adsabs/AstroCLIMB huggingface dataset:
Paper: Radar Circular Polarization Ratio of Near-Earth Asteroids: Links to Spectral Taxonomy and Surface Processes
Authors: Edgard G. Rivera-Valentín, Betzaida Aponte-Hernández, Patrick A. Taylor, Michael C. Nolan, Ellen S. Howell, Dany Waller, Luisa F. Zambrano-Marín, Anne K. Virkki, Ronald-Louis Ballouz, Angela M. Stickle
Figure caption: The resultant empirical PDF for every studied taxonomic class, scaled by its maximum value. The taxonomic classes are denoted by color following the legend in the figure, within which N is the total number of objects in the taxonomic class.
Paper: Numerical Investigation of the Cohesive Strength Regime of the Bilobated Arrokoth after the Sky-crater-forming Impact Event
Authors: Yaeji Kim, Masatoshi Hirabayashi, James Bauer
Figure caption: The result for the FEM simulation showing the variation on a cross section in the critical cohesive strength of the body constrained by the time-varying stress fields over one oscillation cycle. The variation value defines a subtraction of the critical cohesive strength at a specific time state (Y  c ) from the one at the equilibrium state (Y *). The impact speed, the target’s bulk density, Young’s modulus, and viscosity are set as 100 m s−1, 500 kg m−3, 10 MPa, and 10 Mpa s, respectively.
Paper: How Meteor Showers Can Guide the Search for Long-period Comets
Authors: Samantha Hemmelgarn, Nicholas Moskovitz, Stuart Pilorz, Peter Jenniskens
Figure caption: The top panel shows velocity vectors for each observable synthetic comet in a simulation with shower #206 (the Aurigids) on 1909 July 31. The parent comet’s velocity vector is represented with a red arrow. The black box is a 3° FOV region of the search area centered around the parent comet’s position and represents the FOV of a wide-angle sky survey. The bottom panel is a close-up of this region, showing that velocity vectors of synthetic comets are representative of the velocity vector of the parent comet. The mean rate of synthetic comets in this 3° region is 0.″144 ± 0.″016 minute−1, and the rate of the parent comet is 0.″145 minute−1.
Paper: How Meteor Showers Can Guide the Search for Long-period Comets
Authors: Samantha Hemmelgarn, Nicholas Moskovitz, Stuart Pilorz, Peter Jenniskens
Figure caption: Line plots in panels (a) and (c) show average values of δ  l  and δ  r , respectively, with standard deviations for all showers as a function of heliocentric distance. Histograms in panels (b) and (d) provide distributions of δ  l  and δ  r , respectively, for all simulations across all showers. Error bars in the line plots are the standard deviations across all simulations. Error bars in the histograms are calculated as ﹩\sqrt{N}﹩.
Paper: How Meteor Showers Can Guide the Search for Long-period Comets
Authors: Samantha Hemmelgarn, Nicholas Moskovitz, Stuart Pilorz, Peter Jenniskens
Figure caption: Case study for the shower associated with comet C/1939 H1 (Jurlof-Achmarof-Hassel), the position of which is shown by a red star. Colored circles on the line represent the mean r of synthetic comets in 1° bins along the line. Its δ  l  is 0.°40 and its δ  r  is 0.39 au in this simulation.
Paper: How Meteor Showers Can Guide the Search for Long-period Comets
Authors: Samantha Hemmelgarn, Nicholas Moskovitz, Stuart Pilorz, Peter Jenniskens
Figure caption: A celestial sphere projecting all 17 synthetic comet clouds, with the position of the parent comet plotted as a red star. Orange text denotes the shower number used to generate the cloud.
Paper: How Meteor Showers Can Guide the Search for Long-period Comets
Authors: Samantha Hemmelgarn, Nicholas Moskovitz, Stuart Pilorz, Peter Jenniskens
Figure caption: The observability sweet spot for the Aurigids (IAU shower 206) of comet C/1911 N1 (Kiess) for the date of 1909 March 27, when its parent comet was 9 au from the Sun. The red arrow marks the comet position and direction of motion at that time. ⊙ is the Sun, and ⊕ is Earth. Gray circles are the synthetic comets on Aurigid-type orbits. The region with colored symbols highlights the heliocentric distance range that would be observable for a comet with H = 14.
Paper: How Meteor Showers Can Guide the Search for Long-period Comets
Authors: Samantha Hemmelgarn, Nicholas Moskovitz, Stuart Pilorz, Peter Jenniskens
Figure caption: Distribution of H values for LPCs from JPL’s Small-Body Database. Solid red lines denote assumed cutoff values for comets with undefined bare nucleus magnitudes. Dashed orange lines indicate nominal H values for the six comets in our sample that have this property constrained.
Paper: How Meteor Showers Can Guide the Search for Long-period Comets
Authors: Samantha Hemmelgarn, Nicholas Moskovitz, Stuart Pilorz, Peter Jenniskens
Figure caption: Locations of meteoroid and comet node crossings in the ecliptic plane (left) and the projected location of comet and meteoroids on the sky at two epochs (right; see text for details) for a simulation of shower #206 (the Aurigids). The parent body is marked in both panels with plus signs. The locations of approximately 95% of meteors crossing within 500 yr of the comet at epochs “(a)” and “(b)” are encircled (left), or appear in light gray (right). The subset of Earth-intersecting ejecta is shown in black on the left and in gray scale graded by magnitude on the right. On the right, the comet’s location is shown at vernal equinox for all the years it takes to traverse from V = 25 to V = 22.
Paper: How Meteor Showers Can Guide the Search for Long-period Comets
Authors: Samantha Hemmelgarn, Nicholas Moskovitz, Stuart Pilorz, Peter Jenniskens
Figure caption: R.A./decl. rates (arcsec minute−1) for each simulation (n = 850) color-coded by r. The outer circle represents case 1; the middle circle, case 2; and the inner circle, case 3. The example wedge sets bounds on the rates and angles for a shift-and-stack search in the region defined by shower #531 with H = 14 and r = 4 au, based on bounds discussed in Section 3.2 (±0.″15 minute−1 and ±15°). These bounds reduce the parameter space by 96.5% for this simulation.
Paper: How Meteor Showers Can Guide the Search for Long-period Comets
Authors: Samantha Hemmelgarn, Nicholas Moskovitz, Stuart Pilorz, Peter Jenniskens
Figure caption: Search area on sky for shower #16 (σ-Hydrids) on 2023-01-19.326034 (UT). The synthetic comets in this simulation have an assumed H = 16. Its parent comet, C/2023 P1 (Nishimura), is represented by the red star. The model results show δ  l  = 3.°43, Ψ = 8.°25, ψ  l  = 42%, and δ  r  = 0.24 au.
Paper: How Meteor Showers Can Guide the Search for Long-period Comets
Authors: Samantha Hemmelgarn, Nicholas Moskovitz, Stuart Pilorz, Peter Jenniskens
Figure caption: Differences between mean synthetic comet rates and angles and those of the parent comets inside a 3° FOV search region encompassing the parent comet. The legend shows the percentage of total simulations (n = 850) that fall within bounds of 0.″05 minute−1 and 5° (yellow), 0.″1 minute−1 and 10° (purple), and 0.″15 minute−1 and 15° (green).
Paper: How Meteor Showers Can Guide the Search for Long-period Comets
Authors: Samantha Hemmelgarn, Nicholas Moskovitz, Stuart Pilorz, Peter Jenniskens
Figure caption: Histogram of visual magnitudes of synthetic comets in the search region produced by shower #16 (σ-Hydrids) as seen in Figure 10.
Paper: Candidate Distant Trans-Neptunian Objects Detected by the New Horizons Subaru TNO Survey
Authors: Wesley C. Fraser, Simon B. Porter, Lowell Peltier, JJ Kavelaars, Anne J. Verbiscer, Marc W. Buie, S. Alan Stern, John R. Spencer, Susan D. Benecchi, Tsuyoshi Terai, Takashi Ito, Fumi Yoshida, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, Stephen D. J. Gwyn, Hayden Smotherman, Sebastien Fabbro, Kelsi N. Singer, Amanda M. Alexander, Ko Arimatsu, Maria E. Banks, Veronica J. Bray, Mohamed Ramy El-Maarry, Chelsea L. Ferrell, Tetsuharu Fuse, Florian Glass, Timothy R. Holt, Peng Hong, Ryo Ishimaru, Perianne E. Johnson, Tod R. Lauer, Rodrigo Leiva, Patryk S. Lykawka, Raphael Marschall, Jorge I. Núñez, Marc Postman, Eric Quirico, Alyssa R. Rhoden, Anna M. Simpson, Paul Schenk, Michael F. Skrutskie, Andrew J. Steffl, Henry Throop
Figure caption: Density of NH-observable TNOs (contours and blue/gray background) detectable with Subaru/HSC expected from the OSSOS++ model. Gray circles show HSC search fields for each year 2020–2023A. The solid line indicates the location of the ecliptic plane, while the dashed line indicates the invariable plane at 45 au. The red circle marks the location of the bright star π − Sgr, which creates a zone of avoidance. Yellow circles show locations of Subaru-discovered TNOs that were either subsequently observed by (in 2020–2021) or potentially observable by the NH-LORRI instrument. In each panel, the black points show the discoveries made with observations of that year. The 2023A HSC deep search field, centered at (R.A., decl.) = (289.1, −20.36), went ∼0.5 mag deeper than searches before 2022B, and some TNOs that were near bright stars then had moved into clearer sky in 2023A. These 2023A data have been used for linkages to earlier detections, and the search for new targets is ongoing.
Paper: Candidate Distant Trans-Neptunian Objects Detected by the New Horizons Subaru TNO Survey
Authors: Wesley C. Fraser, Simon B. Porter, Lowell Peltier, JJ Kavelaars, Anne J. Verbiscer, Marc W. Buie, S. Alan Stern, John R. Spencer, Susan D. Benecchi, Tsuyoshi Terai, Takashi Ito, Fumi Yoshida, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, Stephen D. J. Gwyn, Hayden Smotherman, Sebastien Fabbro, Kelsi N. Singer, Amanda M. Alexander, Ko Arimatsu, Maria E. Banks, Veronica J. Bray, Mohamed Ramy El-Maarry, Chelsea L. Ferrell, Tetsuharu Fuse, Florian Glass, Timothy R. Holt, Peng Hong, Ryo Ishimaru, Perianne E. Johnson, Tod R. Lauer, Rodrigo Leiva, Patryk S. Lykawka, Raphael Marschall, Jorge I. Núñez, Marc Postman, Eric Quirico, Alyssa R. Rhoden, Anna M. Simpson, Paul Schenk, Michael F. Skrutskie, Andrew J. Steffl, Henry Throop
Figure caption: The bandpasses of the g, r2, i2, and EB-gri filters currently in use with the HSC.
Paper: Radar Circular Polarization Ratio of Near-Earth Asteroids: Links to Spectral Taxonomy and Surface Processes
Authors: Edgard G. Rivera-Valentín, Betzaida Aponte-Hernández, Patrick A. Taylor, Michael C. Nolan, Ellen S. Howell, Dany Waller, Luisa F. Zambrano-Marín, Anne K. Virkki, Ronald-Louis Ballouz, Angela M. Stickle
Figure caption: Comparison of the PDFs for NEAs with a < 1 au and Q < 1.5 au (i.e., close in) and NEAs with a > 2.5 au and Q > 3.9 au (i.e., further out). Each population is denoted by color following the legend, within which N is the total number of objects used to form the PDF. The filled-in space is the 1σ uncertainty envelope. Transparency was added to facilitate viewing of the PDFs simultaneously.
Paper: Radar Circular Polarization Ratio of Near-Earth Asteroids: Links to Spectral Taxonomy and Surface Processes
Authors: Edgard G. Rivera-Valentín, Betzaida Aponte-Hernández, Patrick A. Taylor, Michael C. Nolan, Ellen S. Howell, Dany Waller, Luisa F. Zambrano-Marín, Anne K. Virkki, Ronald-Louis Ballouz, Angela M. Stickle
Figure caption: The standard deviation of CPR as a function of (a) semimajor axis, as well as (b) aphelion and (c) perihelion distance. Each colored point represents an iteration over a constant number of bins, following the color bar. The black dashed line denotes the standard deviation of the entire data set for reference.
Paper: Tour of Asteroids for Characterization Observations (TACO): A Planetary Defense Asteroid Tour Concept
Authors: Angela M. Stickle, Andrew S. Rivkin, Justin Atchison, Jodi Berdis, Rylie Bull, Andy Cheng, R. Terik Daly, Carolyn M. Ernst, Patrick King, Meagan Leary, Emma S. G. Rainey, Ronald J. Vervack, Nancy Chabot
Figure caption: Time period where imaging requirements are met for a variety of flyby close approach distances and velocities. The time includes both inbound and outbound imaging opportunities. (Top) Analysis if the NAC is on a gimbal. The duration is relatively consistent even to low flyby distances, suggesting that closest approach could be tailored by the target without losing observing data or set from other constraints. (Bottom) No-gimbal case. The TACO tour includes flybys at a 10–20 km s−1 range, which limit observation time at the required pixel scale.
Paper: Tour of Asteroids for Characterization Observations (TACO): A Planetary Defense Asteroid Tour Concept
Authors: Angela M. Stickle, Andrew S. Rivkin, Justin Atchison, Jodi Berdis, Rylie Bull, Andy Cheng, R. Terik Daly, Carolyn M. Ernst, Patrick King, Meagan Leary, Emma S. G. Rainey, Ronald J. Vervack, Nancy Chabot
Figure caption: Concept diagram of the OpGrav concept.
Paper: Tour of Asteroids for Characterization Observations (TACO): A Planetary Defense Asteroid Tour Concept
Authors: Angela M. Stickle, Andrew S. Rivkin, Justin Atchison, Jodi Berdis, Rylie Bull, Andy Cheng, R. Terik Daly, Carolyn M. Ernst, Patrick King, Meagan Leary, Emma S. G. Rainey, Ronald J. Vervack, Nancy Chabot
Figure caption: Sample TACO trajectory, plotted in the Sun–Earth rotating frame. Earth lies on the Y  R  = 0 line near X  R  = 1.0 au. The numbers correspond to the flyby events listed in Table 2. This plot illustrates the changes in inclination required to fly by each pair of targets.
Paper: Tour of Asteroids for Characterization Observations (TACO): A Planetary Defense Asteroid Tour Concept
Authors: Angela M. Stickle, Andrew S. Rivkin, Justin Atchison, Jodi Berdis, Rylie Bull, Andy Cheng, R. Terik Daly, Carolyn M. Ernst, Patrick King, Meagan Leary, Emma S. G. Rainey, Ronald J. Vervack, Nancy Chabot
Figure caption: Sample TACO trajectory, plotted in the Earth mean ecliptic heliocentric inertial frame. The numbers 1–13 correspond to the events listed in Table 2.
Paper: Tour of Asteroids for Characterization Observations (TACO): A Planetary Defense Asteroid Tour Concept
Authors: Angela M. Stickle, Andrew S. Rivkin, Justin Atchison, Jodi Berdis, Rylie Bull, Andy Cheng, R. Terik Daly, Carolyn M. Ernst, Patrick King, Meagan Leary, Emma S. G. Rainey, Ronald J. Vervack, Nancy Chabot
Figure caption: Important measurements and properties of interest for three main planetary defense mitigation techniques. The PD tour mission measurements would be relevant for all three potential deflection missions.
Paper: Numerical Investigation of the Cohesive Strength Regime of the Bilobated Arrokoth after the Sky-crater-forming Impact Event
Authors: Yaeji Kim, Masatoshi Hirabayashi, James Bauer
Figure caption: Sky-impact-induced velocity imparted to Arrokoth’s small lobe (SL). The linear momentum derived from the π-scaling law is converted into the impulse velocity experienced by the small lobe, based on the conservation of linear momentum (see Equation (8)). The green, red, and blue lines correspond to impactor velocities of 100 m s−1, 300 m s−1, and 1 km s−1, respectively. The bulk densities of both the target and impactor are varied between 250 and 500 kg m−3. The cohesive strength in the π-scaling law is set to 5 kPa, exceeding all critical cohesive strengths at equilibrium. Higher object density results in slower impulse velocity owing to the increased mass. The direction of the impulse velocity (normal to the surface) and the applied area (highlighted in wine color) on the Arrokoth shape model are illustrated in the right panels.
Paper: Numerical Investigation of the Cohesive Strength Regime of the Bilobated Arrokoth after the Sky-crater-forming Impact Event
Authors: Yaeji Kim, Masatoshi Hirabayashi, James Bauer
Figure caption: The critical cohesive strength of Arrokoth at the equilibrium state (Y *). The equilibrium state refers to the condition where Arrokoth is influenced solely by its self-gravity and rotational forces. The stress fields, computed using FEM simulation based on Arrokoth’s current spin period of 16 hr and a bulk density of 500 kg m−3, are converted to critical cohesive strength using the Drucker−Prager criterion (see Equation (15)). The critical cohesive strength around the neck region is less than 3 kPa, while the entire structure, including the surface, never reaches 5 kPa.
Paper: Numerical Investigation of the Cohesive Strength Regime of the Bilobated Arrokoth after the Sky-crater-forming Impact Event
Authors: Yaeji Kim, Masatoshi Hirabayashi, James Bauer
Figure caption: Critical cohesive strength in Arrokoth at equilibrium state (Y *). The critical cohesive strength at a surface and a cross section of Arrokoth are shown in the left and right panels, respectively. Panel (a) shows the simulation result with the high-resolution mesh, while panel (b) is for the reduced-resolution mesh, which is used for the major simulations in this study.
Paper: Water Generation on the Moon from Solar Wind and Meteoroid Impacts
Authors: Brant M. Jones, Juan Diego Carrillo-Sánchez, Diego Janches, Menelaos Sarantos, Thomas M. Orlando
Figure caption: Pictorial summary of the overall kinetic scheme. The center inset depicts the concentration for each section of the interior grain color-coded for clarity. Green represents the surface with low hydroxyl concentration; yellow represents the subsurface having the highest concentration, with the dashed line signifying the penetration depth; and red represents the bulk. Removal of hydroxyls at the surface coupled with enhanced diffusion in the subsurface creates a chemical gradient that preferentially drives chemistry toward the surface and limits transport into the bulk. (I) Pristine metal oxide lattice network of a regolith grain. (II) Solar wind protons are implanted below the subsurface at approximately 22 nm depth, resulting in the formation of subsurface metal hydroxyl (M–OH) and an unsatisfied bond on the metal cation, M ∗. (III) The hydroxyl sites and protons will then diffuse to the surface and bulk. (IV) Surficial M–OH and M* sites from diffusion of original H defect. (V) Solar wind oxygen ions will implant as well, resulting in a subsurface peroxide defect labeled as M–O–O–M. (VI) Similar to hydrogen, these defects can diffuse to the surface and into the bulk. The surface will then contain an unsatisfied oxygen bond. (VII) Further implantation and diffusion of protons will react with some of these surficial oxygen sites. (VIII) At some critical surface density defined by the local temperature (solar heating or IM), neighboring surficial M–OH sites will react, resulting in gas-phase water. The process is repeated indefinitely while lunar grains are exposed to solar wind.
Paper: Water Generation on the Moon from Solar Wind and Meteoroid Impacts
Authors: Brant M. Jones, Juan Diego Carrillo-Sánchez, Diego Janches, Menelaos Sarantos, Thomas M. Orlando
Figure caption: Cumulative distributions, in g cm−2 s−1, of (a) meteoroid mass impact and (b) production rates of IM over the mass range considered by the MIF and averaged over a full lunar cycle for the four meteoroid populations: the JFCs (blue), the MBAs (green), the HTCs (purple), the OCCs (orange), and the overall flux (black). The dashed–dotted gray line in panel (b) shows the cumulative melting rates estimated by Cintala (1992) at the Moon. The bottom panels (panels (c) and (d)) represent the mass histograms of the mass influx rates (panel (c)) and the melting rates (panel (d)) per mass decade over the mass range considered by the MIF—that is, masses are represented in logarithmic scale in panels (c) and (d), and the width of each mass bin corresponds to a ratio of 10 between two consecutive mass delimiters and partitioned into the four meteoroid populations. The percentages on the top represent the contribution of each meteoroid population to the overall meteoroid mass influx (panel (c)) and the total melting rates (panel (d)) in each mass range; additionally, the colors of the top bars illustrate what is the dominant meteoroid population in that mass range.
Paper: Water Generation on the Moon from Solar Wind and Meteoroid Impacts
Authors: Brant M. Jones, Juan Diego Carrillo-Sánchez, Diego Janches, Menelaos Sarantos, Thomas M. Orlando
Figure caption: Variability of mass influxes of meteoroid impacts, in g cm−2 s−1, as a function of the selenographic longitude and latitude determined by the MIF for JFCs (panels (a) and (b)), ASTs (panels (c) and (d)), HTCs (panels (e) and (f)), and OOCs (panels (g) and (h)) and two Moon phases: new moon (Day 0; left panels) and third quarter (Day 22; right panels). Note that the color scales are different for each meteoroid population, and the corresponding fluxes are plotted over an elevation map of the Moon centered on the prime meridian. The vertical black lines represent the positions of the antihelion (LT = 0 hr, nightside), apex (LT = 6 hr, dawn terminator), and helion (LT = 12 hr, noon side) directions.
Paper: Water Generation on the Moon from Solar Wind and Meteoroid Impacts
Authors: Brant M. Jones, Juan Diego Carrillo-Sánchez, Diego Janches, Menelaos Sarantos, Thomas M. Orlando
Figure caption: Mass influxes of meteoroids, in g cm−2 s−1, as a function of the selenographic latitude and the impact velocity, averaged over a lunar cycle for the (a) JFCs, (b) MBAs, (c) HTCs, (d) OCCs, and (e) total flux. Panel (f) shows the average mass input as a function of the impact velocity over a lunar month for the JFCs (blue line), ASTs (green line), HTCs (purple line), OCCs (orange line), and total (black line), along with the corresponding mass influxes in new moon (dotted lines) and full moon (dashed lines).
Paper: Water Generation on the Moon from Solar Wind and Meteoroid Impacts
Authors: Brant M. Jones, Juan Diego Carrillo-Sánchez, Diego Janches, Menelaos Sarantos, Thomas M. Orlando
Figure caption: Melting production rates, in g cm−2 s−1, as a function of the selenographic latitude and the impact velocity, averaged over a lunar cycle for the (a) JFCs, (b) MBAs, (c) HTCs, (d) OCCs, and (e) total flux. Panel (f) shows the average melting rates (solid lines) as a function of the impact velocity over a lunar month for the JFCs (blue line), the ASTs (green line), the HTCs (purple line), the OCCs (orange line), and the total (black line), along with the corresponding melting rates in new moon (dotted lines) and full moon (dashed lines).
Paper: Water Generation on the Moon from Solar Wind and Meteoroid Impacts
Authors: Brant M. Jones, Juan Diego Carrillo-Sánchez, Diego Janches, Menelaos Sarantos, Thomas M. Orlando
Figure caption: Peak water production rates as a function of time from RD and from meteoroid IM assuming different diffusion activation energies for -OH and -O. The ratio of peak production rates is displayed in panel (c). These cases document the effect of diffusion activation energies on overall water production. For higher energies, diffusion to the surface is limited, resulting in less water production from RD and more from IM. In addition, the higher energies result in a significant delay in the generation of water from RD, as a longer time is needed for surficial hydroxyls to reach the necessary surface density where RD is activated.
Paper: Water Generation on the Moon from Solar Wind and Meteoroid Impacts
Authors: Brant M. Jones, Juan Diego Carrillo-Sánchez, Diego Janches, Menelaos Sarantos, Thomas M. Orlando
Figure caption: Variability of total melting rates produced by meteoroid impacts, in g cm−2 s−1, as a function of the selenographic longitude and latitude determined by the MIF for four Moon phases: new moon (Day 0; panel (a)), first quarter (Day 8; panel (b)), full moon (Day 15; panel (c)), and third quarter (Day 22; panel (d)). Note that the corresponding fluxes are plotted over an elevation map of the Moon centered on the prime meridian. The vertical black lines represent the positions of the antihelion (LT = 0 hr, nightside), apex (LT = 6 hr, dawn terminator), and helion (LT = 12 hr, noon side) directions.