adsabs/AstroCLIMB huggingface dataset:
Paper: Tethys’s Heat Fluxes Varied with Time in the Ithaca Chasma and Telemus Basin Region
Authors: Chloe B. Beddingfield, Richard J. Cartwright, Sierra N. Ferguson, Erin J. Leonard
Figure caption: Profile data (black) with superimposed model flexural profiles (cyan) for all study locations (a–f) within our study area. Gray arrows point to the raised rims bounding Ithaca. See Figure 4(a) for locations of profile lines. See Table 2 for a summary of estimated values for T  e  and F. See Tables A2–A5 for a full list of estimated values of T  e  and F for porosities of 0%, 5%, 15%, and 25%, respectively. In addition to topography associated with flexure, topography associated with impact craters and faults is present, which was excluded from our flexural models. The profiles (distance and elevation) for locations a–f are available as data behind the figure. (The data used to create this figure are available.)
Paper: Tethys’s Heat Fluxes Varied with Time in the Ithaca Chasma and Telemus Basin Region
Authors: Chloe B. Beddingfield, Richard J. Cartwright, Sierra N. Ferguson, Erin J. Leonard
Figure caption: Estimated heat fluxes assuming a pure H2O ice lithosphere with porosities of (a) 0%, (b) 5%, (c) 15%, and (d) 25%. These estimates assume a grain size of d: 1 mm. See Tables A2–A5 for values assuming d: 0.1 mm.
Paper: Influences on Infrared Spectra of Benzene Ices for Titan, Comets, and Beyond: Annealings, Artifacts, and Isosbestic Points
Authors: Reggie L. Hudson, Perry A. Gerakines
Figure caption: (a) Benzene deposited at 10 K and warmed to 45 K. (b) Benzene deposited at 45 K at ∼2 μm hr−1. (c) Benzene deposited at 40 K at ∼2 μm hr−1. (d) Benzene deposited at 40 K at ∼0.4 μm hr−1. Each ice had a thickness of ∼0.5 μm and each spectrum had a resolution of 1 cm−1. Spectra are offset vertically for clarity.
Paper: Influences on Infrared Spectra of Benzene Ices for Titan, Comets, and Beyond: Annealings, Artifacts, and Isosbestic Points
Authors: Reggie L. Hudson, Perry A. Gerakines
Figure caption: Two regions of the IR spectrum of crystalline benzene. Ice #1 (left) was grown at 100 K and warmed to 130 K. Ice #2 (right) was grown at 130 K and cooled to 100 K. Each ice had a thickness of ∼0.83 μm and was grown at ∼1.3 μm hr−1. The spectral resolution was 4 cm−1. Spectra are offset vertically for clarity.
Paper: Influences on Infrared Spectra of Benzene Ices for Titan, Comets, and Beyond: Annealings, Artifacts, and Isosbestic Points
Authors: Reggie L. Hudson, Perry A. Gerakines
Figure caption: The IR spectrum (resolution = 1 cm−1) of amorphous benzene (a) made by vapor-phase condensation at 10 K and warmed to (b) 20, (c) 30, (d) 40, and (e) 50 K. Spectra are offset vertically for clarity. The 10 K ice’s thickness was about 1.9 μm, grown at ∼3 μm hr−1.
Paper: Influences on Infrared Spectra of Benzene Ices for Titan, Comets, and Beyond: Annealings, Artifacts, and Isosbestic Points
Authors: Reggie L. Hudson, Perry A. Gerakines
Figure caption: Survey spectra of amorphous and crystalline benzene (C6H6). Ices were grown and their spectra recorded with a resolution of 0.5 cm−1 at the temperatures indicated. The thicknesses of the amorphous and crystalline ices were about 0.96 and 0.83 μm, respectively, each ice being grown at about 1 μm hr−1. Spectra are offset for clarity. See the text and Hudson & Yarnall (2022) for details.
Paper: Tethys’s Heat Fluxes Varied with Time in the Ithaca Chasma and Telemus Basin Region
Authors: Chloe B. Beddingfield, Richard J. Cartwright, Sierra N. Ferguson, Erin J. Leonard
Figure caption: Estimated heat fluxes assuming a lithosphere with H2O ice and 10% NH3–H2O with porosities of (a) 0%, (b) 5%, (c) 15%, and (d) 25%. These estimates assume a grain size of d: 1 mm. See Tables A2–A5 for values assuming d: 0.1 mm.
Paper: Influences on Infrared Spectra of Benzene Ices for Titan, Comets, and Beyond: Annealings, Artifacts, and Isosbestic Points
Authors: Reggie L. Hudson, Perry A. Gerakines
Figure caption: Spectra of amorphous and crystalline benzene at 1 cm−1 resolution showing the loss of three forbidden transitions as the ice crystallized on warming from 10 to 130 K. The amorphous ice had a thickness of ∼4.8 μm, was grown at ∼3 μm hr−1, and was made and its spectrum recorded at 10 K before warming to 130 K. Spectra are offset vertically for clarity.
Paper: Influences on Infrared Spectra of Benzene Ices for Titan, Comets, and Beyond: Annealings, Artifacts, and Isosbestic Points
Authors: Reggie L. Hudson, Perry A. Gerakines
Figure caption: The IR spectrum (resolution = 1 cm−1) of amorphous benzene (a) made by vapor-phase condensation at 10 K and after annealing at (b) 20, (c) 30, (d) 40, and (e) 50 K. Spectra are offset vertically for clarity, and each was recorded at 10 K. The 10 K ice’s thickness was about 1.9 μm, grown at ∼3 μm hr−1.
Paper: Influences on Infrared Spectra of Benzene Ices for Titan, Comets, and Beyond: Annealings, Artifacts, and Isosbestic Points
Authors: Reggie L. Hudson, Perry A. Gerakines
Figure caption: Spectra of crystalline benzene made at 100 K by vapor-phase deposition at four different deposition rates. The thickness of each ice was about 0.83 μm and the spectral resolution was 0.5 cm−1. Spectra were recorded at 100 K and are offset vertically for clarity.
Paper: Influences on Infrared Spectra of Benzene Ices for Titan, Comets, and Beyond: Annealings, Artifacts, and Isosbestic Points
Authors: Reggie L. Hudson, Perry A. Gerakines
Figure caption: Four IR spectra of crystalline benzene at 130 K. (a) This work, ice made at 130 K. (b) This work, ice grown at 10 K and warmed to 130 K. (c) Ice of Mouzay et al. (2021), grown at 16 K and warmed to 130 K. (d) Ice of Nna-Mvondo & Anderson (2022), grown at 130 K. Resolutions are 0.5 cm−1 for (a) and (b), 1 cm−1 for (c), and 4 cm−1 for (d). Spectra are offset vertically for clarity. Spectrum (c) was recorded in a reflection mode, but the others are conventional transmission spectra.
Paper: Influences on Infrared Spectra of Benzene Ices for Titan, Comets, and Beyond: Annealings, Artifacts, and Isosbestic Points
Authors: Reggie L. Hudson, Perry A. Gerakines
Figure caption: Two regions of the IR spectrum of crystalline benzene. Ice #1 (left) was grown at 100 K and warmed to 130 K. Ice #2 (right) was grown at 130 K and cooled to 100 K. Each ice had a thickness of ∼0.83 μm and was grown at ∼1.3 μm hr−1. The spectral resolution was 0.5 cm−1. Spectra are offset vertically for clarity.
Paper: Influences on Infrared Spectra of Benzene Ices for Titan, Comets, and Beyond: Annealings, Artifacts, and Isosbestic Points
Authors: Reggie L. Hudson, Perry A. Gerakines
Figure caption: Positions of three IR peaks of crystalline benzene as a function of temperature. Changes in position were reversible with temperature. Spectra from eight ices were used to create the figure. The thickness of each ice was ∼1 μm and the spectral resolution was 0.5 cm−1.
Paper: Influences on Infrared Spectra of Benzene Ices for Titan, Comets, and Beyond: Annealings, Artifacts, and Isosbestic Points
Authors: Reggie L. Hudson, Perry A. Gerakines
Figure caption: Crystallization of amorphous benzene at 50 K as followed by the growth of the crystalline-benzene peak near 708 cm−1 and the fall of the amorphous-benzene peak near 1177 cm−1. The absorbance for the crystalline-ice peak has been scaled (normalized) to its final value, while the absorbance for the amorphous-ice peak has been scaled to its initial value.
Paper: Influences on Infrared Spectra of Benzene Ices for Titan, Comets, and Beyond: Annealings, Artifacts, and Isosbestic Points
Authors: Reggie L. Hudson, Perry A. Gerakines
Figure caption: The spectrum of amorphous benzene recorded in a transmission mode (upper, this work) compared to the spectrum recorded in a reflection mode (lower, Mouzay et al. 2021). The upper spectrum is the same as in Figure 1, but scaled vertically to match the lower spectrum (ice thickness unknown) at 680 cm−1, and is offset vertically for clarity.
Paper: Influences on Infrared Spectra of Benzene Ices for Titan, Comets, and Beyond: Annealings, Artifacts, and Isosbestic Points
Authors: Reggie L. Hudson, Perry A. Gerakines
Figure caption: Crystallization of amorphous benzene at 50 K showing isosbestic points in two IR regions. The amorphous ice was grown at ∼3 μm hr−1 at 10 K to a thickness of about 0.5 μm and then warmed to 50 K. The peaks near 1477 and 675 cm−1 are decreasing during crystallization, while the ones marked by asterisks (*) are increasing (rising).
Paper: Sodium Brightening of (3200) Phaethon near Perihelion
Authors: Qicheng Zhang, Karl Battams, Quanzhi Ye, 泉志 叶, Matthew M. Knight, Carl A. Schmidt
Figure caption: Left: Mercury and its Na I tail seen by the HI1 cameras of STEREO-A (HI1A) and STEREO-B (HI1B) at 7 epochs. The Na I tail extends downward (antisunward) from Mercury in all frames; the diagonal branches extending from Mercury in the 2008 and 2010 frames are saturation artifacts, while diagonal stripes along the tail are residual star trails from imperfect background subtraction. Right: HI1 sensitivity to Na I D photons, as measured by the fitted brightness of Mercury’s tail at each epoch. The computed 0 mag flux of (4.7 ± 0.7) × 1010 photons m−2 s−1 (equivalent to a V = 0 Na I D source magnitude of +0.89 ± 0.16) under the Tappin et al. (2022) HI1A broadband photometric calibration is indicated by the dotted line and shaded region. The uncertainties in these values were generously estimated by the scatter of the HI1A points, allowing for potentially correlated measurement errors comparable to this scatter. Note that Na I D sensitivity varies with the assumed r = 1 au ionization rate, with the values in this plot computed for an assumed rate of 7.59 × 10−6 s−1 (Huebner & Mukherjee 2015).
Paper: Sodium Brightening of (3200) Phaethon near Perihelion
Authors: Qicheng Zhang, Karl Battams, Quanzhi Ye, 泉志 叶, Matthew M. Knight, Carl A. Schmidt
Figure caption: Left: Na I production of Phaethon, 322P, and 323P at perihelion with mean slopes indicated by a faded line, as well as the 3σ upper limits for the asteroids (137924), (174158), and (394130). Right: Na I production multiplied by 100.4H  (proportional to the Na I production per unit reflection cross section) for the same objects. The n = 13.7 ± 0.5 of Phaethon’s activity is considerably steeper than expected for sublimation of metallic Na and instead implies a modified latent heat of L = (1.8 ± 0.2) eV atom−1 = (170 ± 20) kJ mol−1. The uncertainties illustrated for the metallic Na and modified L extrapolations reflect uncertainties in Phaethon’s Na I production rate and subsurface temperature, as elaborated in Appendix C.
Paper: Sodium Brightening of (3200) Phaethon near Perihelion
Authors: Qicheng Zhang, Karl Battams, Quanzhi Ye, 泉志 叶, Matthew M. Knight, Carl A. Schmidt
Figure caption: LASCO C3 color composite (RGB = orange/clear/blue) of the disintegrating Oort Cloud comet C/2012 S1 (ISON) at r = 0.1 au, which may serve as a visual if not physical analog for a more active, Geminids-forming Phaethon. Bright Na I D emission, which appears with a golden hue in this image, highlights the remnants of the nucleus and a heavy (≳millimeter-sized) dust/debris trail. As with Phaethon’s observed activity, this Na I D emission far outshines the sunlight scattered by light (micron-sized) dust grains that typically dominates the optical brightness of active comets at similar r.
Paper: Sodium Brightening of (3200) Phaethon near Perihelion
Authors: Qicheng Zhang, Karl Battams, Quanzhi Ye, 泉志 叶, Matthew M. Knight, Carl A. Schmidt
Figure caption: Variation of the STEREO-A HI1 Na I D calibration with assumed Na I lifetime at r = 1 au (with ∝r 2 scaling). Values from Huebner & Mukherjee (2015; quiet and active Sun mean, selected as our nominal a priori value), Huebner et al. (1992; quiet and active Sun mean), and Fulle et al. (2007) are indicated by their labeled vertical lines. We also indicate the r = 1 au equivalent (40 ± 3) hr lifetime from our Phaethon photometric fit for comparison.
Paper: Sodium Brightening of (3200) Phaethon near Perihelion
Authors: Qicheng Zhang, Karl Battams, Quanzhi Ye, 泉志 叶, Matthew M. Knight, Carl A. Schmidt
Figure caption: Illustration explaining the Na I tail model’s simplified treatment of optical depth along the tail, where only the Na I atoms immediately sunward of any point along the tail contribute to the attenuation of Na I D emission at that point.
Paper: Sodium Brightening of (3200) Phaethon near Perihelion
Authors: Qicheng Zhang, Karl Battams, Quanzhi Ye, 泉志 叶, Matthew M. Knight, Carl A. Schmidt
Figure caption: LASCO C2 and C3 zero-point (ZP) magnitudes derived from 39 Tau. The lines and associated shading indicate linear fits to the zero-points, with the slopes in all C2 and C3 assumed to match the fitted slopes of C2 orange and C3 clear, respectively.
Paper: Sodium Brightening of (3200) Phaethon near Perihelion
Authors: Qicheng Zhang, Karl Battams, Quanzhi Ye, 泉志 叶, Matthew M. Knight, Carl A. Schmidt
Figure caption: Top: visualization of the modeled Na I D tail brightness profile from 3 days before to 3 days after perihelion (T p), smoothed to an FWHM of 250,000 km to approximate the HI1 appearance at α ∼ 90° and normalized to the brightness of the head to illustrate the increasing brightness of the tail relative to the head following perihelion. Bottom left: evolution in the lengths of the tail containing 50%–90% of the total Na I D emission and the effective fluorescence efficiency of the first 3000–100,000 km of the tail and that of the full tail, defined as the mean number of Na I D photons emitted per atom while within that section of tail or, equivalently, the total Na I D photon emission rate from that tail section divided by the Na I production rate. Bottom right: comparison of Phaethon’s observed and modeled Na I D morphology in HI1 under similar observing geometry and stacked to a similar S/N in 2016 before perihelion and in 2022 after perihelion, as well as in LASCO C2 at higher α and resolution in 2022 after perihelion. Models use symmetric ﹩3^{\prime} ﹩ (HI1) and 30″ (C2) FWHM PSFs to approximate the actual slightly trailed PSFs. Dotted curves in the C2 panel trace the expected positions of a tail of β = 1 (micron-sized) dust and one of Na I, demonstrating that the observed tail is compatible only with the latter.
Paper: Sodium Brightening of (3200) Phaethon near Perihelion
Authors: Qicheng Zhang, Karl Battams, Quanzhi Ye, 泉志 叶, Matthew M. Knight, Carl A. Schmidt
Figure caption: Left: phase angle dependence of Phaethon’s r- and Δ-normalized HI1 brightness. Excluding all bins extending to r < 0.2 au isolates measurements presumed to be free of activity to yield our H = 14.33 ± 0.10, G 12 = 0.76 ± 0.29 surface reflection model, with a linear fit shown for comparison. Right: surface-subtracted flux from all 18 apparitions, normalized to Δ = 1 au, expressed relative to the mean solar flux through each bandpass (f ⊙). Dark/light symbols for C2 orange and HI1 highlight observations from 2022/earlier apparitions. Note that these fluxes are measured within differently sized apertures of 45″ radius for C2, 2′ for C3, and ﹩3^{\prime} ﹩ for HI1, so the plotted flux differences correspond only approximately to the physical colors. Vertical error bars indicate ±1σ, upper limits indicate +3σ, and horizontal error bars indicate the full range of the observations contributing to each point for both of these and all following plots.
Paper: Sodium Brightening of (3200) Phaethon near Perihelion
Authors: Qicheng Zhang, Karl Battams, Quanzhi Ye, 泉志 叶, Matthew M. Knight, Carl A. Schmidt
Figure caption: Total Na I D emission rate (top) and Na I production rate (bottom) from Phaethon near perihelion as measured by LASCO and HI1 over all 18 observed apparitions, with the fitted model shown in brown. Darker symbols highlight observations from the 2022 apparition. While fitted by the model, offsets between the different bandpasses have not been corrected for these plotted points to visually demonstrate the close agreement between the observed colors and those expected for Na I D emission. We did, however, use the nominal fitted τ Na = 40 hr rather than the a priori 37 hr to calibrate the plotted HI1 photometry, which amounted to a 13% difference in those points.
Paper: Sodium Brightening of (3200) Phaethon near Perihelion
Authors: Qicheng Zhang, Karl Battams, Quanzhi Ye, 泉志 叶, Matthew M. Knight, Carl A. Schmidt
Figure caption: Stacked frames of Phaethon during its 2022 apparition from SOHO LASCO C2 (top), LASCO C3 (bottom left), and STEREO-A HI1 (bottom right). Phaethon and its tail are much brighter through the orange filters, which transmit Na I D emission, than through the blue filters, which block Na I D emission and where Phaethon is not visible. Each orange/blue pair has been scaled such that a solar-colored source would appear similarly bright in both frames to permit visual comparison. The upward ⊙ arrows indicate the sunward direction to which individual frames were aligned prior to stacking, while the +v arrows indicate the heliocentric velocity direction near the midpoint time of each stack. The C2 and HI1 stacks show slight trailing due to the motion of Phaethon over individual exposures, together with small errors in the astrometric solutions used to align the individual frames.
Paper: Sodium Brightening of (3200) Phaethon near Perihelion
Authors: Qicheng Zhang, Karl Battams, Quanzhi Ye, 泉志 叶, Matthew M. Knight, Carl A. Schmidt
Figure caption: Top: 322P/SOHO and 323P/SOHO seen by LASCO C2 during their latest apparitions. Note the presence of a fragment leading 323P/SOHO by ﹩\sim 1^{\prime} ﹩. Middle/bottom: Na I D emission rates for 322P/323P, with models fitted to all apparitions of 322P and the 2004–2012 apparitions of 323P while its orbit had q = 0.048 au. These models do not fit the observations as well as the one for Phaethon, possibly due to some combination of spatially extended Na I production and optical depths higher than those valid for the approximations used.
Paper: Sodium Brightening of (3200) Phaethon near Perihelion
Authors: Qicheng Zhang, Karl Battams, Quanzhi Ye, 泉志 叶, Matthew M. Knight, Carl A. Schmidt
Figure caption: Apparent trajectory of (3200) Phaethon during its 2022 apparition through the fields of view of the SOHO LASCO C3 (left) and C2 (middle) coronagraphs and the STEREO-A HI1 (HI1A; right), with dates and the location of perihelion labeled. Highlighted sections of the track indicate the periods of each camera’s observations included in our analysis of this apparition. The ⊙ markers in the C3 and C2 panels indicate the size and position of the Sun behind each camera’s occulter, while the square in the C3 panel indicates the relative field of view of C2. The Sun is off the left edge of the HI1A frame.
Paper: Sodium Brightening of (3200) Phaethon near Perihelion
Authors: Qicheng Zhang, Karl Battams, Quanzhi Ye, 泉志 叶, Matthew M. Knight, Carl A. Schmidt
Figure caption: Phaethon’s perihelion activity at all 17 apparitions between 1997 and 2020, as observed by SOHO LASCO C2/C3 and both STEREO-A and STEREO-B HI1. Text labels in each image indicate the perihelion year of the respective apparition along with the time spanned by the image stack, given in days relative to the perihelion time. The sunward direction is oriented upward in all frames.
Paper: Sodium Brightening of (3200) Phaethon near Perihelion
Authors: Qicheng Zhang, Karl Battams, Quanzhi Ye, 泉志 叶, Matthew M. Knight, Carl A. Schmidt
Figure caption: Peak Na I production rate Q max at each apparition, fitted with all other parameters constrained to the results of the all-apparition fit. No trends appear evident, with the Q max of individual apparitions generally consistent with the all-apparition fit of (5.5 ± 0.8) × 1023 atoms s−1.
Paper: Erratum: “Large Impacts onto the Early Earth: Planetary Sterilization and Iron Delivery” (2022, PSJ, 3, 116)
Authors: Robert I. Citron, Sarah T. Stewart
Figure caption: (a) Energy increase in silicate atmospheric particles for θ = 45° simulations. (b) Energy increase in silicate surface particles for θ = 45° simulations. The energy increase for only the supercritical fluid (SCF) component of the atmosphere and surface is shown in gray. The values for the best fit to a power law (Ae  b ) are listed.
Paper: The Upper Atmosphere of Uranus from Stellar Occultations. I. Methods and Validation
Authors: William R. Saunders, Michael J. Person, Paul Withers, Richard G. French, Chanita Tubthong
Figure caption: The U0 channel 2 ingress (left column) and egress (right column) light curves in black compared with simulated H87 (panels (a) and (b)) and S93 (panels (e) and (f)) profiles. Panels (a), (b), (e), and (f) plot the normalized stellar flux of the light curves vs. the projected observer altitude above the 1 bar pressure level. Residuals are shown below each comparison in the same colors (panels (c), (d), (g), and (h)) and share the abscissa. Notice that all of the residuals show scatter near zero above approximately 800 km but diverge significantly from zero at lower altitudes, indicating that the simulated Voyager 2 light curves diverge most strongly from the U0 light curve at the very beginning and end of the occultation.
Paper: The Upper Atmosphere of Uranus from Stellar Occultations. I. Methods and Validation
Authors: William R. Saunders, Michael J. Person, Paul Withers, Richard G. French, Chanita Tubthong
Figure caption: Empirical distribution functions for the H87 Voyager 2 stellar and solar occultation profiles. The residuals shown in Figure 6 were divided into 10 blocks, nine of which are baseline (in black) and one of which is for the occultation (in color). The colors in this figure correspond to the colors used in Figure 6. Notice that the distribution functions for the occultation blocks are all clearly different from the tightly grouped baseline distributions, especially at the tails.
Paper: The Upper Atmosphere of Uranus from Stellar Occultations. I. Methods and Validation
Authors: William R. Saunders, Michael J. Person, Paul Withers, Richard G. French, Chanita Tubthong
Figure caption: Diagram showing the geometry of an occultation. Parallel rays of time-separated starlight enter from the left and are bent by an angle θ as a function of their close approach distance to the planet r. They are received at the observer position y at a distance D from the planet. The ﹩r^{\prime} ﹩ and r″ are dummy variables. Notice that the distance scale (dy) is expanded in the plane of the observer compared to the actual dimensions at the planet (dr). This figure is the same as Figure 1 from Elliot et al. (2003).
Paper: The Upper Atmosphere of Uranus from Stellar Occultations. I. Methods and Validation
Authors: William R. Saunders, Michael J. Person, Paul Withers, Richard G. French, Chanita Tubthong
Figure caption: Filled circles show Q–Q values for the S93 residuals shown in Figures 6(g) and (h), as in Figure 9. Similar to Figures 6(g) and (h), blue circles show S93 stellar ingress, orange circles show S93 stellar egress, and green circles show S93 solar ingress. The quantiles of the residuals are shown on the y-axis, and the theoretical quantiles for a normal distribution are shown on the x-axis. The solid red line represents the two distributions being equal, and the dashed red lines are the 99.99% confidence intervals. Notice that in all six panels, the distributions lie outside the confidence intervals in some areas, especially at the tails.
Paper: The Upper Atmosphere of Uranus from Stellar Occultations. I. Methods and Validation
Authors: William R. Saunders, Michael J. Person, Paul Withers, Richard G. French, Chanita Tubthong
Figure caption: Filled circles show Q–Q values for the H87 residuals shown in Figures 6(c) and (d). Similar to Figures 6(c) and (d), red circles show H87 stellar ingress/egress, and purple circles show H87 solar ingress. The quantiles of the residuals are shown on the y-axis, and the theoretical quantiles for a normal distribution are shown on the x-axis. The solid black line represents the two distributions being equal, and the dashed black lines are the 99.99% confidence intervals. Notice that in all four panels, the distributions lie outside the confidence intervals in some areas, especially at the tails.