adsabs/AstroCLIMB huggingface dataset:
Paper: Detecting Lipids on Planetary Surfaces with Laser Desorption Ionization Mass Spectrometry
Authors: Nikita J. Boeren, Salome Gruchola, Coenraad P. de Koning, Peter Keresztes Schmidt, Kristina A. Kipfer, Niels F. W. Ligterink, Marek Tulej, Peter Wurz, Andreas Riedo
Figure caption: Comparison of mass spectra for a platinum-coated and a stainless steel sample substrate for α-tocopherol, 17α-ethynylestradiol, cholecalciferol, and phylloquinone. All measurements were performed with a 3 μJ laser pulse energy.
Paper: Detecting Lipids on Planetary Surfaces with Laser Desorption Ionization Mass Spectrometry
Authors: Nikita J. Boeren, Salome Gruchola, Coenraad P. de Koning, Peter Keresztes Schmidt, Kristina A. Kipfer, Niels F. W. Ligterink, Marek Tulej, Peter Wurz, Andreas Riedo
Figure caption: Mass spectra of cholecalciferol, α-tocopherol, retinol, phylloquinone, menadione, and 17α-ethynylestradiol standards. Identified lipid and fragment peaks are annotated with their mass-to-charge ratio [m/z] expressed as integers, and molecular structures of each lipid are given in the corresponding mass spectrum.
Paper: Detecting Lipids on Planetary Surfaces with Laser Desorption Ionization Mass Spectrometry
Authors: Nikita J. Boeren, Salome Gruchola, Coenraad P. de Koning, Peter Keresztes Schmidt, Kristina A. Kipfer, Niels F. W. Ligterink, Marek Tulej, Peter Wurz, Andreas Riedo
Figure caption: Scan of laser power for cholecalciferol (concentration 200 μM, on platinum-coated substrate) with applied laser pulse energies of 2, 3, 4, 5 μJ. Signal intensity is very low at low laser power, while high power introduces a lot of background peaks. Pulse energy of 3 μJ was selected for the other measurements to allow for direct comparison with previous measurements of different compounds and to also assess the applicability of the measurement protocol, while also being the trade-off between signal intensity and background noise.
Paper: Detecting Lipids on Planetary Surfaces with Laser Desorption Ionization Mass Spectrometry
Authors: Nikita J. Boeren, Salome Gruchola, Coenraad P. de Koning, Peter Keresztes Schmidt, Kristina A. Kipfer, Niels F. W. Ligterink, Marek Tulej, Peter Wurz, Andreas Riedo
Figure caption: Mass spectra of three different mixtures, namely, six lipids (top), four lipids and two amino acids (middle), and four lipids and two PAHs (bottom). Intensity was cut off at 5 × 1012 to also show lower-intensity peaks, and peaks corresponding to the different compounds are annotated by symbols.
Paper: AFM Force Measurements to Explore Grain Contacts with Relevance for Planetary Materials
Authors: Keanna Jardine, Adrienne Dove, Laurene Tetard
Figure caption: Adhesion forces measured between the 45 μm spherical glass cantilever tip and the different grain size of simulants at 15% RH (labeled (15)) and at ambient laboratory RH conditions (labeled (A)), both at room temperature.
Paper: AFM Force Measurements to Explore Grain Contacts with Relevance for Planetary Materials
Authors: Keanna Jardine, Adrienne Dove, Laurene Tetard
Figure caption: Topographic images of the spherical tips over an area considered to calculate the rms roughness. In each image, the orange box represents the mask of the measurement area. 1(a) 2 μm tip, with roughness estimated to be about 1.01 ± 0.11 nm. 1(b) 15 μm tip, with roughness estimated to be about 10.74 ± 2.18 nm. 1(c) 45 μm tip, with roughness estimated to be about 4.15 ± 1.22 nm.
Paper: AFM Force Measurements to Explore Grain Contacts with Relevance for Planetary Materials
Authors: Keanna Jardine, Adrienne Dove, Laurene Tetard
Figure caption: Adhesion forces measured between the 15 μm spherical SiO2 cantilever tip and the different grain size of simulants at 15% RH (labeled (15)) and at ambient laboratory RH conditions (labeled (A)), both at room temperature.
Paper: AFM Force Measurements to Explore Grain Contacts with Relevance for Planetary Materials
Authors: Keanna Jardine, Adrienne Dove, Laurene Tetard
Figure caption: Adhesion forces measured between the 2 μm spherical SiO2 cantilever tip and the different grain sizes of simulants at 15% RH (labeled (15)) and at ambient laboratory RH conditions (labeled (A)), both at room temperature.
Paper: The Horizontal Wavelength Spectrum of Gravity Wave Activity in Mars’s Lower Atmosphere: The Perspective from MGS–TES Nadir Observations
Authors: Nicholas G. Heavens, Alexey Pankine, J. Michael Battalio, Corwin Wright
Figure caption: Number of diagnoses in the A3 channel binned at 5°×5° resolution for L  s  = 120°–150° for the labeled Mars Year, baseline, and time of day.
Paper: 3 μm Spectroscopic Survey of Near-Earth Asteroids
Authors: L. E. McGraw, J. P. Emery, C. A. Thomas, A. R. Rivkin, N. R. Wigton, M. McAdam
Figure caption: Three NEAs with definite features. The blue points with error bars represent the thermally corrected reflectance spectrum, and the red dashed line represents the reflected continuum. (a) (433) Eros as observed on 2019 January 4. (b) (1036) Ganymed as observed on 2011 October 19. Data points shown for Eros and Ganymed from 1.7 to 2.55 μm are from prism due to noise in the LXD data. (c) 2014 JO25 as observed on 2017 April 22; spectrum longward of 2.85 μm binned by a factor of 2.
Paper: 3 μm Spectroscopic Survey of Near-Earth Asteroids
Authors: L. E. McGraw, J. P. Emery, C. A. Thomas, A. R. Rivkin, N. R. Wigton, M. McAdam
Figure caption: Five NEAs with potential features. (a) (214088) 2004 JN13 as observed on 2014 November 30; spectrum longward of 2.85 μm binned by a factor of 2. (b) (159402) 1999 AP10 as observed on 2020 October 8/9; spectrum longward of 2.85 μm binned by a factor of 2. (c) (3122) Florence as observed on 2017 September 4; spectrum longward of 2.85 μm binned by a factor of 3. (d) (96590) 1998 XB as observed on 2016 November 27; spectrum longward of 2.85 μm binned by a factor of 2. (e) (163373) 2002 PZ39 as observed on 2020 February 12; spectrum binned by a factor of 3.
Paper: 3 μm Spectroscopic Survey of Near-Earth Asteroids
Authors: L. E. McGraw, J. P. Emery, C. A. Thomas, A. R. Rivkin, N. R. Wigton, M. McAdam
Figure caption: Spectrum (normalized reflectance values vs. wavelength in μm) of (433) Eros as observed on 2019 January 4. Black data points represent the spectrum before thermal tail removal (i.e., reflected and thermal components), blue represents the spectrum after thermal tail removal (i.e., only reflected component), and the red dashed line represents reflected continuum. Data points from 1.7 to 2.55 μm are from prism due to noise in the LXD data.
Paper: 3 μm Spectroscopic Survey of Near-Earth Asteroids
Authors: L. E. McGraw, J. P. Emery, C. A. Thomas, A. R. Rivkin, N. R. Wigton, M. McAdam
Figure caption: Prism spectrum of (433) Eros observed on 2019 January 4 showing graphical results of BAR-Ast. The red and yellow shaded regions represent band area. The vertical red and yellow dashed lines mark the band centers, and the slanted red and yellow dashed lines mark the continuum and the FWHM of the bands (MacLennan 2019). The gray shaded bars illustrate spectral regions of telluric water vapor absorptions, which were corrected using ATRAN, as described in Section 3.2.
Paper: Spectroscopic Mapping of Io’s Surface with HST/STIS: SO2 Frost, Sulfur Allotropes, and Large-scale Compositional Patterns
Authors: Samantha K. Trumbo, M. Ryleigh Davis, Benjamin Cassese, Michael E. Brown
Figure caption: Example average HST spectra of Io compared to laboratory spectra of candidate materials. Several species exhibit similar features to Io’s 380–500 nm absorption edge, which has long been attributed to some form of sulfur. The inflection at the base of the band edge may be better matched by the presence of metastable polymeric sulfur (S μ  ; a significant component of the shown sulfur melt freeze) than by S8 alone. Though the 560 nm band is perhaps best matched by the spectrum of Na2S, considerations of Io’s plume chemistry and of the geography of the feature point to the spectral influence of metastable S4 (also seen in the spectrum of red sulfur glass and likely that of S2O) as a more likely cause. The S4 spectrum is from Carlson et al. (2009) after Meyer et al. (1972b) and is scaled for clarity. The red sulfur glass spectrum is from Meyer et al. (1972a). Both reflect samples at 77 K and are converted to approximate reflectance from absorption profiles. The α-S8 spectrum is from Carlson et al. (2009) after Gradie et al. (1980) and was measured at room temperature, the spectra of β-S8 and the sulfur melt freeze (from 453 K melt) are of room-temperature samples from Moses & Nash (1991), and the Na2S spectrum shows an irradiated sample at 170 K from Nash & Nelson (1979). The S2O and PSO spectra are from Hapke & Graham (1989) and were taken at 77 K and 195 K, respectively. The shown SO2 frost spectrum from Hapke et al. (1981) (at ∼77 K) lacks the above features. All spectra are normalized at their longest wavelengths and, with the exception of the Pele spectrum, are offset for clarity. The offsets used are 0.13, 0.4, 1.3, 1.4, 1.6, 2.3, 2.5, 3, 3.2, and 3.4 units, respectively, from bottom (yellow plains) to top (SO2). Dashed lines at 380 and 560 nm pass through Io’s primary visible absorptions.
Paper: Spectroscopic Mapping of Io’s Surface with HST/STIS: SO2 Frost, Sulfur Allotropes, and Large-scale Compositional Patterns
Authors: Samantha K. Trumbo, M. Ryleigh Davis, Benjamin Cassese, Michael E. Brown
Figure caption: Maps of Io’s 560 nm absorption, which we measure in two ways. We retrieve the top distribution by measuring the band area beneath a fitted polynomial continuum across the visible absorption, while we retrieve the bottom distribution by measuring the slope of the 585–665 nm band edge normalized at its long-wavelength end. Both maps agree extremely well and indicate that the absorption is primarily constrained to the high latitudes with the notable exception of a clear association with Pele’s ring of pyroclastic material, the approximate center of which is indicated by the black circle at 19°S and 255°W. This geography is potentially indicative of a thermodynamically unstable species that is continuously produced. In agreement with the interpretations of Spencer et al. (1997) and Carlson et al. (2007), we suggest that the metastable short-chain allotrope S4 may form directly from plume gases at Pele and possibly be independently produced by irradiation and/or preserved by low temperatures at the high latitudes (see Section 5).
Paper: Spectroscopic Mapping of Io’s Surface with HST/STIS: SO2 Frost, Sulfur Allotropes, and Large-scale Compositional Patterns
Authors: Samantha K. Trumbo, M. Ryleigh Davis, Benjamin Cassese, Michael E. Brown
Figure caption: Example HST spectra of the white, yellow, and red color units defined from Galileo imagery (Geissler et al. 1999). Colored dots on the background USGS mosaic of Io indicate the pixel locations for the example spectra. The white materials show generally shallower slopes than do the red and yellow materials, with the exception of a steep drop short of ∼320 nm that is indicative of SO2, as well as strong SO2 absorption (low relative reflectivity) near 280 nm in the UV. The yellow materials are primarily characterized by a steep positive slope from roughly 380 to 500 nm, while the red materials exhibit a similarly strong slope in addition to a strong absorption near 560 nm. We performed 7 pixel and 5 pixel moving average smoothing to the shown UV and visible spectra, respectively.
Paper: Spectroscopic Mapping of Io’s Surface with HST/STIS: SO2 Frost, Sulfur Allotropes, and Large-scale Compositional Patterns
Authors: Samantha K. Trumbo, M. Ryleigh Davis, Benjamin Cassese, Michael E. Brown
Figure caption: Map of Io’s 280 nm SO2 absorption maximum from the UV HST/STIS G230L spectra. This distribution corresponds extremely well to the Voyager SO2 frost map of McEwen et al. (1988) and to the visibly bright regions of the above USGS Galileo/Voyager mosaic. We observe strong SO2 bands within Colchis Regio and Bosphorus Regio at low latitudes between roughly 100° and 250°W, which is also in agreement with ground-based mapping of weak infrared SO2 bands (Laver & de Pater 2008, 2009; de Pater et al. 2020). Such agreement, in combination with the relative strengths of different SO2 bands observed by Galileo NIMS (Carlson et al. 1997; Douté et al. 2001), is consistent with these regions harboring the largest-grained, thickest, and/or purest SO2 deposits, which appear stable over multidecade timescales. For context, the location of Pele is indicated by a black circle.
Paper: Spectroscopic Mapping of Io’s Surface with HST/STIS: SO2 Frost, Sulfur Allotropes, and Large-scale Compositional Patterns
Authors: Samantha K. Trumbo, M. Ryleigh Davis, Benjamin Cassese, Michael E. Brown
Figure caption: Maps of Io’s 380–500 nm absorption edge, which we measure in two ways. We create the top map by measuring the band area beneath a fitted linear continuum across the inflection of the absorption, while we create the bottom map by measuring the slope of the band edge normalized at its long-wavelength end. The distributions of both proxies agree extremely well, demonstrating that the absorption is entirely anti-correlated with the SO2 signature mapped in Figure 5. Instead, it appears strong across much of the mid and high latitudes on Io and in some low-latitude locations not covered by SO2 deposits. This geography is consistent with a wide distribution of sulfurous material, potentially rich in S8 or Sμ. The location of Pele (19°S, 255°W) is indicated by the black circle.
Paper: Spectroscopic Mapping of Io’s Surface with HST/STIS: SO2 Frost, Sulfur Allotropes, and Large-scale Compositional Patterns
Authors: Samantha K. Trumbo, M. Ryleigh Davis, Benjamin Cassese, Michael E. Brown
Figure caption: Geographic distributions of our extracted spectral endmembers. The given fractional abundances are the coefficients of the best-fit linear combinations of the three components at each pixel. White stars indicate the location of the endmember pixels, and a black circle indicates the location of Pele (19°S, 255°W). Component 1 closely follows the Voyager SO2 unit identified by McEwen et al. (1988) and also matches our SO2 map in Figure 5 well. Component 2 correlates with the yellow, likely sulfur-rich plains immediately surrounding the SO2 deposits, while our map of component 3 highlights the upper latitudes and Pele’s pyroclastic ring (19°S, 255°W) in good correspondence to our map of Io’s 560 nm absorption in Figure 7.
Paper: Spectroscopic Mapping of Io’s Surface with HST/STIS: SO2 Frost, Sulfur Allotropes, and Large-scale Compositional Patterns
Authors: Samantha K. Trumbo, M. Ryleigh Davis, Benjamin Cassese, Michael E. Brown
Figure caption: Ternary diagram demonstrating the progression of our endmember extraction routine, in which the endmembers converge to the corners of the diagram. The initial set of spectral endmembers is indicated by the encircled stars, while colored dots show iteratively chosen subsequent endmembers that lowered the overall rms. Gray dots represent the remaining pixels as best-fit linear combinations of the final three components.
Paper: Spectroscopic Mapping of Io’s Surface with HST/STIS: SO2 Frost, Sulfur Allotropes, and Large-scale Compositional Patterns
Authors: Samantha K. Trumbo, M. Ryleigh Davis, Benjamin Cassese, Michael E. Brown
Figure caption: The final three endmembers extracted from the visible-wavelength HST data set. The spectra have been smoothed by a 5 pixel moving average filter. The first, second, and third components appear similar to spectra of the Galileo white, yellow, and red materials, respectively.
Paper: The Horizontal Wavelength Spectrum of Gravity Wave Activity in Mars’s Lower Atmosphere: The Perspective from MGS–TES Nadir Observations
Authors: Nicholas G. Heavens, Alexey Pankine, J. Michael Battalio, Corwin Wright
Figure caption: Horizontal wavelength spectrum of ﹩\hat{{{\rm{\Omega }}}_{\mathrm{GW}}}﹩ (K2 K−2) reconstructed from MGS–TES measurements: (a) Western Valles Marineris (averaging bin of 5°–10°S, 95°–100°W) for A1 dayside and nightside, MY 24, without detiding; eastern Valles Marineris (averaging bin of 10°–15°S, 60°–65°W) for A1 nightside and A3 nightside, MY 24, without detiding; (c) Argyre (averaging bin of 45°–50°S, 50°–55°W) for the labeled Mars Year, time of day, channel, and detiding algorithm. Reconstruction is based on baselines ≥84 km; (d) Near Hellas (averaging bin of 35°–40°S, 85°–90°E) for the labeled Mars Year, time of day, channel, and detiding algorithm. Reconstruction is based on baselines ≥84 km; (e) Near Hellas (averaging bin of 35°–40°S, 85°–90°E) for A3 dayside (no detiding) in MY 24 and MY 25. Reconstruction during MY 25 is based on baselines ≥84 km, while reconstruction during MY 24 uses baselines as low as 21 km.
Paper: The Horizontal Wavelength Spectrum of Gravity Wave Activity in Mars’s Lower Atmosphere: The Perspective from MGS–TES Nadir Observations
Authors: Nicholas G. Heavens, Alexey Pankine, J. Michael Battalio, Corwin Wright
Figure caption:                       ﹩\hat{{{\rm{\Omega }}}_{\mathrm{GW}}}﹩ (K2 K−2, log10 scale) vs. baseline in MGS–TES measurements of four key source areas in the labeled averaging bins and in the labeled channels, MY, time of day, and use of the detiding algorithm. Thick, dotted line indicates ﹩\hat{{{\rm{\Omega }}}_{\mathrm{GW}}}﹩ > ﹩2.5\hat{{\epsilon }_{\mathrm{GW}}};﹩ thin, solid line indicates ﹩\hat{{{\rm{\Omega }}}_{\mathrm{GW}}}﹩ below this detection limit. The black dashed line indicates the number of observations contributing to the average at each baseline.
Paper: The Horizontal Wavelength Spectrum of Gravity Wave Activity in Mars’s Lower Atmosphere: The Perspective from MGS–TES Nadir Observations
Authors: Nicholas G. Heavens, Alexey Pankine, J. Michael Battalio, Corwin Wright
Figure caption:                       ﹩\hat{{{\rm{\Omega }}}_{\mathrm{GW}}}﹩ (K2 K−2, log10 scale) versus baseline in zonal mean MGS–TES measurements at 1° latitude resolution, further averaged over the labeled 32° wide bands for the labeled channels, MY, time of day, and use of the detiding algorithm. The panels are arranged so the northernmost band is at the top and the southernmost band is at the bottom. Thick, dotted line indicates ﹩\hat{{{\rm{\Omega }}}_{\mathrm{GW}}}﹩ > ﹩2.5\hat{{\epsilon }_{\mathrm{GW}}};﹩ thin, solid line would indicate ﹩\hat{{{\rm{\Omega }}}_{\mathrm{GW}}}﹩ below this detection limit. The black dashed line indicates the number of observations contributing to the average at each baseline.
Paper: The Horizontal Wavelength Spectrum of Gravity Wave Activity in Mars’s Lower Atmosphere: The Perspective from MGS–TES Nadir Observations
Authors: Nicholas G. Heavens, Alexey Pankine, J. Michael Battalio, Corwin Wright
Figure caption: Horizontal wavelength spectrum of ﹩\hat{{{\rm{\Omega }}}_{\mathrm{GW}}}﹩ (K2 K−2) zonal mean MGS–TES measurements at 1° latitude resolution, further averaged over 64°S ± 16° and 32°N ± 16° for the labeled Mars Year, time of day, channel, and detiding algorithm. The 32°N centered spectrum has been scaled by a factor of 8.49 to ensure that the peak of the baseline variance spectrum is of the same magnitude as the peak of the 64°S centered spectrum. Reconstruction is based on baselines ≥42 km.
Paper: The Horizontal Wavelength Spectrum of Gravity Wave Activity in Mars’s Lower Atmosphere: The Perspective from MGS–TES Nadir Observations
Authors: Nicholas G. Heavens, Alexey Pankine, J. Michael Battalio, Corwin Wright
Figure caption: Comparison of ﹩\hat{{\epsilon }_{\mathrm{GW}}}﹩ (K2 K−2, log10 scale) at the 21 km baseline in MGS–TES measurements with ﹩\hat{{\epsilon }_{\mathrm{GW}}}﹩ in MRO–MCS equivalent baselines for the labeled channels and time of day. Averaging period is L  s  = 120°–150° in MY 24 for MGS–TES and the same period in MY 28 for MRO–MCS.
Paper: The Horizontal Wavelength Spectrum of Gravity Wave Activity in Mars’s Lower Atmosphere: The Perspective from MGS–TES Nadir Observations
Authors: Nicholas G. Heavens, Alexey Pankine, J. Michael Battalio, Corwin Wright
Figure caption: Comparison of the distributions of individual diagnoses of ΩGW and ϵ GW (K2) on the dayside in the A3 channel for a baseline of 105 km for the labeled areas.
Paper: The Horizontal Wavelength Spectrum of Gravity Wave Activity in Mars’s Lower Atmosphere: The Perspective from MGS–TES Nadir Observations
Authors: Nicholas G. Heavens, Alexey Pankine, J. Michael Battalio, Corwin Wright
Figure caption: Variability in the potential energy spectrum of Imamura et al. (2007) near the highest wavenumbers sampled for the latitudinal bin of 0°N ± 16° (red line with crosses) compared with the mean scan mode of observations in each MGS–TES data volume. Single scan = 1 and double scan = 2.
Paper: The Horizontal Wavelength Spectrum of Gravity Wave Activity in Mars’s Lower Atmosphere: The Perspective from MGS–TES Nadir Observations
Authors: Nicholas G. Heavens, Alexey Pankine, J. Michael Battalio, Corwin Wright
Figure caption:                          ﹩\hat{{{\rm{\Omega }}}_{\mathrm{GW}}}﹩ (K2 K−2, log10 scale) at the labeled baseline in MGS–TES measurements for the A2 and A3 channels, with the detiding filter applied, on the dayside, MY 24, L  s  = 120°–150°, as labeled.
Paper: The Horizontal Wavelength Spectrum of Gravity Wave Activity in Mars’s Lower Atmosphere: The Perspective from MGS–TES Nadir Observations
Authors: Nicholas G. Heavens, Alexey Pankine, J. Michael Battalio, Corwin Wright
Figure caption:                          ﹩\hat{{{\rm{\Omega }}}_{\mathrm{GW}}}﹩ (K2 K−2, log10 scale) at the labeled baseline in MGS–TES measurements for the A2 and A3 channels on the dayside, MY 24, L  s  = 120°–150°, as labeled.
Paper: Air–Sea Interactions on Titan: Effect of Radiative Transfer on the Lake Evaporation and Atmospheric Circulation
Authors: Audrey Chatain, Scot C. R. Rafkin, Alejandro Soto, Ricardo Hueso, Aymeric Spiga
Figure caption: Evolution with time of the energy fluxes (solar and IR radiative fluxes, sensible and latent heat fluxes) at the center and border of the lake, of the Bowen ratio, the surface temperature, the air temperature at 3 m, and the CH4 mixing ratio at different locations. Results shown are obtained in simulations S-C (0% relative humidity RH), S-E (20%), S-A (45%), and S-F (70%).
Paper: Air–Sea Interactions on Titan: Effect of Radiative Transfer on the Lake Evaporation and Atmospheric Circulation
Authors: Audrey Chatain, Scot C. R. Rafkin, Alejandro Soto, Ricardo Hueso, Aymeric Spiga
Figure caption: Evolution with time of the horizontal wind and the methane mixing ratio at 3 m altitude. Results shown are obtained with the simulations S-E (20% humidity) and S-F (70% humidity). The dark blue line indicates the lake position. Simulations are started at midnight.
Paper: Air–Sea Interactions on Titan: Effect of Radiative Transfer on the Lake Evaporation and Atmospheric Circulation
Authors: Audrey Chatain, Scot C. R. Rafkin, Alejandro Soto, Ricardo Hueso, Aymeric Spiga
Figure caption: Richardson number along the 2D simulation. Contours give the virtual potential temperature every 0.05 K. Average over 1–3 am (left column) and 1–3 pm (right column) on the third (panels (a) and (b)) and fourth (panels (c) and (d)) Titan days of simulation for S-B, and on the fourth tsol (which is very similar to the third tsol) for S-A (panels (e) and (f)). The dark blue line indicates the lake position.
Paper: Air–Sea Interactions on Titan: Effect of Radiative Transfer on the Lake Evaporation and Atmospheric Circulation
Authors: Audrey Chatain, Scot C. R. Rafkin, Alejandro Soto, Ricardo Hueso, Aymeric Spiga
Figure caption: Evolution with time of the energy fluxes (solar and IR radiative fluxes, sensible and latent heat fluxes) at the border of the lake and over the land, the surface temperature, the air temperature at 3 m and the CH4 mixing ratio at different locations. Results shown are obtained in simulations S-O (maximum insolation), S-A (reference, equinox at latitude 42°), S-U (equinox at 70°), S-V (equinox at 85°), S-N (polar night), and S-P (polar day).