adsabs/AstroCLIMB huggingface dataset:
Paper: The Viability of Glycine Fermentation in Titan’s Subsurface Ocean
Authors: Antonin Affholder, Peter M. Higgins, Charles S. Cockell, Catherine Neish, Krista M. Soderlund, Michael J. Malaska, Kendra K. Farnsworth, Rosaly M. C. Lopes, Conor A. Nixon, Mohit Melwani Daswani, Kelly E. Miller, Christophe Sotin
Figure caption: The temperature and pressure dependence of the standard free energy of glycine fermentation (under thermodynamic standard conditions). Computed using SUPCRT and the slop07 database (J. W. Johnson et al. 1992).
Paper: 2020 BX12—The Last Binary Asteroid Discovered at Arecibo
Authors: Luisa Fernanda Zambrano-Marin, Sean E. Marshall, Ellen S. Howell, Julia de León, Noemi Pinilla-Alonso, Anne K. Virkki, Jon Giorgini, Flaviane C. F. Venditti
Figure caption: Objective function values (on vertical axis, increasing upwards) for various combinations of semimajor axis (horizontal axis, increasing to the right) and orbital period (colors). Any model with an objective function value of less than about 3.4 gives acceptable fits to the radar data, although some such models would have physically unlikely densities or orbital elements. Marker shapes indicate the system’s average density, with diamonds for preferred values 0.4–3.0 g cm−3, downward-pointing triangles for densities less than 0.4 g cm−3, upward-pointing triangles for densities greater than 3.0 g cm−3, crosses for models with a primary diameter greater than 270 m (for any density), and Xs for models above the objective function cutoff (regardless of diameter or density). The blue and red circles indicate the two models from Figures 5 and 6. The pole directions of the acceptable models cover most of the celestial sphere. The density of points in certain regions does not necessarily indicate preferred solutions, since we did not uniformly sample the entire parameter space. We ran over 6000 models for combinations of five orbital elements: pole longitude, pole latitude, orbital period, semimajor axis, and time of pericenter.
Paper: 2020 BX12—The Last Binary Asteroid Discovered at Arecibo
Authors: Luisa Fernanda Zambrano-Marin, Sean E. Marshall, Ellen S. Howell, Julia de León, Noemi Pinilla-Alonso, Anne K. Virkki, Jon Giorgini, Flaviane C. F. Venditti
Figure caption: The observed Doppler spectrum (2020 February 4, 20:17 UT, OC polarization) with the simulated CW spectra from two different shape models and the corresponding plane-of-sky views of the models at that time. The blue line (and top right plane-of-sky frame) shows the fit for a solution with pole orientation (0∘, +15∘) (ecliptic coordinates), an orbital period of 2.1 days, a semimajor axis of 890 m, and average diameters for the components of 230 and 50 m. The red line (and bottom right plane-of-sky frame) shows a model with pole (295∘, +30∘), an orbital period of 2.4 days, a semimajor axis of 400 m, and component diameters of 160 and 50 m. These two models are indicated with blue and red circles in Figures 7 and 8. The plane-of-sky images are oriented with celestial north toward the top and east toward the left. The colored rods mark the principal axes of inertia, where red represents the minimum inertia axis, and green represents the intermediate axis. The magenta arrow points to the rotation vector, which aligns with the axis of maximum inertia (shortest axis).
Paper: 2020 BX12—The Last Binary Asteroid Discovered at Arecibo
Authors: Luisa Fernanda Zambrano-Marin, Sean E. Marshall, Ellen S. Howell, Julia de León, Noemi Pinilla-Alonso, Anne K. Virkki, Jon Giorgini, Flaviane C. F. Venditti
Figure caption: Delay-Doppler images for two good orbit models at two different times. The first row shows 2020 BX12 on 2020 February 4 at 21:09 UT, and the second row is 2020 February 5 at 20:25 UT. Within each row, from left to right, the frames show the plane-of-sky view of the first model at the observation time, the simulated delay-Doppler image for the first model, the data, the simulated image for the second model, and the plane-of-sky view of the second model. The first model has a pole direction (0∘, +15∘), an orbital period of 2.1 days, a semimajor axis of 890 m, and average diameters for the components at 230 and 50 m. The second model has pole direction (295∘, +30∘), an orbital period of 2.4 days, a semimajor axis of 400 m, and component diameters of 160 and 50 m. Both data and model delay-Doppler images have Doppler frequency on the horizontal axis (increasing to the right) and delay on the vertical axis (increasing downward). The delay-Doppler frames have been stretched so that they have approximately the same scale as the plane-of-sky frames, so the original delay-Doppler pixels appear rectangular here. The plane-of-sky views are oriented as in Figure 5.
Paper: 2020 BX12—The Last Binary Asteroid Discovered at Arecibo
Authors: Luisa Fernanda Zambrano-Marin, Sean E. Marshall, Ellen S. Howell, Julia de León, Noemi Pinilla-Alonso, Anne K. Virkki, Jon Giorgini, Flaviane C. F. Venditti
Figure caption: Optical spectrum of 2020 BX12 obtained with the OSIRIS camera-spectrograph at the GTC. The spectrum is binned by 20 channels. Error bands are plotted with ±3σ within the bin. The blue dots (line and bars) denote 2020 BX12 data; purple squares (line and band) correspond to the Sq-type spectra, and the green diamonds (line and band) to the Q-type spectrum. The Sq- and Q-type spectral data are from the Bus–DeMeo taxonomy (F. E. DeMeo et al. 2009) range.
Paper: 2020 BX12—The Last Binary Asteroid Discovered at Arecibo
Authors: Luisa Fernanda Zambrano-Marin, Sean E. Marshall, Ellen S. Howell, Julia de León, Noemi Pinilla-Alonso, Anne K. Virkki, Jon Giorgini, Flaviane C. F. Venditti
Figure caption: Objective function values (on vertical axis, increasing upwards) for various combinations of mean diameter of the primary (on horizontal axis, increasing to the right) and average density (colors) increasing upward. The blue and red circles indicate the two models from Figures 5 and 6. This figure only shows models for which the average density has values between 0.4 and 3.0 g cm−3.
Paper: 2020 BX12—The Last Binary Asteroid Discovered at Arecibo
Authors: Luisa Fernanda Zambrano-Marin, Sean E. Marshall, Ellen S. Howell, Julia de León, Noemi Pinilla-Alonso, Anne K. Virkki, Jon Giorgini, Flaviane C. F. Venditti
Figure caption: Rotation period vs. absolute magnitude plot of NEAs (black circles) and binary asteroids (green squares) from the Light Curve Database (2023 October), with reasonably known period (<30% uncertainty). 2020 BX12 is marked with a purple star. Although not an outlier, we see it being quite close to the critical period line (dotted horizontal line at 2.2 hr).
Paper: 2020 BX12—The Last Binary Asteroid Discovered at Arecibo
Authors: Luisa Fernanda Zambrano-Marin, Sean E. Marshall, Ellen S. Howell, Julia de León, Noemi Pinilla-Alonso, Anne K. Virkki, Jon Giorgini, Flaviane C. F. Venditti
Figure caption: Continuous-wave echo power spectra of both days of observation. (a) Sum of all scans for February 4. The secondary is clearly visible with its signal superposed over the primary. Figure 10 shows an alternate version of this plot. (b) Sum of all scans for February 5 observations, where the data are noisier. There was no clear signal in the SC channel, so we discarded this day’s circular polarization ratio.
Paper: 2020 BX12—The Last Binary Asteroid Discovered at Arecibo
Authors: Luisa Fernanda Zambrano-Marin, Sean E. Marshall, Ellen S. Howell, Julia de León, Noemi Pinilla-Alonso, Anne K. Virkki, Jon Giorgini, Flaviane C. F. Venditti
Figure caption: Delay-Doppler images of PHA 2020 BX12, summed for both days of observation. The frame on the left displays the data acquired with a baud length of 0.05 μs, a range resolution of 7.5 m px−1 in range at 1 sample per baud. The image on the right was acquired with a baud length of 0.2 μs, with a sampling rate of four times per baud, plotted in range at 7.5 m px−1. In both frames, delay increases downward, and Doppler increases to the right.
Paper: 2020 BX12—The Last Binary Asteroid Discovered at Arecibo
Authors: Luisa Fernanda Zambrano-Marin, Sean E. Marshall, Ellen S. Howell, Julia de León, Noemi Pinilla-Alonso, Anne K. Virkki, Jon Giorgini, Flaviane C. F. Venditti
Figure caption: Objective function (vertical axis) values for a wide range of possible mass values (horizontal axis), and diameters (colored band); shape markers denote densities, with diamonds being between 0.4 and 3.0 g cm−1. The density of points in certain regions does not necessarily indicate preferred solutions, since we did not uniformly sample the entire parameter space.
Paper: 2020 BX12—The Last Binary Asteroid Discovered at Arecibo
Authors: Luisa Fernanda Zambrano-Marin, Sean E. Marshall, Ellen S. Howell, Julia de León, Noemi Pinilla-Alonso, Anne K. Virkki, Jon Giorgini, Flaviane C. F. Venditti
Figure caption: Replotting Figure 2(a), to better visualize the circular polarization, presenting the CW data in units of cross section per frequency bin, over the spectra. The 1σ uncertainties due to thermal noise are 106 m2 Hz−1 for OC and 277 m2 Hz−1 for SC (in each channel)—both too small to appear clearly on this plot, and smaller than the uncertainty from self-noise (F. T. Ulaby et al. 1982).
Paper: 2020 BX12—The Last Binary Asteroid Discovered at Arecibo
Authors: Luisa Fernanda Zambrano-Marin, Sean E. Marshall, Ellen S. Howell, Julia de León, Noemi Pinilla-Alonso, Anne K. Virkki, Jon Giorgini, Flaviane C. F. Venditti
Figure caption: Delay-Doppler montage of delay-Doppler images obtained on 2020 February 5. Each frame is a sum of two scans. Data were taken at 0.2 μs but sampled at four samples per baud, giving a delay resolution of 7.5 m px−1 (with neighboring delay rows having correlated noise). The Doppler resolution is 0.075 Hz. Delay increases downward, and Doppler increases to the right.
Paper: 2020 BX12—The Last Binary Asteroid Discovered at Arecibo
Authors: Luisa Fernanda Zambrano-Marin, Sean E. Marshall, Ellen S. Howell, Julia de León, Noemi Pinilla-Alonso, Anne K. Virkki, Jon Giorgini, Flaviane C. F. Venditti
Figure caption: Montage of delay-Doppler images taken on 2020 February 4 with a delay resolution of 7.5 m px−1 and Doppler resolution of 0.074 Hz. We present sums of six scans, with delay increasing downward and Doppler increasing to the right.
Paper: 2020 BX12—The Last Binary Asteroid Discovered at Arecibo
Authors: Luisa Fernanda Zambrano-Marin, Sean E. Marshall, Ellen S. Howell, Julia de León, Noemi Pinilla-Alonso, Anne K. Virkki, Jon Giorgini, Flaviane C. F. Venditti
Figure caption: Model for the data of day 1, with pole orientation at ecliptic (295∘, +30∘).
Paper: 2020 BX12—The Last Binary Asteroid Discovered at Arecibo
Authors: Luisa Fernanda Zambrano-Marin, Sean E. Marshall, Ellen S. Howell, Julia de León, Noemi Pinilla-Alonso, Anne K. Virkki, Jon Giorgini, Flaviane C. F. Venditti
Figure caption: Model for the data of day 2, with pole orientation at ecliptic (295, +30∘).
Paper: 2020 BX12—The Last Binary Asteroid Discovered at Arecibo
Authors: Luisa Fernanda Zambrano-Marin, Sean E. Marshall, Ellen S. Howell, Julia de León, Noemi Pinilla-Alonso, Anne K. Virkki, Jon Giorgini, Flaviane C. F. Venditti
Figure caption: Model for the data of day 1, with pole orientation at ecliptic (0, +15∘).
Paper: Wind Shear and the Role of Eddy Vapor Transport in Driving Water Convection on Jupiter
Authors: Ramanakumar Sankar, Michael H. Wong, Csaba Palotai, Shawn Brueshaber
Figure caption: (a) The average zonal wind profile at 4 bars. (b) The temporally and zonally averaged ratio of water vapor mass mixing ratio between 600 mbar and 4 bars, which denotes the convection due to water. (c) The eddy meridional water vapor mixing at 4 bars. (d) The critical N2 for instability formation based on the Eady model (solid) and the atmospheric N2 at 4 bars (dashed). The locations of strong convection require both a strong meridional gradient in water vapor and strong eddy formation, resulting in water vapor mixing at the cloud base, highlighting the idea that the vapor transport is a primary driver for convection. The locations of these eddies correspond to locations where the atmospheric N2 is smaller than the critical value required for instability formation in the Eady model. Note that the north/south boundaries of the model do not show strong convection even though the atmospheric N2 is smaller than ﹩{N}_{{\rm{crit}}}^{2}﹩ since the meridional vapor gradient is negligible, and thus even though there is eddy mixing, it does not lead to strong buildup of CAPE.
Paper: Wind Shear and the Role of Eddy Vapor Transport in Driving Water Convection on Jupiter
Authors: Ramanakumar Sankar, Michael H. Wong, Csaba Palotai, Shawn Brueshaber
Figure caption: (a) Integrated water cloud density (with the same color bar as in Figure 4), with the local 4-bar wind field in black and the location of water vapor convergence (i.e., local increase in water vapor) in red. (b) 4-bar water vapor mixing ratio, on a linear scale ranging from 5 × 10−4 kg m–3 (black) to 5 × 10−3 kg m−3 (white). (c, d) Cross-sectional view at 21° north and 16° north, respectively, showing the water cloud density as blue shaded regions (corresponding to water cloud density between 10−3 and 10−2 kg m−3). This corresponds to the m = 0.25 case at 110 days. The location of the water vapor convergence is shown in red, and the local water snow and rain are shown in blue and green, respectively. We see how the convective storms form upstream of the water vapor convergence, with precipitation happening behind the top of the tower (the bulges in the snow contours are to the left of the convergence at 21° north and to the right at 17° north). The eddy transport of water vapor is responsible for initiating and maintaining convection. The downdrafts from precipitation refuel the next eddy wave packet.
Paper: Wind Shear and the Role of Eddy Vapor Transport in Driving Water Convection on Jupiter
Authors: Ramanakumar Sankar, Michael H. Wong, Csaba Palotai, Shawn Brueshaber
Figure caption: Zonally and temporally averaged ammonia (left) and water (right) cloud density for each of the cases studied. The zonal wind profile is shown with the black lines, with each contour separated by 25 m s−1. We see that clouds are forming thicker higher in the atmosphere at specific locations, due to convection carrying volatile-rich air to the upper regions. These are prominently at high meridional shear or in the peaks of jet streams.
Paper: Wind Shear and the Role of Eddy Vapor Transport in Driving Water Convection on Jupiter
Authors: Ramanakumar Sankar, Michael H. Wong, Csaba Palotai, Shawn Brueshaber
Figure caption: Top: VMR of water (black) and ammonia (blue) vapor near the pressure levels of 4 bars and 700 mbar, respectively. Bottom: the integrated cloud density for water (black) and ammonia (blue). Both profiles are at 18° north latitude in our model for the m = 0.4 case. Note how the thicker clouds for both species are coupled, due to being induced by convection by the water, as observed by G. L. Bjoraker et al. (2022). However, both the ammonia clouds and peak in the ammonia vapor distribution are slightly downstream of the main convective tower for water owing to the vertical wind shear.
Paper: Wind Shear and the Role of Eddy Vapor Transport in Driving Water Convection on Jupiter
Authors: Ramanakumar Sankar, Michael H. Wong, Csaba Palotai, Shawn Brueshaber
Figure caption: Integrated ammonia cloud column density for the different cases studied in the model, along with a Hubble OPAL (A. A. Simon et al. 2015) image of the same region. Note that the arc shapes in the ammonia clouds increase with wind shear, which matches the bright cloud patterns in OPAL observation. These clouds are set up by convective water clouds in our model, and the undulations are characterized by the deep eddy circulation.
Paper: Wind Shear and the Role of Eddy Vapor Transport in Driving Water Convection on Jupiter
Authors: Ramanakumar Sankar, Michael H. Wong, Csaba Palotai, Shawn Brueshaber
Figure caption: Integrated water cloud density (left; same color bar as in Figure 4) and water vapor mixing ratio at 4 bars (right), with the same color scale as in Figure 9, along with the associated wind field at 4 bars and the water vapor convergence in red, at day 110 into the model. Note how both the turbulence and the meridional volatile gradient increase with m, increasing the strength of convection in the atmosphere.
Paper: Wind Shear and the Role of Eddy Vapor Transport in Driving Water Convection on Jupiter
Authors: Ramanakumar Sankar, Michael H. Wong, Csaba Palotai, Shawn Brueshaber
Figure caption: The ratio of water vapor mass mixing ratio between 1 bar and the cloud base at 4 bars (solid) and between 600 mbar and 4 bars (dashed), as a function of model time. The ratio is globally averaged for each time step. We see that convection carries water to the upper altitudes and is generally sustained throughout the duration of the model.
Paper: Wind Shear and the Role of Eddy Vapor Transport in Driving Water Convection on Jupiter
Authors: Ramanakumar Sankar, Michael H. Wong, Csaba Palotai, Shawn Brueshaber
Figure caption: The ratio of water vapor mass mixing ratio between 600 mbar and 4 bars (top) and between 1 and 4 bars (bottom), as a function of latitude. Here the ratios are zonally and temporally averaged for each simulation. We see that the ratio peaks at specific latitudes, which show dominant convective intensity.
Paper: Wind Shear and the Role of Eddy Vapor Transport in Driving Water Convection on Jupiter
Authors: Ramanakumar Sankar, Michael H. Wong, Csaba Palotai, Shawn Brueshaber
Figure caption: The contribution to the increase in CAPE from each of the processes described in Section 2. The total value is shown with the black line. We can see that across all the cases the “chemical” effect (i.e., advection of water vapor) is the most prominent driver of CAPE increase across all the processes. Boxes (a), (b), and (c) correspond to regions that show high convection across all cases, high convection in the high-shear case, and low convection, respectively.
Paper: A Catalytic Pathway for the Formation of Cyanobenzene in Nitrogen-rich Environments and the Spectroscopy of the Reactive Intermediates
Authors: Vincent J. Esposito, Silvia Alessandrini, David Dubois, Ryan C. Fortenberry
Figure caption: The fragments employed within the Lego-brick approach to obtain the “TM+LR” equilibrium structures and the corresponding rotational constants.
Paper: Origin of Phobos and Deimos: Orbital Evolution Shortly after Formation from a Potential Dislocation
Authors: Ryan Dahoumane, Kévin Baillié, Valéry Lainey
Figure caption: Cumulative fraction of collisions as a function of simulation time, with different values of tides. We compare the cumulative fraction of collisions in simulations where we included all the effects presented in this paper. To maximize the effect of the tidal forces, we have considered extreme values of k2/Q significantly above the current values. It appears that even under such extreme circumstances, the collision rate after 25,000 yr remains above 89% in every case.
Paper: Origin of Phobos and Deimos: Orbital Evolution Shortly after Formation from a Potential Dislocation
Authors: Ryan Dahoumane, Kévin Baillié, Valéry Lainey
Figure caption: Cumulative fraction of simulations in which all the bodies collided for different numbers of fragments. We made simulations considering all the physical effects presented in this paper, but we considered that the fragmentation led to more than two fragments. The orbital elements repartitions are given in Table 3, and we did 1000 simulations for each number of fragments. We consider that a simulation undergoes “full collision” when all the fragments of the simulation collide with each other.
Paper: Origin of Phobos and Deimos: Orbital Evolution Shortly after Formation from a Potential Dislocation
Authors: Ryan Dahoumane, Kévin Baillié, Valéry Lainey
Figure caption: Cumulative collision fraction as a function of time for different values of Mars' obliquity. We tried to change Mars' obliquity to see if this could affect the probability of collision of postfragmentation Phobos and Deimos. A total of 1000 simulations were made for each value of the obliquity, and all the physical effects described in this paper were considered. The Martian orbital elements for these simulations are given in Table 2.
Paper: Laser-induced Breakdown Spectroscopy of Ice-regolith Mixtures: Implications for Measurements on Planetary Surfaces
Authors: Frédéric Diotte, Myriam Lemelin, François R. Doucet, Lütfü Ç. Özcan
Figure caption: Single-wavelength and line ratio maps of “discrete” ice-regolith mixtures. Each column shows measurements acquired from lunar regolith simulants with different H2O contents (0, 10, and 32 wt%). Each row shows a different spectral line or line ratio at which emission was measured. Single line intensities are displayed in counts. The first ablation performed by the instrument corresponds to the upper left pixel of the elemental maps, with the scan proceeding horizontally in an S-shaped pattern, as shown in Figure 2.
Paper: Laser-induced Breakdown Spectroscopy of Ice-regolith Mixtures: Implications for Measurements on Planetary Surfaces
Authors: Frédéric Diotte, Myriam Lemelin, François R. Doucet, Lütfü Ç. Özcan
Figure caption: Comparison of LIBS scans with camera images of ice-regolith mixtures. The first row presents PC maps (red = PC1, green = PC2, blue = PC3), while the second row displays corresponding camera images captured immediately before the LIBS scan. The samples include a dry LHS sample compressed at 40 T using a pelletizer (panels (a) and (b)), a “cemented” LMS ice sample containing 24 wt% water ice (panels (c) and (d)), and a “cemented” LHS ice sample containing 0.5 wt% water ice (panels (e) and (f)). Red arrows point to spatially corresponding features identified in both data sets.
Paper: Laser-induced Breakdown Spectroscopy of Ice-regolith Mixtures: Implications for Measurements on Planetary Surfaces
Authors: Frédéric Diotte, Myriam Lemelin, François R. Doucet, Lütfü Ç. Özcan
Figure caption: PCA results for LIBS scans of LHS and LMS samples with 0, 10, and 32 wt% water ice. (a) RGB color-composite images (also referred to as PCA maps) of the first three PCs, with the following channel attribution: R = PC1, G = PC2, B = PC3. (b) Coefficients of the first three PCs for all samples analyzed. (c) Scatter plots of the values of the first three PCs for the scans shown in panel (a). Each point in the scatter plots corresponds to a pixel in the images in panel (a) and is color-coded accordingly, linking image features to their positions in the PC space.
Paper: Laser-induced Breakdown Spectroscopy of Ice-regolith Mixtures: Implications for Measurements on Planetary Surfaces
Authors: Frédéric Diotte, Myriam Lemelin, François R. Doucet, Lütfü Ç. Özcan
Figure caption: Camera photos of an LHS sample containing water ice taken during a scan performed with CORIOSITY. The images were converted to gray scale to enhance contrast discernment. Shown is the sample cup standing on top of the sample holder as seen through the laser safety window. A dark halo of increasing size can be observed around the ablation sites, corresponding to the progressive melting of ice during the scan (a) after 1 scan line, (b) after 25 scan lines, and (c) after 200 scan lines.
Paper: Laser-induced Breakdown Spectroscopy of Ice-regolith Mixtures: Implications for Measurements on Planetary Surfaces
Authors: Frédéric Diotte, Myriam Lemelin, François R. Doucet, Lütfü Ç. Özcan
Figure caption: CORIOSITY scanning scheme for a 4 × 4 grid. All data presented in this manuscript were acquired on 200 × 200 grids.