planet Atmospheres with an Application to Uranus and Neptune
Authors: Huazhi Ge, 华志 葛, Cheng Li, Xi Zhang, Chris Moeckel
Figure caption: Horizontally averaged temperature profile (panel (a)), temperature difference to the initial chemical equilibrium moist adiabat (panel (b)), local atmospheric lapse rate (solid lines in panel (c)), and local adiabatic lapse rate (dashed lines in panel (c)) with different metallicity. We first collect the physical quantity (i.e., temperature, lapse rate) of every time step. The local adiabatic lapse rate is dry adiabatic if the relative humidity is smaller than 100% (i.e., subsaturated) or moist adiabatic if the relative humidity is 100% (i.e., saturated). Then, we compute the averaged value as a function of pressure or height. Pressure and altitude are interchangeable at the statistically steady state in local simulations since the spatial variation of pressure at a certain altitude is negligible.
Paper: Heat-flux-limited Cloud Activity and Vertical Mixing in Giant Planet Atmospheres with an Application to Uranus and Neptune
Authors: Huazhi Ge, 华志 葛, Cheng Li, Xi Zhang, Chris Moeckel
Figure caption: The averaged eddy diffusivity of CH4 (blue lines) and H2S (red lines) vapor from numerical solutions (solid lines) and analytical solutions (dashed lines). The analytical eddy diffusivity is calculated by the simulated concentration gradient using Equation (10). In most layers, the analytical eddy diffusivity (dashed lines) is larger than or very close to the numerical solutions of the same species (solid lines). Not the analytical K  zz  in this figure is smaller than the estimated numbers in Section 2.2 because of the superadiabatic and subsaturated weather layers (see Appendix C for the derivation).
Paper: Heat-flux-limited Cloud Activity and Vertical Mixing in Giant Planet Atmospheres with an Application to Uranus and Neptune
Authors: Huazhi Ge, 华志 葛, Cheng Li, Xi Zhang, Chris Moeckel
Figure caption: The cloud density of the averaged CH4 and H2S cloud content (thick lines) and intermittent localized storms (thin lines). Thinner lines denote localized and transient cloud content in each vertical column. The CH4 cloud density inside the storm could be more than 10−4 to 10−3 kg m−3 but these storms cannot last long and are eventually turned off by the exceedingly large latent heat flux compared with the averaged planetary heat flux. It is also noticeable that this data set does not capture the variation of storms at each time step.
Paper: Heat-flux-limited Cloud Activity and Vertical Mixing in Giant Planet Atmospheres with an Application to Uranus and Neptune
Authors: Huazhi Ge, 华志 葛, Cheng Li, Xi Zhang, Chris Moeckel
Figure caption: Same as Figure 3 but for relative humidity. Dashed lines denote the relative humidity at the initial chemical equilibrium state (Li et al. 2018a), and light lines show the temporal and spatial variation of relative humidity. Similar to the snapshots in Figure 3, the output does not capture every time step. Relative humidity of CH4 is slightly larger than the initial condition below the initial lifting condensation level because the superadiabat induced by the condensation of H2S reduces the temperature in that region. Condensation only occurs when the localized air parcel is saturated and the relative humidity is at least 100%. Snapshots of relative humidity show that H2S is rarely saturated below the 5 bar level for all cases.
Paper: Heat-flux-limited Cloud Activity and Vertical Mixing in Giant Planet Atmospheres with an Application to Uranus and Neptune
Authors: Huazhi Ge, 华志 葛, Cheng Li, Xi Zhang, Chris Moeckel
Figure caption: The square of the buoyancy frequency at H2S weather layer (a) from 20 to 2 bars and CH4 weather layer (b) from 2 to 0.2 bars. The atmospheric buoyancy frequency is about 10−3 s−1 at about 9 bars level and 10−2 s−1 near the 1 bar level for the case with 50 times solar of CH4 and H2S.