adsabs/AstroCLIMB huggingface dataset:
Paper: Rotationally Resolved Mid-infrared Spectroscopy of (16) Psyche
Authors: Anicia Arredondo, Margaret M. McAdam, Tracy M. Becker, Linda Elkins-Tanton, Zoe Landsman, Thomas Müller
Figure caption: Left: shape model of Psyche viewed from the south pole. Major deviations from the ellipsoid shape are referred to as Alpha, Bravo, and Charlie. Right: global map of Psyche with features labeled. Colors correspond to optical albedo. Both plots are from Shepard et al. (2021).
Paper: Rotationally Resolved Mid-infrared Spectroscopy of (16) Psyche
Authors: Anicia Arredondo, Margaret M. McAdam, Tracy M. Becker, Linda Elkins-Tanton, Zoe Landsman, Thomas Müller
Figure caption: Comparison of the average spectrum found in this work with previously published MIR spectra of Psyche. Gray dotted lines guide the eye to features of interest and are referenced in the text by the numbers 1–5. Shaded area represents error in the spectra. The error for our average spectrum is smaller than the line thickness. Spectra were digitized using WebPlotDigitizer (Marin et al. 2017).
Paper: Rotationally Resolved Mid-infrared Spectroscopy of (16) Psyche
Authors: Anicia Arredondo, Margaret M. McAdam, Tracy M. Becker, Linda Elkins-Tanton, Zoe Landsman, Thomas Müller
Figure caption: Average emissivity for each night (blue, red, and yellow) compared with the average of all nights (black). The location of the potential CF is marked by a gray arrow.
Paper: Rotationally Resolved Mid-infrared Spectroscopy of (16) Psyche
Authors: Anicia Arredondo, Margaret M. McAdam, Tracy M. Becker, Linda Elkins-Tanton, Zoe Landsman, Thomas Müller
Figure caption: Left: orientation of the asteroid at the beginning of each night. The shape model is from Viikinkoski et al. (2018) and was accessed using the Interactive Service for Asteroid Models. Right: approximate phase coverage of the three nights of observations.
Paper: Rotationally Resolved Mid-infrared Spectroscopy of (16) Psyche
Authors: Anicia Arredondo, Margaret M. McAdam, Tracy M. Becker, Linda Elkins-Tanton, Zoe Landsman, Thomas Müller
Figure caption: Best NEATM fit (red line) for scaled G111 (left) and G227 (right) F821 spectra. The derived values for p  V  and η do not match for each set.
Paper: Rotationally Resolved Mid-infrared Spectroscopy of (16) Psyche
Authors: Anicia Arredondo, Margaret M. McAdam, Tracy M. Becker, Linda Elkins-Tanton, Zoe Landsman, Thomas Müller
Figure caption: Emissivity spectra resulting from scaling G227 spectra to the flux of the TPM and dividing the TPM out.
Paper: Rotationally Resolved Mid-infrared Spectroscopy of (16) Psyche
Authors: Anicia Arredondo, Margaret M. McAdam, Tracy M. Becker, Linda Elkins-Tanton, Zoe Landsman, Thomas Müller
Figure caption: F821 Emissivity spectra resulting from fitting NEATM to G111 spectra and scaling G227 spectra to match.
Paper: Rotationally Resolved Mid-infrared Spectroscopy of (16) Psyche
Authors: Anicia Arredondo, Margaret M. McAdam, Tracy M. Becker, Linda Elkins-Tanton, Zoe Landsman, Thomas Müller
Figure caption: Emissivity of each set with an offset in descending order of rotational phase. The average of all sets is shown in black.
Paper: Surface Roughness at the Moon’s South Pole: The Influence of Condensed Volatiles on Surface Roughness at the Moon’s South Pole
Authors: Lizeth O. Magaña, Parvathy Prem, Ariel N. Deutsch, Anna C. Martin, Heather M. Meyer, Caleb I. Fassett, Michael K. Barker, Angela Stickle, Benjamin D. Byron, Kathleen E. Mandt, Kurt D. Retherford
Figure caption: Annual (a) maximum and (b) average bolometric temperature for the lunar south pole. Cold traps (T max <110 K) are outlined in black.
Paper: Surface Roughness at the Moon’s South Pole: The Influence of Condensed Volatiles on Surface Roughness at the Moon’s South Pole
Authors: Lizeth O. Magaña, Parvathy Prem, Ariel N. Deutsch, Anna C. Martin, Heather M. Meyer, Caleb I. Fassett, Michael K. Barker, Angela Stickle, Benjamin D. Byron, Kathleen E. Mandt, Kurt D. Retherford
Figure caption: South pole (poleward of 85° S) surface roughness (50 m baseline) vs. temperatures, where the colored points correspond to the normalized LAMP Off-band/On-band ratio and have a minimum threshold of 1.0. Slopes greater than 10° are not included. Vertical dashed lines represent 1 Gyr and 1 Myr lifetimes of surface and subsurface condensed H2O. Red trend lines represent a linearly increasing best fit between 70 K < T max < 110 K and 150 K < T max < 250 K.
Paper: Surface Roughness at the Moon’s South Pole: The Influence of Condensed Volatiles on Surface Roughness at the Moon’s South Pole
Authors: Lizeth O. Magaña, Parvathy Prem, Ariel N. Deutsch, Anna C. Martin, Heather M. Meyer, Caleb I. Fassett, Michael K. Barker, Angela Stickle, Benjamin D. Byron, Kathleen E. Mandt, Kurt D. Retherford
Figure caption: Frequency distribution of topographic roughness at 50 m scales and 2.5 cm bins. Cold traps are shown in the darker-green shade, and non-cold-trap regions are shown in the lighter-green shade.
Paper: Surface Roughness at the Moon’s South Pole: The Influence of Condensed Volatiles on Surface Roughness at the Moon’s South Pole
Authors: Lizeth O. Magaña, Parvathy Prem, Ariel N. Deutsch, Anna C. Martin, Heather M. Meyer, Caleb I. Fassett, Michael K. Barker, Angela Stickle, Benjamin D. Byron, Kathleen E. Mandt, Kurt D. Retherford
Figure caption: 50 m baseline (1 km resolution) roughness at Amundsen crater (84.°44 S, 83.°07 E). ROIs are outlined in black contours.
Paper: Gravity Investigation to Characterize Enceladus's Ocean and Interior
Authors: Antonio Genova, Marzia Parisi, Anna Maria Gargiulo, Flavio Petricca, Simone Andolfo, Tommaso Torrini, Edoardo Del Vecchio, Christopher R. Glein, Morgan L. Cable, Cynthia B. Phillips, Nicholas E. Bradley, Ricardo L. Restrepo, Declan M. Mages, Alessandra Babuscia, Jonathan I. Lunine
Figure caption: Body-fixed 3D (left) and polar (right) views of the spacecraft orbit evolution during the gravity mapping phase.
Paper: Hunting for Hydrated Minerals on Trans-Neptunian Objects
Authors: Tom Seccull, Wesley C. Fraser, Dominik A. Kiersz, Thomas H. Puzia
Figure caption: The optical reflectance properties of 2004 EW95. (A) Our new GMOS reflectance spectrum of 2004 EW95 is compared to those reported by Seccull et al. (2018). The 2004 EW95/BD-00 2514 spectrum presented here is the same as that reported by Seccull et al. (2018), except that we have doubled its binning factor from 20 to 40. Coarse reflectance spectra produced from single-epoch colors are also shown (Perna et al. 2013; Fraser et al. 2015). Note that the Fraser et al. (2015) VRI colors presented here are not the average colors reported in that work; instead, they are those observed in support of the TNOs are Cool program (Perna et al. 2013) and then reduced and published by Fraser et al. (2015; V − R = 0.38 ± 0.04, R − I = 0.41 ± 0.07). All data sets are scaled to unit reflectance at 0.589 μm. A copy of our GMOS spectrum and the coarse spectra overlaying it are similarly vertically offset by −0.3 for clarity. Hollow points in the GMOS spectrum are affected by incomplete background subtraction, telluric band residuals, proximity to the GMOS chip gaps, or a combination of these effects. (B) Our GMOS spectrum of 2004 EW95 after removal of the linear continuum (fitted at 0.54–0.57 μm and 0.83–0.87 μm). Points affected by residuals of telluric absorption or imperfect background subtraction have been omitted. For comparison we plot a reflectance spectrum of the Hilda asteroid 748 Simeisa that has been similarly continuum corrected, vertically offset by +0.03 for clarity, and binned to approximately the same resolution as that of our 2004 EW95 spectrum. The 748 Simeisa spectrum was retrieved from the PDS Small Bodies Node (Vilas et al. 2020). The data behind this figure are available in FITS format in a .tar.gz package.(The data used to create this figure are available.)
Paper: Hunting for Hydrated Minerals on Trans-Neptunian Objects
Authors: Tom Seccull, Wesley C. Fraser, Dominik A. Kiersz, Thomas H. Puzia
Figure caption: The optical reflectance properties of 2003 AZ84. (A) Our new GMOS reflectance spectra of 2003 AZ84 are presented alongside coarse reflectance spectra derived from single-epoch VRI colors (Fornasier et al. 2004; Santos-Sanz et al. 2009; Perna et al. 2010). Hollow points in the spectra are affected by incomplete background subtraction, telluric band residuals, proximity to the GMOS chip gaps, or a combination of these effects. All data sets are scaled to unit reflectance at 0.7 μm and are vertically offset for clarity. Reflectance spectra observed at different epochs are offset in increments of +0.3, and those from the same epoch but calibrated with different stars are offset from each other by ±0.1. (B) The new spectra of 2003 AZ84 are directly compared to each other to highlight the differences in their gradients. Spectra on the left are calibrated with HD 78534; those on the right are calibrated with HD 54351. (C) Here we show our 2003 AZ84 spectra following division by a line fitted to them across their full wavelength coverage. Spectra from each epoch are vertically offset for clarity in increments of +0.1. Only spectra calibrated with HD 78534 are shown. Points affected by residuals of telluric absorption or imperfect background subtraction have been omitted. (D) A plot of the gradients (see Table 1) measured for each spectrum of 2003 AZ84 calibrated with HD 78534 against the estimated rotational phase of the object at the time of observation. We adopt a nominal rotational period of 6.75 ± 0.04 hr (Thirouin et al. 2010) and set a phase of zero to coincide with the start of our first observation of 2003 AZ84. Rotational phase error bars show the rotational coverage of each observation. The black bar in the upper right corner shows the total rotational phase uncertainty accumulated over all four epochs; for each individual epoch the uncertainty is <0.001 (see text). The data behind this figure are available in FITS format in a .tar.gz package.(The data used to create this figure are available.)
Paper: Hunting for Hydrated Minerals on Trans-Neptunian Objects
Authors: Tom Seccull, Wesley C. Fraser, Dominik A. Kiersz, Thomas H. Puzia
Figure caption: The 2004 EW95/HD 117286 reflectance spectrum published by Seccull et al. (2018) compared to the model of its 0.7 μm band reported by Seccull (2020). We also compare the Cycle 18 HST colors reported for 2004 EW95 by Fraser et al. (2015). All data sets are scaled to unit reflectance at 0.589 μm.
Paper: Hunting for Hydrated Minerals on Trans-Neptunian Objects
Authors: Tom Seccull, Wesley C. Fraser, Dominik A. Kiersz, Thomas H. Puzia
Figure caption: Our GMOS-N 2003 AZ84/HD 78534 reflectance spectra presented as in Figure 4, but with each spectrum presented in its binned (yellow) and unbinned (black) states. Spectra are ordered from bottom to top in order of observation date: 2021 November 5, 2021 December 14, 2022 January 23, and 2022 January 25. The binned spectrum from 2022 January 23 has a binning factor of 94; the binned spectra from all other epochs are binned by a factor of 66.
Paper: Hunting for Hydrated Minerals on Trans-Neptunian Objects
Authors: Tom Seccull, Wesley C. Fraser, Dominik A. Kiersz, Thomas H. Puzia
Figure caption: Our GMOS-S 2004 GV9/HD 124523 reflectance spectra presented as in Figure 1, but with each spectrum presented in its binned (yellow) and unbinned (black) states. Spectra are ordered from bottom to top in order of observation date: 2022 March 7, 2023 April 19, 2023 April 20, and 2023 April 25. The lowest (first) binned spectrum has a binning factor of 60, and all other binned spectra are binned by a factor of 12.
Paper: Hunting for Hydrated Minerals on Trans-Neptunian Objects
Authors: Tom Seccull, Wesley C. Fraser, Dominik A. Kiersz, Thomas H. Puzia
Figure caption: Our new GMOS-S reflectance spectrum of 2004 EW95 presented as in Figure 2, but in both its binned (×30; yellow) and unbinned (black) states.
Paper: Dynamic Secondary Illumination in Permanent Shadows within Artemis III Candidate Landing Regions
Authors: Prasun Mahanti, Jean-Pierre Williams, Mark S. Robinson, Robert Wagner, Erwan Mazarico, Megan Henriksen, Holly Brown, Nandita Kumari
Figure caption: Role of local topography outside the PSR boundary in moderating the maximum secondary illumination within the four PSRs (A: PSR 1, B: PSR 2, C: PSR 3, and D: PSR 4). Note the “perched” nature of the location of PSRs 3 and 4 visible in the average elevation profiles (vertical: 12 o’clock to 6 o’clock in red; horizontal: 9 o’clock to 3 o’clock in blue) with respect to the topographic grid. Note that the average elevation profile represents the whole map area. The yellow arrow shows the direction of the south pole. Spatial X- and Y-axes are in kilometers, and elevations are in meters. The color scale indicates normalized primary illumination—darker shades indicate low illumination, and brighter shades indicate higher levels of primary illumination for the summer season. Inside PSRs, darker shades indicate lower levels of secondary illumination, and brighter shades indicate higher levels of secondary illumination (see Figure 5).
Paper: Dynamic Secondary Illumination in Permanent Shadows within Artemis III Candidate Landing Regions
Authors: Prasun Mahanti, Jean-Pierre Williams, Mark S. Robinson, Robert Wagner, Erwan Mazarico, Megan Henriksen, Holly Brown, Nandita Kumari
Figure caption: Histograms of the mean sublimation rates for water from the PSRs in Figure 10 (A: PSR 1, B: PSR 2, C: PSR 3, and D: PSR 4). The vertical dashed lines show the sublimation rate for 100 kg m−2 Gyr−1, the approximate threshold for long-term ice stability.
Paper: Dynamic Secondary Illumination in Permanent Shadows within Artemis III Candidate Landing Regions
Authors: Prasun Mahanti, Jean-Pierre Williams, Mark S. Robinson, Robert Wagner, Erwan Mazarico, Megan Henriksen, Holly Brown, Nandita Kumari
Figure caption: Change in secondary illumination (Wm−2 sr−1 μm−1) at a specific location (blue) and the PSR average between 2024 January 16 and 2024 January 18 for the PSR within Marvin.
Paper: Dynamic Secondary Illumination in Permanent Shadows within Artemis III Candidate Landing Regions
Authors: Prasun Mahanti, Jean-Pierre Williams, Mark S. Robinson, Robert Wagner, Erwan Mazarico, Megan Henriksen, Holly Brown, Nandita Kumari
Figure caption: Radially and time-averaged illuminance of surface versus distance from the center of the PSR.
Paper: Dynamic Secondary Illumination in Permanent Shadows within Artemis III Candidate Landing Regions
Authors: Prasun Mahanti, Jean-Pierre Williams, Mark S. Robinson, Robert Wagner, Erwan Mazarico, Megan Henriksen, Holly Brown, Nandita Kumari
Figure caption: Peak summer illumination magnitudes for PSRs 1, 2, and 4 corresponding to subsolar longitudes for high-signal (top row) and low-signal (bottom row) cases in Figure 9 (Section 2.3). Note that the low-signal color bar is 3 orders of magnitude lower.
Paper: Dynamic Secondary Illumination in Permanent Shadows within Artemis III Candidate Landing Regions
Authors: Prasun Mahanti, Jean-Pierre Williams, Mark S. Robinson, Robert Wagner, Erwan Mazarico, Megan Henriksen, Holly Brown, Nandita Kumari
Figure caption: Cumulative distribution function of sublimation rates estimated spatially for the four PSRs (pixel size = 240 m). The dashed line indicates the sublimation rate for water (A: PSR 1, B: PSR 2, C: PSR 3, D: PSR 4).
Paper: Dynamic Secondary Illumination in Permanent Shadows within Artemis III Candidate Landing Regions
Authors: Prasun Mahanti, Jean-Pierre Williams, Mark S. Robinson, Robert Wagner, Erwan Mazarico, Megan Henriksen, Holly Brown, Nandita Kumari
Figure caption: Change in secondary illumination magnitude for PSR 2 inside Marvin crater on 2024 January 18.
Paper: Dynamic Secondary Illumination in Permanent Shadows within Artemis III Candidate Landing Regions
Authors: Prasun Mahanti, Jean-Pierre Williams, Mark S. Robinson, Robert Wagner, Erwan Mazarico, Megan Henriksen, Holly Brown, Nandita Kumari
Figure caption: Maximum secondary illumination for PSRs (A: PSR 1, B: PSR 2, C: PSR 3, D: PSR 4) integrated over summer (subsolar latitude < − 1.5). X, Y are in kilometers, and color scale is in radiance.
Paper: Dynamic Secondary Illumination in Permanent Shadows within Artemis III Candidate Landing Regions
Authors: Prasun Mahanti, Jean-Pierre Williams, Mark S. Robinson, Robert Wagner, Erwan Mazarico, Megan Henriksen, Holly Brown, Nandita Kumari
Figure caption: Average summer illumination magnitudes in log scale. Primary illumination in blue, secondary illumination in red, and error bars indicate the standard deviation of illumination over summer.
Paper: Dynamic Secondary Illumination in Permanent Shadows within Artemis III Candidate Landing Regions
Authors: Prasun Mahanti, Jean-Pierre Williams, Mark S. Robinson, Robert Wagner, Erwan Mazarico, Megan Henriksen, Holly Brown, Nandita Kumari
Figure caption: Number of days in summer.
Paper: Dynamic Secondary Illumination in Permanent Shadows within Artemis III Candidate Landing Regions
Authors: Prasun Mahanti, Jean-Pierre Williams, Mark S. Robinson, Robert Wagner, Erwan Mazarico, Megan Henriksen, Holly Brown, Nandita Kumari
Figure caption: Simulated secondary illumination within PSRs (radiance units) overlaid on simulated primary illumination, cropped to 3 km distance from the PSR perimeter in all directions. The color bar indicates radiance values for the PSR. The maps show maximum secondary illumination over the peak summer period; pixel values can have different time stamps. PSRs 1 and 2 show a larger spatial variability in secondary illumination magnitude over the peak summer compared to the other two PSRs. Note (A) PSR 1 near de Gerlache crater, (B) PSR 2 in Marvin crater, (C) PSR 3 on Leibnitz plateau (Mons Mouton), and (D) PSR 4 in peak near Shackleton.
Paper: Dynamic Secondary Illumination in Permanent Shadows within Artemis III Candidate Landing Regions
Authors: Prasun Mahanti, Jean-Pierre Williams, Mark S. Robinson, Robert Wagner, Erwan Mazarico, Megan Henriksen, Holly Brown, Nandita Kumari
Figure caption: Hourly map for the primary and secondary illumination for PSR 2 at Marvin crater for 2024 January 18.
Paper: Pre-impact Thermophysical Properties and the Yarkovsky Effect of NASA DART Target (65803) Didymos
Authors: Benjamin Rozitis, Simon F. Green, Samuel L. Jackson, Colin Snodgrass, Cyrielle Opitom, Thomas G. Müller, Ulrich C. Kolb, Steven R. Chesley, R. Terik Daly, Cristina A. Thomas, Andrew S. Rivkin
Figure caption: Thermal-infrared observations and thermophysical modeling of the Didymos system. (a) Mid-infrared photometry and spectroscopy acquired by the VLT telescope prior to the DART impact. The average fluxes are shown for each wavelength, and the best-fit continua determined by the ATPM are shown for comparison. Here, Dimorphos contributes ∼5% to the total observed flux. (b) Example reduced-χ 2 contour plot showing the best-fit thermophysical solution when the diameters of Didymos and Dimorphos are held constant at their nominal values. (c) Two-dimensional histogram demonstrating the co-variance between the combined diameter and best-fit thermal inertia resulting from Monte Carlo sampling of the diameter uncertainties. (d) Two-dimensional histogram of the best-fit thermal inertia and thermal roughness resulting from Monte Carlo sampling of the input physical properties and mid-infrared data.
Paper: Pre-impact Thermophysical Properties and the Yarkovsky Effect of NASA DART Target (65803) Didymos
Authors: Benjamin Rozitis, Simon F. Green, Samuel L. Jackson, Colin Snodgrass, Cyrielle Opitom, Thomas G. Müller, Ulrich C. Kolb, Steven R. Chesley, R. Terik Daly, Cristina A. Thomas, Andrew S. Rivkin
Figure caption: Photometric phase curve and modeling of the Didymos system. (a) Observations acquired by the PIRATE telescope in 2022 combined with historical observations reported in Kitazato et al. (2004). The combined data set has been fit with the two-parameter H, G model. (b) Observations reported to the Minor Planet Center (MPC) in the V band. This data set has been fit with both a shape-based Hapke model and the two-parameter H, G model. (c) Residuals of the shape-based Hapke model as a function of observation date. (d) Same as panel (c) but as a function of heliocentric distance. In panels (b)–(d), the MPC observations reported immediately post-impact are highlighted (red asterisks) to demonstrate the DART-induced increase in brightness of the Didymos system.
Paper: Pre-impact Thermophysical Properties and the Yarkovsky Effect of NASA DART Target (65803) Didymos
Authors: Benjamin Rozitis, Simon F. Green, Samuel L. Jackson, Colin Snodgrass, Cyrielle Opitom, Thomas G. Müller, Ulrich C. Kolb, Steven R. Chesley, R. Terik Daly, Cristina A. Thomas, Andrew S. Rivkin
Figure caption: Spacecraft resolved images (not all to scale) of the S-type near-Earth asteroids (433) Eros (left), (25143) Itokawa (top right), and (65803) Didymos/Dimorphos (bottom right). These asteroids have thermal inertia values of 150 ± 50 (Mueller 2012; Rozitis 2017), 700 ± 200 (Müller et al. 2005; Müller et al. 2014), and 320 ± 70 (this work) J m−2 K−1 s−1/2, respectively. For the Didymos/Dimorphos composite image (bottom right), Dimorphos (smaller body) is shown at a higher resolution than Didymos (larger body), their north poles are oriented upwards, and their relative sizes and the distance between them are drawn to scale (Daly et al. 2023). Image credit NASA and JAXA.
Paper: Pre-impact Thermophysical Properties and the Yarkovsky Effect of NASA DART Target (65803) Didymos
Authors: Benjamin Rozitis, Simon F. Green, Samuel L. Jackson, Colin Snodgrass, Cyrielle Opitom, Thomas G. Müller, Ulrich C. Kolb, Steven R. Chesley, R. Terik Daly, Cristina A. Thomas, Andrew S. Rivkin
Figure caption: Residuals of the ATPM fit to the (a) August and (b) September mid-infrared photometry as a function of observation time. The shaded gray area indicates the level of flux variability expected from the Didymos system, as inferred from optical light curves (Pravec et al. 2022; Scheirich & Pravec 2022). The observation start times including light-time corrections were 59815.26401 and 59848.18858 in Modified Julian Date (MJD), respectively.
Paper: Pre-impact Thermophysical Properties and the Yarkovsky Effect of NASA DART Target (65803) Didymos
Authors: Benjamin Rozitis, Simon F. Green, Samuel L. Jackson, Colin Snodgrass, Cyrielle Opitom, Thomas G. Müller, Ulrich C. Kolb, Steven R. Chesley, R. Terik Daly, Cristina A. Thomas, Andrew S. Rivkin
Figure caption: Bulk density of the Didymos system derived from model-to-measurement comparisons of its Yarkovsky orbital drift. (a) Two-dimensional histogram of bulk density derived from Monte Carlo sampling of the input thermophysical properties and measured Yarkovsky orbital drift. The reference model trend gives the bulk density derived as a function of thermal inertia when the other input properties have been held constant. (b) Bulk density distributions derived if either the thermal inertia (TI) remains constant or varies during the eccentric heliocentric orbit of Didymos. In both panels, the spin-limit density (∼2640 kg m−3) indicates the bulk density at which self-gravity balances equatorial centrifugal forces for the Didymos primary body.
Paper: Pre-impact Thermophysical Properties and the Yarkovsky Effect of NASA DART Target (65803) Didymos
Authors: Benjamin Rozitis, Simon F. Green, Samuel L. Jackson, Colin Snodgrass, Cyrielle Opitom, Thomas G. Müller, Ulrich C. Kolb, Steven R. Chesley, R. Terik Daly, Cristina A. Thomas, Andrew S. Rivkin
Figure caption: Yarkovsky effect induced accelerations of the Didymos system as a function of heliocentric distance. The radial component gives the acceleration directed along the Sun-asteroid vector, and the transverse component gives the acceleration directed along the vector perpendicular to the radial vector in the direction of the asteroid velocity. The constant thermal inertia accelerations assume a constant value of 320 J m−2 K−1 s−1/2 around the Didymos orbit, and the variable thermal inertia accelerations assume it varies with heliocentric distance according to Equation (18) with an exponent ξ of −0.75. Both acceleration profiles have been computed assuming a bulk density of 2750 kg m−3.