adsabs/AstroCLIMB huggingface dataset:
Paper: Plume Activity on Europa: Current Knowledge and Search Strategy for Europa Clipper
Authors: Lorenz Roth, Erin Leonard, Kelly Miller, Matt Hedman, Lynnae C. Quick, Tracy M. Becker, Shawn Brooks, Corey Cochrane, Ashley Gerard Davies, Carolyn M. Ernst, Cyril Grima, Candice J. Hansen, Carly Howett, Sean Hsu, Xianzhe Jia, Adrienn Luspay-Kuti, Margaret Kivelson, Fabian Klenner, Alfred McEwen, William B. McKinnon, Robert T. Pappalardo, Frank Postberg, Julie Rathbun, Kurt D. Retherford, Kirk Scanlan, K. Marshall Seaton, John R. Spencer, J. Hunter Waite, Paul Withers, Danielle Wyrick, Mikhail Yu. Zolotov
Figure caption: (a) Search for surface changes with Galileo (left) and JunoCam (right) images. White arrows highlight differences in ridges attributed to increased emission angles in the JunoCam images. The black arrow highlights a difference attributed to varied photometric phase functions. (b) Processed JunoCam limb image for high contrast shows no anomalies along the limb (both from C. J. Hansen et al. 2024).
Paper: The NASA Exoplanet Archive and Exoplanet Follow-up Observing Program: Data, Tools, and Usage
Authors: Jessie L. Christiansen, Douglas L. McElroy, Marcy Harbut, David R. Ciardi, Megan Crane, John Good, Kevin K. Hardegree-Ullman, Aurora Y. Kesseli, Michael B. Lund, Meca Lynn, Ananda Muthiar, Ricky Nilsson, Toba Oluyide, Michael Papin, Amalia Rivera, Melanie Swain, Nicholas D. Susemiehl, Raymond Tam, Julian van Eyken, Charles Beichman
Figure caption: A screenshot of the interactive table plotting tool, which is accessible from the top menu bar of each interactive table (Section 3.1). Users can select x- and y-values from a subset of the (typically numerical) columns in the originating table and also select additional columns to control the size and color of the plotted values. The plots are available in a range of color palettes and a set of themes (light, dark, and presentation, shown here). Additional functionality includes zooming, panning, and downloading the final plot. Individual points can be hovered over for a brief summary of the plotted data and clicked on to be taken straight to the overview page for that object.
Paper: The NASA Exoplanet Archive and Exoplanet Follow-up Observing Program: Data, Tools, and Usage
Authors: Jessie L. Christiansen, Douglas L. McElroy, Marcy Harbut, David R. Ciardi, Megan Crane, John Good, Kevin K. Hardegree-Ullman, Aurora Y. Kesseli, Michael B. Lund, Meca Lynn, Ananda Muthiar, Ricky Nilsson, Toba Oluyide, Michael Papin, Amalia Rivera, Melanie Swain, Nicholas D. Susemiehl, Raymond Tam, Julian van Eyken, Charles Beichman
Figure caption: An example air-mass plot provided with the results of the Transit and Ephemeris Service (Section 3.3). The plot shows the altitude/air mass of an object as it rises and sets over the course of a night, with any predicted transits highlighted in pink and the 1σ uncertainty on the predicted transit midpoint time shown in green. This example shows the visibility of the transit of HAT-P-63 b as seen from Palomar Observatory on the night of 2025 May 22.
Paper: Classifying and Characterizing the Evolution of the Minimum Orbit Intersection Distance for Near-Earth Asteroids
Authors: Shoucun Hu, Yuanyuan Chen, Xinran Li, Xiuhai Wang, Xuefeng Wang
Figure caption: The left panel shows the 200 yr MOID evolution of six selected PHAs. Δt = t − t0 is the time elapsed since the initial epoch t0 (2025 January 1). The right panel depicts the maximal amplitude of short-period variation of the MOID as a function of the semimajor axis. The objects that have close encounters with Venus, Earth, Mars and Jupiter are marked in different colors. The six PHAs in the left panel are also labeled (with asterisks) in the right panel.
Paper: Classifying and Characterizing the Evolution of the Minimum Orbit Intersection Distance for Near-Earth Asteroids
Authors: Shoucun Hu, Yuanyuan Chen, Xinran Li, Xiuhai Wang, Xuefeng Wang
Figure caption: The left panel depicts the fitting results of the MOID variations for eight selected NEAs. The solid lines represent the precise values, while the dashed lines illustrate the linear fits. The right panel depicts the corresponding migration of the critical points projected on the x−z plane in the migration frame. The asterisks indicate the initial position of the points, and the red plus symbol represents the origin of the frame (which is the position of the critical point related to the EMB’s orbit).
Paper: Classifying and Characterizing the Evolution of the Minimum Orbit Intersection Distance for Near-Earth Asteroids
Authors: Shoucun Hu, Yuanyuan Chen, Xinran Li, Xiuhai Wang, Xuefeng Wang
Figure caption: The 200 day backward propagation of the dE (left panel) and dB (right panel) of nine NEAs that impacted Earth shortly after discovery are illustrated. Δt = 0 corresponds to the moment of impact. The reference distances of 1 R⊕ and one lunar distance are indicated by dotted and dashed lines, respectively.
Paper: Classifying and Characterizing the Evolution of the Minimum Orbit Intersection Distance for Near-Earth Asteroids
Authors: Shoucun Hu, Yuanyuan Chen, Xinran Li, Xiuhai Wang, Xuefeng Wang
Figure caption: Illustration of the MOID evolution classification scheme using the two-digit MEI metric m.n, with the m value defined based on d1 and the n value on d2–d1. The cataloged NEAs are classified and plotted in black within their respective grid cells, with the PHAs distinctly highlighted in red.
Paper: Classifying and Characterizing the Evolution of the Minimum Orbit Intersection Distance for Near-Earth Asteroids
Authors: Shoucun Hu, Yuanyuan Chen, Xinran Li, Xiuhai Wang, Xuefeng Wang
Figure caption: The lines show the variations of gravitational acceleration (normalized by the Sun’s gravity) with heliodistance for the six planets. The blue dots illustrate the distribution of semimajor axis vs. eccentricity of the NEAs.
Paper: Classifying and Characterizing the Evolution of the Minimum Orbit Intersection Distance for Near-Earth Asteroids
Authors: Shoucun Hu, Yuanyuan Chen, Xinran Li, Xiuhai Wang, Xuefeng Wang
Figure caption: The left panel shows the variations of the difference between dE and dB within 1 yr for 50 selected NEAs whose orbits were computed using the two-body model. The right panel depicts the discrepancy in dB between two models utilized to compute the EMB’s orbit for the 50 NEAs: one employs a two-body model, while the other is derived from the DE441 ephemeris.
Paper: Classifying and Characterizing the Evolution of the Minimum Orbit Intersection Distance for Near-Earth Asteroids
Authors: Shoucun Hu, Yuanyuan Chen, Xinran Li, Xiuhai Wang, Xuefeng Wang
Figure caption: MOID propagations (panels in the left column), migration of the critical points (panels in the middle column), and evolution of orbital configurations (panels in the right column) for the four selected NEAs. For the case of 2006 DL and 2001 FR85, the MOID is assigned to be negative after orbit crossing. The asterisks in the middle panels indicate the initial position of the critical points, while the red plus symbol represents the origin of the frame. The orbits of the EMB and the asteroids are represented in blue and orange, respectively. Additionally, the critical points along both orbits are illustrated with asterisks. All the measurements of the MOID and orbit coordinates are in au.
Paper: Classifying and Characterizing the Evolution of the Minimum Orbit Intersection Distance for Near-Earth Asteroids
Authors: Shoucun Hu, Yuanyuan Chen, Xinran Li, Xiuhai Wang, Xuefeng Wang
Figure caption: Fitting results of the MOID variations (left) and the corresponding critical points migration in the x−z plane (right) for asteroids 2002 CB19 and 2023 HV2. In the left panel, the solid lines represent the precise values, while the dotted lines illustrate the signed MOID and the dashed lines demonstrate the fits of the signed MOID. The reference frame and symbols used in the right panel are identical to those employed in Figure 6.
Paper: Classifying and Characterizing the Evolution of the Minimum Orbit Intersection Distance for Near-Earth Asteroids
Authors: Shoucun Hu, Yuanyuan Chen, Xinran Li, Xiuhai Wang, Xuefeng Wang
Figure caption: The left panel depicts the MOID evolution of three asteroids exhibiting multiple orbital crossings. The vertical coordinates are the signed MOIDs defined according to G. F. Gronchi & C. Tardioli (2013). The events of Earth flyby and orbit crossing are noted for 1999 AN10. The right panel illustrates the ω − q distribution (argument of perihelion vs. perihelion distance) for objects categorized according to their crossing numbers.
Paper: Classifying and Characterizing the Evolution of the Minimum Orbit Intersection Distance for Near-Earth Asteroids
Authors: Shoucun Hu, Yuanyuan Chen, Xinran Li, Xiuhai Wang, Xuefeng Wang
Figure caption: Distribution of the critical points at the initial epoch t0 for the NEAs, projected in the x−z (left; divided into four quadrants) and x−y (right) planes of the migration frame, with the origin marked with a red plus symbol (the correspondent critical points along the EMB orbit). In the left panel, the asteroids with different orbital types are represented by different colors. The two asymptotes described in the text, represented by the blue dotted line, are illustrated in the right panel.
Paper: Classifying and Characterizing the Evolution of the Minimum Orbit Intersection Distance for Near-Earth Asteroids
Authors: Shoucun Hu, Yuanyuan Chen, Xinran Li, Xiuhai Wang, Xuefeng Wang
Figure caption: Comparative analysis of MOID fitting performance for two asteroids, 1979 XB (left panel) and 2024 LU1 (right panel), using the two different methods. The blue solid line represents the precise MOID values computed through orbit integration using the full-force dynamical model, while the blue dashed line illustrates the fitting results obtained through our direct fitting approach. For comparison, the red solid line denotes the MOID values calculated using G. F. Gronchi & C. Tardioli’s (2013) double-averaged method, with the corresponding fitting results shown as red dashed lines.
Paper: Classifying and Characterizing the Evolution of the Minimum Orbit Intersection Distance for Near-Earth Asteroids
Authors: Shoucun Hu, Yuanyuan Chen, Xinran Li, Xiuhai Wang, Xuefeng Wang
Figure caption: Illustration of the defined critical point migration frame. The light blue and red spheres represent the EMB (which is the origin of the coordinate system) and the asteroid position associated with the minimum distance d. In the case of a circular EMB orbit, the asteroid is situated within the x−z plane (the angle ϕ is also illustrated).
Paper: Classifying and Characterizing the Evolution of the Minimum Orbit Intersection Distance for Near-Earth Asteroids
Authors: Shoucun Hu, Yuanyuan Chen, Xinran Li, Xiuhai Wang, Xuefeng Wang
Figure caption: Distribution of ϕ vs. i for the four types of NEAs exhibiting a single crossing within the 200 yr period. The parameter values are adopted at the initial epoch, with points in different ranges of ω highlighted in distinct colors.
Paper: Classifying and Characterizing the Evolution of the Minimum Orbit Intersection Distance for Near-Earth Asteroids
Authors: Shoucun Hu, Yuanyuan Chen, Xinran Li, Xiuhai Wang, Xuefeng Wang
Figure caption: Comparison of MOID evolution (solid curves) and the linear approximations (dashed lines) for 16 selected NEAs spanning η values from 0.005 to 2. The sign inversion strategy is applied to asteroids 253841, 451124, and 2002 GJ8 yet reveals significant discrepancies (η > 0.3) in the latter two cases.
Paper: Classifying and Characterizing the Evolution of the Minimum Orbit Intersection Distance for Near-Earth Asteroids
Authors: Shoucun Hu, Yuanyuan Chen, Xinran Li, Xiuhai Wang, Xuefeng Wang
Figure caption: Variations of ϕ for the eight asteroids in Figure 6 and the two asteroids in Figure 7.
Paper: A New Saturn Model of Ionospheric Transport and Electrodynamics (SMITE)
Authors: Omakshi Agiwal, Luke Moore, Carlos Martinis, Ingo Mueller-Wodarg, J.D. Huba
Figure caption: The normalized TEC distribution is shown as latitude–altitude contours for six iterations of the SMITE Model 1 run. (a) The basic model, which only includes photochemistry (including the scaled H2 vibrational reaction) and plasma motion in the presence of a field-aligned grid, (b) the basic model with equatorial inflow, (c) the basic model with ring shadow, (d) the basic model with field-aligned ion–neutral-wind-driven plasma transport, (e) the basic model without the H2 vibrational reaction included, and (f) the baseline model, which is the basic model with equatorial inflow, ring shadowing, and neutral winds included. Each panel also has an additional panel directly below the TEC contours, which shows the normalized TEC latitudinal line profile at dawn and dusk.
Paper: A New Saturn Model of Ionospheric Transport and Electrodynamics (SMITE)
Authors: Omakshi Agiwal, Luke Moore, Carlos Martinis, Ingo Mueller-Wodarg, J.D. Huba
Figure caption: Saturn’s neutral upper atmospheres modeled by STIM at a single longitude are shown. (a) The altitude variations of the dominant neutral species are shown using solid colored lines. Neutral species other than H2O vary primarily in altitude, with negligible changes with latitude, local time, and Saturnian season. The dashed blue line shows the modified H2O density profile implemented in SMITE. Panel (b) shows the latitudinal profile of the H2O influx used by STIM, which serves as a proxy for the equatorial inflow of magnetospheric material. Finally, the altitudinal variation of the (c)–(e) neutral temperature Tn, (f)–(h) meridional winds Uθ, and (i)–(k) zonal winds Uϕ are shown for STIM runs during (left column) southern hemisphere summer, (middle column) equinox, and (right column) northern hemisphere summer conditions. Panels (c)–(e) each show Tn using black lines at latitudes of −26° (dotted), 0° (solid), and 26° (dashed), corresponding to the peak solar illumination latitude for southern hemisphere summer, equinox, and northern hemisphere summer, respectively. Panels (f)–(k) show a red–blue (negative–positive) contour map, indicating the magnitude of the winds. The zonal winds are defined as positive eastward (blue), and meridional winds as positive northward (blue).
Paper: A New Saturn Model of Ionospheric Transport and Electrodynamics (SMITE)
Authors: Omakshi Agiwal, Luke Moore, Carlos Martinis, Ingo Mueller-Wodarg, J.D. Huba
Figure caption: The normalized, field-perpendicular drift velocity at the magnetic equator, vD, is shown as a function of local time for three different electrodynamic drift patterns (Drifts 1, 2, and 3 shown by green, purple, and yellow lines, respectively). For each drift pattern, two iterations exist, corresponding to whether the peak drift velocity is oriented upward (positive, solid line) or downward (negative, dashed line) in altitude on the “dayside” (between 7 hr and 19 hr local time). (a) Drift 1 is a sinusoidal drift, and the “up” version is the default SAMI2 analytical drift at Earth, (b) Drift 2 is constant with local time, and (c) Drift 3 varies diurnally in magnitude but not direction.
Paper: A New Saturn Model of Ionospheric Transport and Electrodynamics (SMITE)
Authors: Omakshi Agiwal, Luke Moore, Carlos Martinis, Ingo Mueller-Wodarg, J.D. Huba
Figure caption: Various cross sections of the electron densities, ne, from the SMITE Model 1 baseline run (see Table 2) are shown in panels (a)–(c). Panel (a) shows ne at local noon in latitude–altitude space, panel (b) shows the evolution of the ∼1500 km altitude level at all latitudes over one Saturn rotation (24 hr local time, but ∼10.6 hr UT), and panel (c) shows the altitude variation in ne as a function of local time at 0° latitude, where the altitudes shown are not in Saturn’s ring shadow. Also shown are SMITE Model 1 baseline run altitude profiles of (d) densities and (e) temperatures for electron (solid black line) and dominant ions (solid colored lines). The profiles are at 18 hr local time and 0° latitude, where the ionosphere is modified by ring-shadow-driven interhemispheric transport at altitudes between ∼1500 km and 3500 km.
Paper: A New Saturn Model of Ionospheric Transport and Electrodynamics (SMITE)
Authors: Omakshi Agiwal, Luke Moore, Carlos Martinis, Ingo Mueller-Wodarg, J.D. Huba
Figure caption: An illustration showing a meridional view of Saturn and the SMITE modeled ionosphere in a cylindrical ρ−Z coordinate system. The SMITE modeled ionospheric electron densities, ne, are projected onto the 2D dipole magnetic field model grid. Gray isocontours indicate Saturn’s empirically constrained internally generated quadrupole magnetic field. The SMITE grid intersects the location of Saturn’s D, C, and B rings, indicated by brown slabs, in the rotational plane. However, the rings are not included as a source/sink of magnetospheric neutrals and plasma in the current version of SMITE. The SMITE ionosphere shown is extracted at 12 hr local time, modeled using a subsolar latitude of ∼2° (near equinox), and is shaped by the following dynamics: photochemistry; equatorial inflow of magnetospheric material, shown by the dashed blue curve, where the flux peaks at the equator and decreases with increasing ∣z∣; the ring shadow, indicated by the black region on Saturn; the neutral winds, shown by brown arrows indicating the expected flow of the meridional winds; and equatorial electrodynamics, shown by red arrows depicting a terrestrial-like E × B plasma drift at local noon.
Paper: A New Saturn Model of Ionospheric Transport and Electrodynamics (SMITE)
Authors: Omakshi Agiwal, Luke Moore, Carlos Martinis, Ingo Mueller-Wodarg, J.D. Huba
Figure caption: The plasma drift motion imposed in SMITE to treat the field-parallel and field-perpendicular motion of plasma in response to an east–west electric field are shown at local noon, assuming an upward drift in altitude on the dayside. (a) The magnetic-field-parallel motion ﹩{v}_{E\times {B}_{\parallel }}﹩ is zero at the magnetic equator and diverges away from this center point, resulting in the downward (in altitude) motion of plasma along the planetary field at all latitudes and altitudes. The intensity of the drift is largest near the magnetic equator and falls off with latitude. The normalized plasma velocities in (a) are positive in the field-aligned direction. (b) The magnetic-field-perpendicular motion ﹩{v}_{E\times {B}_{\perp }}﹩ maximizes at the magnetic equator, where the east–west electric field is directly perpendicular to the north–south magnetic field, and decreases with latitude. The normalized plasma velocities in (b) are positive in the direction of increasing altitude.
Paper: A New Saturn Model of Ionospheric Transport and Electrodynamics (SMITE)
Authors: Omakshi Agiwal, Luke Moore, Carlos Martinis, Ingo Mueller-Wodarg, J.D. Huba
Figure caption: Electron density altitude profiles for the SMITE Model 1 iterations from Figure 5 are shown at (a) 6 hr and (b) 18 hr local times. The basic model is shown as a solid gray line, and the iterations are shown as dashed lines: with equatorial inflow (blue), with ring shadow (yellow), with neutral winds (red), and without the H﹩{}_{2}^{+}﹩ vibrational reaction (brown). The baseline model is shown as a solid black line. Additionally, a “1D model” is shown by a dotted gray line, which effectively excludes the detailed 2D treatment of diffusive field-aligned plasma transport from the basic model run.
Paper: A JWST Study of the Remarkable Oort Cloud Comet C/2017 K2 (PanSTARRS)
Authors: Charles E. Woodward, Dominique Bockélee-Morvan, David E. Harker, Michael S. P. Kelley, Nathan X. Roth, Diane H. Wooden, Stefanie N. Milam
Figure caption: The tile positions of 1﹩\mathop{.}\limits^{^{\prime\prime} }﹩0-diameter circular aperture beams used to study the spatial distribution of coma emission from the 2.9–27.9 μm JWST spectra of comet C/20217 K2 (PanSTARRS) derived from NIRSpec and MRS s3d data cubes. The background is the wavelength-collapsed MRS Ch1 MEDIUM(B) s3d data cube (arbitrary lognormal scaling); the direction of the Sun vector is indicated for the date of the MRS observations, MJD 2459812 (2022 August 21 UT). North is up, and east is to the left.
Paper: A JWST Study of the Remarkable Oort Cloud Comet C/2017 K2 (PanSTARRS)
Authors: Charles E. Woodward, Dominique Bockélee-Morvan, David E. Harker, Michael S. P. Kelley, Nathan X. Roth, Diane H. Wooden, Stefanie N. Milam
Figure caption: (a) Radial surface brightness profiles (solid lines) for six selected wavelength ranges targeting the spectral continuum. Wavelength range and best-fit power-law slope (k; dashed lines) are as indicated. The bottom three profiles are based on the NIRSpec data, and the remaining profiles are based on the MRS data. The profiles are offset for clarity. (b) Model radial profiles for the MRS and a monochromatic wavelength of 5.55 μm. Three models are provided: a pure point source (PSF), a pure coma with a radial surface brightness profile equivalent to that observed at 5.4–5.7 μm (coma), and a combined coma and nucleus model, based on a nucleus-to-coma ratio of 30/70 within a 1″-diameter aperture. The profiles are offset for clarity.
Paper: A JWST Study of the Remarkable Oort Cloud Comet C/2017 K2 (PanSTARRS)
Authors: Charles E. Woodward, Dominique Bockélee-Morvan, David E. Harker, Michael S. P. Kelley, Nathan X. Roth, Diane H. Wooden, Stefanie N. Milam
Figure caption: The spatial distribution of the 4.9–28.0 μm SEDs of comet C/2017 K2 (PanSTARRS) obtained on 2022-08-21TT14:42:00 (JWST MRS observation date) when the comet was at a heliocentric distance rh =  2.35 au and Δ =  2.02 au in 1﹩\mathop{.}\limits^{^{\prime\prime} }﹩0-diameter circular beams that tile the coma (see Section 2). Tiles indicating no data are places in the beam grid where the MRS Ch1 SHORT(A) cube had no valid data. The center of the beam grid is a beam placed on the approximate centroid position of the peak in the surface brightness of the comet (as measured in all the channels drilled) as given in Figure 1. The 1﹩\mathop{.}\limits^{^{\prime\prime} }﹩0-diameter beam accounts for the values of PIX_SAR variations in each channel.
Paper: A JWST Study of the Remarkable Oort Cloud Comet C/2017 K2 (PanSTARRS)
Authors: Charles E. Woodward, Dominique Bockélee-Morvan, David E. Harker, Michael S. P. Kelley, Nathan X. Roth, Diane H. Wooden, Stefanie N. Milam
Figure caption: Upper-limit nucleus models (dashed, dashed–dotted, and dotted lines) compared to the combined NIRSpec and MRS spectrum (solid line). The 5–7 μm range provides the strongest constraint on the model nucleus radius (R) for our assumed IR beaming parameter values (η).
Paper: A JWST Study of the Remarkable Oort Cloud Comet C/2017 K2 (PanSTARRS)
Authors: Charles E. Woodward, Dominique Bockélee-Morvan, David E. Harker, Michael S. P. Kelley, Nathan X. Roth, Diane H. Wooden, Stefanie N. Milam
Figure caption: The composite 2.9–27.9 μm JWST spectrum of comet C/20217 K2 (PanSTARRS) derived from drilling the NIRSpec and MRS s3d data cubes using a 1﹩\mathop{.}\limits^{^{\prime\prime} }﹩0-diameter circular aperture centered on the comet photocenter (position 0:0, see Figure 1) along their wavelength dimension (hence a cylinder in the s3d data cube space) on MJD 2459812 (2022 August 21 UT).