adsabs/AstroCLIMB huggingface dataset:
Paper: The Outer Edge of the Venus Zone around Main-sequence Stars
Authors: Monica R. Vidaurri, Sandra T. Bastelberger, Eric T. Wolf, Shawn Domagal-Goldman, Ravi Kumar Kopparapu
Figure caption: A comparison of CO2 condensation occurrence as a function of incident stellar flux between each star type. Each near-vertical dashed black line indicates the input mixing ratio of CO2. The solid curves indicate the ratio of saturation vapor pressure of CO2 and the ambient pressure, labeled as F SAT. Onset of CO2 condensation occurs when F SAT converges to the CO2 volume mixing ratio—in other words, when F SAT is less than or equal to the mixing ratio of CO2. Note that this is equivalent to more conventional descriptions that define the onset of condensation to occur when the partial pressure of a given gas exceeds its saturation vapor pressure. We define the outer edge of the Venus zone as the stellar flux where CO2 begins condensing. Condensation occurs under lower amounts of incident stellar flux for the smaller, cooler stars owing to the efficiency of CO2 in absorbing the higher amounts of near-IR radiation emitted by these stars, thus maintaining a warm atmosphere where CO2 is not readily condensed (see the Figure 1 temperature profile for different stars). For larger, warmer stars, condensation occurs at a higher S eff value owing to scattering of blue light by atmospheric N2, rendering these atmospheres unable to retain greenhouse warming as efficiently as a planet with CO2 around an M dwarf.
Paper: Dust Evolution in the Coma of Distant, Inbound Comet C/2017 K2 (PANSTARRS)
Authors: Qicheng Zhang, Ludmilla Kolokolova, Quanzhi Ye, 泉志 叶, Shreyas Vissapragada
Figure caption: HST ACS/WFC color imaging and polarimetry of C/2017 K2. Upper left: composite of nonpolarized F475W (﹩g^{\prime} ﹩) and F775W (﹩i^{\prime} ﹩) frames, overlaid with a selection of isophots. The compasses indicate north (N) and east (E), as well as the sunward (+⊙) and heliocentric velocity (+v) directions. Upper right: F475W–F775W color map of the same region, with values labeled as reflectance slopes relative to solar color, median smoothed to 0.″5 ∼ 2500 km resolution for display clarity. The color map shows a relatively bluer region surrounding the nucleus. Lower left: F775W intensity divided by a 1/ρ model, overlaid with markers indicating the direction and degree of polarization. The scale bar to the upper left indicates the length of a marker representing 3% polarization degree. Lower right: F775W polarization map, smoothed to 1″ ∼ 5000 km resolution, showing a region of relatively weaker negative polarization surrounding the nucleus. All panels are displayed at the same scale and orientation.
Paper: The Outer Edge of the Venus Zone around Main-sequence Stars
Authors: Monica R. Vidaurri, Sandra T. Bastelberger, Eric T. Wolf, Shawn Domagal-Goldman, Ravi Kumar Kopparapu
Figure caption: A comparison of CO2 condensation zones for our various Venus analogs. Solid thick bands indicate where CO2 is condensed within the atmosphere of a given Venus analog. For a 3000 K M star, CO2 begins condensing in our Venus analog at 0.3 S eff, and for a 3400 K M star, CO2 begins condensing at 0.32 S eff. For a G star, CO2 begins condensing in our Venus-analog atmosphere at 0.55 S eff, whereas a Venus analog around a K star and an F star begins CO2 condensation at 0.38 and 0.8 S eff, respectively. For M- and K-star profiles, CO2 condensation occurs lower in the atmosphere compared to F and G stars. As noted in Figure 1, the N2 in our Venus analogs is effective at scattering blue light that is most present in F and G stars, while CO2 is effective at absorbing light in the infrared that is most present in M and K stars, therefore maintaining heat and additionally allowing heat to be maintained to the surface.
Paper: The Outer Edge of the Venus Zone around Main-sequence Stars
Authors: Monica R. Vidaurri, Sandra T. Bastelberger, Eric T. Wolf, Shawn Domagal-Goldman, Ravi Kumar Kopparapu
Figure caption: The Venus-zone outer edge (gray line) as a function of stellar flux received relative to Earth, with the inner edge (green dashed) and outer edge (blue dashed) of the habitable zone included for comparison. Conservative habitable-zone estimates were taken from Kopparapu et al. (2013).
Paper: The Volatile Carbon-to-oxygen Ratio as a Tracer for the Formation Locations of Interstellar Comets
Authors: Darryl Z. Seligman, Leslie A. Rogers, Samuel H. C. Cabot, John W. Noonan, Theodore Kareta, Kathleen E. Mandt, Fred Ciesla, Adam McKay, Adina D. Feinstein, W. Garrett Levine, Jacob L. Bean, Thomas Nordlander, Mark R. Krumholz, Megan Mansfield, Devin J. Hoover, Eric Van Clepper
Figure caption: Overview of measurements of the C/O in solar system and interstellar comets. The comets presented in A’Hearn et al. (1995) with only C2, C3, CN, and OH production rates measured are shown with purple points. The comets with measured CO2, CO, and H2O production rates listed in Table 1 are shown with blue points. The C/O ratios of Borisov and ‘Oumuamua are shown in gold and red, assuming that the acceleration of ‘Oumuamua was caused by CO outgassing. We include points for all four CO detections of 2I/Borisov (see Figure 6) to highlight their relevance to this paper. The vertical dashed line indicates the region interior to which H2O is active, which explains the high inferred C/O ratio of the Centaur 29P. The blue and pink regions indicate primordial cometary C/O ratios indicative of formation interior and exterior to the CO snow line. The comets C/2009 P1 Garradd, C/2010 G2 Hill, and C/2006 W3 Christensen also have high C/O ratios and are indicated with arrows.
Paper: The Volatile Carbon-to-oxygen Ratio as a Tracer for the Formation Locations of Interstellar Comets
Authors: Darryl Z. Seligman, Leslie A. Rogers, Samuel H. C. Cabot, John W. Noonan, Theodore Kareta, Kathleen E. Mandt, Fred Ciesla, Adam McKay, Adina D. Feinstein, W. Garrett Levine, Jacob L. Bean, Thomas Nordlander, Mark R. Krumholz, Megan Mansfield, Devin J. Hoover, Eric Van Clepper
Figure caption: The C/O ratios for comets calculated using weighted production rates of C2, C3, CN, and H2O (from OH). These comets are in the sample presented by A’Hearn et al. (1995). The error bars are calculated by adding the reported uncertainties in quadrature scaled by the weighting of the species for the abundance ratio.
Paper: The Volatile Carbon-to-oxygen Ratio as a Tracer for the Formation Locations of Interstellar Comets
Authors: Darryl Z. Seligman, Leslie A. Rogers, Samuel H. C. Cabot, John W. Noonan, Theodore Kareta, Kathleen E. Mandt, Fred Ciesla, Adam McKay, Adina D. Feinstein, W. Garrett Levine, Jacob L. Bean, Thomas Nordlander, Mark R. Krumholz, Megan Mansfield, Devin J. Hoover, Eric Van Clepper
Figure caption: Schematic diagram showing two distinct stages of an interstellar comet’s lifetime. On the left-hand side, the comet is traveling through the ISM. It experiences continuous isotropic radiation and interaction with ambient gas, which removes volatile material off of the surface. The overall reduction of the radius in this phase of the object’s lifetime is denoted as ΔR ISM. On the right-hand side, the comet has finished its journey through the ISM and is traveling through the solar system. There is a focused ablation of material due to sublimation from solar irradiation, which produces a cometary tail. Averaged over many tumbles of the object and orientations to the Sun, this erosion produces an additional change in radius, which we denote as ΔR SS.
Paper: The Volatile Carbon-to-oxygen Ratio as a Tracer for the Formation Locations of Interstellar Comets
Authors: Darryl Z. Seligman, Leslie A. Rogers, Samuel H. C. Cabot, John W. Noonan, Theodore Kareta, Kathleen E. Mandt, Fred Ciesla, Adam McKay, Adina D. Feinstein, W. Garrett Levine, Jacob L. Bean, Thomas Nordlander, Mark R. Krumholz, Megan Mansfield, Devin J. Hoover, Eric Van Clepper
Figure caption: Evolution of the relative production rates of a kilometer-scale comet experiencing mass loss in the ISM. The blue and red curves indicate the time-integrated number of sublimated CO and CO2 relative to H2O molecules. The lower x- axis corresponds to the look-back time prior to entering the solar system, while the upper axis shows the corresponding present-day maximum vertical excursion in the galactic orbit. The dashed–dotted lines indicate the inferred age and excursion of ‘Oumuamua and Borisov.
Paper: The Volatile Carbon-to-oxygen Ratio as a Tracer for the Formation Locations of Interstellar Comets
Authors: Darryl Z. Seligman, Leslie A. Rogers, Samuel H. C. Cabot, John W. Noonan, Theodore Kareta, Kathleen E. Mandt, Fred Ciesla, Adam McKay, Adina D. Feinstein, W. Garrett Levine, Jacob L. Bean, Thomas Nordlander, Mark R. Krumholz, Megan Mansfield, Devin J. Hoover, Eric Van Clepper
Figure caption: Comparison of the composition of R2, 2I, and typical carbon-enriched and carbon-depleted solar system comets. This figure is a generalized version of the analogous figure in McKay et al. (2019). It is feasible that R2 and Borisov are representative of comets that formed exterior to the CO snow line in their original protoplanetary disks, while typical solar system comets formed interior to the CO snow line. The carbon-depleted comet is representative of many of the comets in Table 1, and the carbon-enriched comet is W3 Christensen. The composition for Borisov is derived from Table 2 and references therein, and R2 is from McKay et al. (2019). The lack of CO2 for 2I is only because no measurement of CO2 has been reported.
Paper: The Volatile Carbon-to-oxygen Ratio as a Tracer for the Formation Locations of Interstellar Comets
Authors: Darryl Z. Seligman, Leslie A. Rogers, Samuel H. C. Cabot, John W. Noonan, Theodore Kareta, Kathleen E. Mandt, Fred Ciesla, Adam McKay, Adina D. Feinstein, W. Garrett Levine, Jacob L. Bean, Thomas Nordlander, Mark R. Krumholz, Megan Mansfield, Devin J. Hoover, Eric Van Clepper
Figure caption: Production rate of various volatile species as a function of time relative to perihelia for the interstellar comet 2I/Borisov. The top panel shows the production rates for H2O and CO, which are 2 orders of magnitude higher than those for CN, C2, C3, NH2, and HCN shown in the bottom panel. We also show upper limits measured for OH in the top panel. These production rates and their respective references are itemized in Table 2.
Paper: The Volatile Carbon-to-oxygen Ratio as a Tracer for the Formation Locations of Interstellar Comets
Authors: Darryl Z. Seligman, Leslie A. Rogers, Samuel H. C. Cabot, John W. Noonan, Theodore Kareta, Kathleen E. Mandt, Fred Ciesla, Adam McKay, Adina D. Feinstein, W. Garrett Levine, Jacob L. Bean, Thomas Nordlander, Mark R. Krumholz, Megan Mansfield, Devin J. Hoover, Eric Van Clepper
Figure caption: Comparison of the C/O ratio of comets inferred from production rates of CO2, CO, and H2O (blue) and C2, C3, CN, and H2O from OH (purple). These 13 comets represent the overlap between the comets in Table 1 and those presented in A’Hearn et al. (1995). With only one exception, CO2 and CO are the dominant carbon-bearing species for calculating the C/O ratio.
Paper: The Volatile Carbon-to-oxygen Ratio as a Tracer for the Formation Locations of Interstellar Comets
Authors: Darryl Z. Seligman, Leslie A. Rogers, Samuel H. C. Cabot, John W. Noonan, Theodore Kareta, Kathleen E. Mandt, Fred Ciesla, Adam McKay, Adina D. Feinstein, W. Garrett Levine, Jacob L. Bean, Thomas Nordlander, Mark R. Krumholz, Megan Mansfield, Devin J. Hoover, Eric Van Clepper
Figure caption: Measured C/O ratios in solar twins from Bedell et al. (2018) and Nissen (2015). The resulting combined data set has a mean C/O ratio of ∼0.50 with a standard deviation of σ ∼ 0.04.
Paper: The Volatile Carbon-to-oxygen Ratio as a Tracer for the Formation Locations of Interstellar Comets
Authors: Darryl Z. Seligman, Leslie A. Rogers, Samuel H. C. Cabot, John W. Noonan, Theodore Kareta, Kathleen E. Mandt, Fred Ciesla, Adam McKay, Adina D. Feinstein, W. Garrett Levine, Jacob L. Bean, Thomas Nordlander, Mark R. Krumholz, Megan Mansfield, Devin J. Hoover, Eric Van Clepper
Figure caption: Fraction of mass located exterior to the CO ice line in circumstellar disks for a range of stellar masses and assigned surface density profiles. The dotted line indicates the classically adopted power-law exponent for the minimum-mass solar nebula.
Paper: Formation of Vitreous Salt Hydrates Under Conditions Relevant to Europa
Authors: Paul V. Johnson, Tuan H. Vu
Figure caption: Raman spectra of frozen 2 M MgSO4 brines at 100 K, with the sulfate ν 1 symmetric stretch region highlighted in the inset. The blue trace was obtained from a flash-frozen sample and demonstrates the lineshape (FWHM = 10.1 cm−1 and x 0 = 984.7 cm−1) of the sulfate ν 1 symmetric stretch feature that is characteristic of vitreous MgSO4 hydrate. The red trace was obtained from a sample that was cooled from room temperature to 100 K at 20 K minute−1 and shows the lineshape of the sulfate ν 1 stretch feature that is characteristic of crystalline MgSO4•11H2O (meridianiite) (FWHM = 3.8 cm−1, x 0 = 989.3 cm−1).
Paper: Formation of Vitreous Salt Hydrates Under Conditions Relevant to Europa
Authors: Paul V. Johnson, Tuan H. Vu
Figure caption: Raman spectra of frozen 2 M MgCl2 brines at 100 K. The blue trace was obtained from a flash-frozen sample and demonstrates the smooth, relatively featureless spectrum. The red trace was obtained from a sample that was cooled from room temperature to 100 K at 20 K minute−1 and shows the many sharp features characteristic of crystalline MgCl2•12H2O, with the most prominent at 3512 cm−1.
Paper: Formation of Vitreous Salt Hydrates Under Conditions Relevant to Europa
Authors: Paul V. Johnson, Tuan H. Vu
Figure caption: Raman spectra of frozen 0.1 M NaCl brines at 100 K. The blue trace was obtained from a flash-frozen sample and demonstrates the smooth relatively featureless spectrum. The red trace was obtained from a sample that was cooled from room temperature to 100 K at 50 K minute−1 and shows the sharp features characteristic of crystalline NaCl•2H2O (hydrohalite) at 3400 and 3417 cm−1.
Paper: Formation of Vitreous Salt Hydrates Under Conditions Relevant to Europa
Authors: Paul V. Johnson, Tuan H. Vu
Figure caption: Raman spectrum of a frozen 0.1 M Na2SO4 brine at 100 K with the sulfate ν 1 symmetric stretch region highlighted in the inset. The spectrum was obtained from a flash-frozen sample and shows the lineshape of the sulfate stretch feature that is characteristic of crystalline Na2SO4•10H2O (mirabilite) (FWHM = 3.6 cm−1, x 0 = 991.0 cm−1).
Paper: Juno Spacecraft Measurements of Jupiter’s Gravity Imply a Dilute Core
Authors: Burkhard Militzer, William B. Hubbard, Sean Wahl, Jonathan I. Lunine, Eli Galanti, Yohai Kaspi, Yamila Miguel, Tristan Guillot, Kimberly M. Moore, Marzia Parisi, John E. P. Connerney, Ravid Helled, Hao Cao, Christopher Mankovich, David J. Stevenson, Ryan S. Park, Mike Wong, Sushil K. Atreya, John Anderson, Scott J. Bolton
Figure caption: Comparison of Juno measurements (diamonds) and model predictions for the even and odd gravity coefficients. The large open symbols show results from the dilute core model A in Table 1, while the small symbols represent ensembles of A- and I-type models. The stars show earlier model predictions from Hubbard & Militzer (2016) and Wahl et al. (2017). The large triangles show models that combine dilute and compact cores. The labels indicate the masses of their compact cores in Earth masses.
Paper: Surface Properties of Near-Sun Asteroids
Authors: Carrie E. Holt, Matthew M. Knight, Michael S. P. Kelley, Quanzhi Ye, 泉 志 叶, Henry H. Hsieh, Colin Snodgrass, Alan Fitzsimmons, Derek C. Richardson, Jessica M. Sunshine, Nora L. Eisner, Annika Gustaffson
Figure caption: Color–color diagram of low-q asteroids. The gray crosses are the color values of NEAs from the SDSS MOC (Ivezić et al. 2001, 2002). The large capital letters represent the average colors of the taxonomic classes of NEAs from Dandy et al. (2003). The color of comet 322P from Knight et al. (2016) is shown as a magenta triangle. The first reported color of 323P from Hui et al. (2022) is shown as a magenta diamond. The red circles and blue squares are low-q asteroids with T J less than and greater than 3, respectively.
Paper: Surface Properties of Near-Sun Asteroids
Authors: Carrie E. Holt, Matthew M. Knight, Michael S. P. Kelley, Quanzhi Ye, 泉 志 叶, Henry H. Hsieh, Colin Snodgrass, Alan Fitzsimmons, Derek C. Richardson, Jessica M. Sunshine, Nora L. Eisner, Annika Gustaffson
Figure caption: The KDE plots of low-q asteroid colors with underlying histograms (blue), where data points are weighted by their 1σ uncertainty and the kernel bandwidth is selected according to Scott’s rule (Scott 1992). This allows us to assess the color distribution as a smooth probability density instead of only discrete bins in the histogram. The black shaded curve is the color distribution of NEAs from SDSS MOC. The colors of the most common asteroid types according to Dandy et al. (2003) are shown as letters, and solar colors are shown as an orange symbol. We find a preference toward bluer colors for both ﹩g^{\prime} -r^{\prime} ﹩ (top) and ﹩r^{\prime} -i^{\prime} ﹩ (bottom).
Paper: Surface Properties of Near-Sun Asteroids
Authors: Carrie E. Holt, Matthew M. Knight, Michael S. P. Kelley, Quanzhi Ye, 泉 志 叶, Henry H. Hsieh, Colin Snodgrass, Alan Fitzsimmons, Derek C. Richardson, Jessica M. Sunshine, Nora L. Eisner, Annika Gustaffson
Figure caption: Absolute magnitude comparisons between this work and JPL. The solid line represents equality between the measurements. For all but one point, the error bars are within the marker. We find agreement between the values suggesting none of the objects were active during observations. All measurements, including the largest difference between magnitudes of 1.02 (2008 MG1), are still within typical estimates for rotational variation.
Paper: Surface Properties of Near-Sun Asteroids
Authors: Carrie E. Holt, Matthew M. Knight, Michael S. P. Kelley, Quanzhi Ye, 泉 志 叶, Henry H. Hsieh, Colin Snodgrass, Alan Fitzsimmons, Derek C. Richardson, Jessica M. Sunshine, Nora L. Eisner, Annika Gustaffson
Figure caption: Spectrophotometry of low-q asteroid observations created by transforming colors into reflectance values. Our measurements are in blue at their central wavelength, normalized to the ﹩g^{\prime} ﹩ filter, with uncertainties shown. The gray bar shows the measured gri  -slope. The object’s name and date of observation (YYYYMMDD) are given in each panel.
Paper: Surface Properties of Near-Sun Asteroids
Authors: Carrie E. Holt, Matthew M. Knight, Michael S. P. Kelley, Quanzhi Ye, 泉 志 叶, Henry H. Hsieh, Colin Snodgrass, Alan Fitzsimmons, Derek C. Richardson, Jessica M. Sunshine, Nora L. Eisner, Annika Gustaffson
Figure caption: The gri-slope and ﹩z^{\prime} -i^{\prime} ﹩ reflectance values of low-q asteroids (blue dots). For comparison, we show the distribution of NEAs from the SDSS MOC4 catalog (gray crosses) and the boundaries used to classify SDSS data from DeMeo & Carry (2013). Low-q asteroids have a flatter spectral slope than the NEA population.
Paper: A Numerical Approach Using a Finite Element Model to Constrain the Possible Interior Layout of (16) Psyche
Authors: Yaeji Kim, Masatoshi Hirabayashi
Figure caption: Impact cratering process schematic for a crater-like region on the surface of Psyche. Here, brown shades indicate silicates, while gray shades mean metal.
Paper: A Numerical Approach Using a Finite Element Model to Constrain the Possible Interior Layout of (16) Psyche
Authors: Yaeji Kim, Masatoshi Hirabayashi
Figure caption: Comparison of color maps that shows the core radius between compression rates of 30% and 5%.
Paper: Dust Evolution in the Coma of Distant, Inbound Comet C/2017 K2 (PANSTARRS)
Authors: Qicheng Zhang, Ludmilla Kolokolova, Quanzhi Ye, 泉志 叶, Shreyas Vissapragada
Figure caption: The 1/ρ-equivalent Afρ of annuli (top)—proportional to the intensity divided by a 1/ρ profile—and their radial gradient (bottom). Both observed profiles (red and blue curves) are nearly 1/ρ (∼0%/1000 km gradient) within ρ ∼ 10,000 km, which is shallower than expected by Monte Carlo simulations (black curves; arbitrarily scaled) of only stable, millimeter-sized grains (solid), as found in the outer coma and tail. Faster, micron-sized grains (dashed) produce a shallower profile consistent with the observed profiles within ρ ∼ 10,000 km.
Paper: Dust Evolution in the Coma of Distant, Inbound Comet C/2017 K2 (PANSTARRS)
Authors: Qicheng Zhang, Ludmilla Kolokolova, Quanzhi Ye, 泉志 叶, Shreyas Vissapragada
Figure caption: Radial profiles of F475W–F775W reflectance slope (top) and F775W polarization (bottom), showing a trend of reddening and strengthened negative polarization outward from the nucleus. The solid black curves with error bars indicate values measured from full, 360° annuli, while the dotted red (labeled +⊙) and dashed blue (−⊙) curves show values measured from 90° annular segments centered on the sunward and antisunward directions, respectively.
Paper: Dust Evolution in the Coma of Distant, Inbound Comet C/2017 K2 (PANSTARRS)
Authors: Qicheng Zhang, Ludmilla Kolokolova, Quanzhi Ye, 泉志 叶, Shreyas Vissapragada
Figure caption: Radial profiles of the polarization of C/2012 S1 (ISON), analogous to the one in Figure 2 for C/2017 K2, processed from data collected by HST program GO/DD 13199 (PI: D. Hines) with all frames included (top) and excluding the trailed POL60V frame jc7f01jmq (bottom), showing that removal of this trailed frame effectively eliminates the apparent positively polarized region over the nucleus.
Paper: Dust Evolution in the Coma of Distant, Inbound Comet C/2017 K2 (PANSTARRS)
Authors: Qicheng Zhang, Ludmilla Kolokolova, Quanzhi Ye, 泉志 叶, Shreyas Vissapragada
Figure caption: Radial profiles of J − H (top), H − K  s  (middle), and J − K  s  (bottom) colors from Palomar/WIRC on 2021 May 18, showing no clear trend in any color above the noise limit.
Paper: Dust Evolution in the Coma of Distant, Inbound Comet C/2017 K2 (PANSTARRS)
Authors: Qicheng Zhang, Ludmilla Kolokolova, Quanzhi Ye, 泉志 叶, Shreyas Vissapragada
Figure caption: Composite of J and H frames by Palomar/WIRC. Representative syndynes and synchrones are drawn over the same image and a selection of isophots in the middle and right panels, respectively, and show the prominent northward tail to be predominantly comprising large β ≲ 0.01 (a  d  ≳ 0.1 mm) grains produced years earlier.
Paper: The Volatile Carbon-to-oxygen Ratio as a Tracer for the Formation Locations of Interstellar Comets
Authors: Darryl Z. Seligman, Leslie A. Rogers, Samuel H. C. Cabot, John W. Noonan, Theodore Kareta, Kathleen E. Mandt, Fred Ciesla, Adam McKay, Adina D. Feinstein, W. Garrett Levine, Jacob L. Bean, Thomas Nordlander, Mark R. Krumholz, Megan Mansfield, Devin J. Hoover, Eric Van Clepper
Figure caption: The C/O ratio of grains and gas as a function of heliocentric distance. The ratio is impacted by condensation of oxygen- and carbon-bearing molecules at and beyond their respective snow lines. The C/O profile of gas ends at the CO snow line because all major C- and O-bearing species have condensed beyond this point. Comets that form exterior to the CO snow line have higher C/O ratios than those that form interior to it. This figure is a rendition of Figure 1 in Öberg et al. (2011).