adsabs/AstroCLIMB huggingface dataset:
Paper: System Architecture and Planetary Obliquity: Implications for Long-term Habitability
Authors: Pam Vervoort, Jonathan Horner, Stephen R. Kane, Sandra Kirtland Turner, James B. Gilmore
Figure caption: Maximum eccentricity and mean angular momentum deficit. (a) The maximum eccentricity of an Earth-like planet under different planetary architectures, i.e., with a Jupiter-like planet having different initial semimajor axes and eccentricities. (b) The percentage of deviation in the angular momentum (AMD) relative to that of a circular orbit, calculated as the mean deviation across the 10 Myr integration time. Blue colors indicate AMDs less than the modern Earth, below 0.0477%. The red circle is the current position of Jupiter in our solar system.
Paper: System Architecture and Planetary Obliquity: Implications for Long-term Habitability
Authors: Pam Vervoort, Jonathan Horner, Stephen R. Kane, Sandra Kirtland Turner, James B. Gilmore
Figure caption: The period of the main obliquity cycle of an Earth-like planet plotted on a logarithmic scale, under different planetary architectures, i.e., with a Jupiter-like planet having different initial semimajor axes and eccentricities. The red circle indicates the current position of Jupiter in our solar system.
Paper: Lyα Escape from Low-mass, Compact, High-redshift Galaxies
Authors: Ragadeepika Pucha, Naveen A. Reddy, Arjun Dey, Stéphanie Juneau, Kyoung-Soo Lee, Moire K. M. Prescott, Irene Shivaei, Sungryong Hong
Figure caption: Image cutouts (10″ × 10″) of zLAEs in BW, IA445, R, I, F110W, F139M, and F160W (left to right). The green circles denote the apertures used for performing photometry. 1 of 3 images
Paper: Lyα Escape from Low-mass, Compact, High-redshift Galaxies
Authors: Ragadeepika Pucha, Naveen A. Reddy, Arjun Dey, Stéphanie Juneau, Kyoung-Soo Lee, Moire K. M. Prescott, Irene Shivaei, Sungryong Hong
Figure caption: Image cutouts (10″ × 10″) of pLAEs in BW, IA445, R, I, F110W, F139M, and F160W (left to right). The green circles denote the apertures used for performing photometry. 1 of 4 images
Paper: A Deep and Wide Twilight Survey for Asteroids Interior to Earth and Venus
Authors: Scott S. Sheppard, David J. Tholen, Petr Pokorný, Marco Micheli, Ian Dell'Antonio, Shenming Fu, Chadwick A. Trujillo, Rachael Beaton, Scott Carlsten, Alex Drlica-Wagner, Clara Martínez-Vázquez, Sidney Mau, Toni Santana-Ros, Luidhy Santana-Silva, Cristóbal Sifón, Sunil Simha, Audrey Thirouin, David Trilling, A. Katherina Vivas, Alfredo Zenteno
Figure caption: Known NEOs plotted with semimajor axis vs. eccentricity. The new discoveries from this survey are shown by big blue circles. The yellow area shows the region near Venus’ orbit that dynamcially stable low-eccentricity Venus co-orbitals would be expected to be found, where no asteroid is known. All known asteroids with semimajor axes similar to Venus are on dynamically unstable, highly eccentric orbits that cross Earth’s orbit (small green circles). Atira-type object orbits remain interior to Earth’s orbit, shown as red circles to the left of the vertical dashed line starting at 1 au, which is the inner edge of the Earth crossing zone.
Paper: A Deep and Wide Twilight Survey for Asteroids Interior to Earth and Venus
Authors: Scott S. Sheppard, David J. Tholen, Petr Pokorný, Marco Micheli, Ian Dell'Antonio, Shenming Fu, Chadwick A. Trujillo, Rachael Beaton, Scott Carlsten, Alex Drlica-Wagner, Clara Martínez-Vázquez, Sidney Mau, Toni Santana-Ros, Luidhy Santana-Silva, Cristóbal Sifón, Sunil Simha, Audrey Thirouin, David Trilling, A. Katherina Vivas, Alfredo Zenteno
Figure caption: Same as Figure 1 but using inclination.
Paper: ARMADA. II. Further Detections of Inner Companions to Intermediate-mass Binaries with Microarcsecond Astrometry at CHARA and VLTI
Authors: Tyler Gardner, John D. Monnier, Francis C. Fekel, Jean-Baptiste Le Bouquin, Adam Scovera, Gail Schaefer, Stefan Kraus, Fred C. Adams, Narsireddy Anugu, Jean-Philippe Berger, Theo Ten Brummelaar, Claire L. Davies, Jacob Ennis, Douglas R. Gies, Keith J. C. Johnson, Pierre Kervella, Kaitlin M. Kratter, Aaron Labdon, Cyprien Lanthermann, Johannes Sahlmann, Benjamin R. Setterholm
Figure caption: We show our ARMADA epochs along with published WDS data for the binary systems that do not have any new RV data. The orbital coverage is quite poor for HD 196089 and HD 48581. This is especially true for HD 48581, where we present the first guess at the orbital elements. Due to its long-period and high-amplitude “wobble” orbit, the shape of the outer orbit is visually distorted for HD 185762. We show the best-fit orbit for two revolutions of the orbital period in order to match up in time with the early WDS data and our recent ARMADA epochs. The gray shaded regions depict 100 random orbits from the MCMC chains, for one orbital revolution.
Paper: ARMADA. II. Further Detections of Inner Companions to Intermediate-mass Binaries with Microarcsecond Astrometry at CHARA and VLTI
Authors: Tyler Gardner, John D. Monnier, Francis C. Fekel, Jean-Baptiste Le Bouquin, Adam Scovera, Gail Schaefer, Stefan Kraus, Fred C. Adams, Narsireddy Anugu, Jean-Philippe Berger, Theo Ten Brummelaar, Claire L. Davies, Jacob Ennis, Douglas R. Gies, Keith J. C. Johnson, Pierre Kervella, Kaitlin M. Kratter, Aaron Labdon, Cyprien Lanthermann, Johannes Sahlmann, Benjamin R. Setterholm
Figure caption: Our residuals to the pure binary fit are high for the systems in Figure 11, and we see a clear peak in the period search for inner companions. In HD 196089 and HD 48581, the “wobble” amount is relatively small at <200 μas. For HD 185762, our best-fit wobble is >10 mas, and the period search is aided by including historical data from WDS for the long-period “wobble” motion.
Paper: ARMADA. II. Further Detections of Inner Companions to Intermediate-mass Binaries with Microarcsecond Astrometry at CHARA and VLTI
Authors: Tyler Gardner, John D. Monnier, Francis C. Fekel, Jean-Baptiste Le Bouquin, Adam Scovera, Gail Schaefer, Stefan Kraus, Fred C. Adams, Narsireddy Anugu, Jean-Philippe Berger, Theo Ten Brummelaar, Claire L. Davies, Jacob Ennis, Douglas R. Gies, Keith J. C. Johnson, Pierre Kervella, Kaitlin M. Kratter, Aaron Labdon, Cyprien Lanthermann, Johannes Sahlmann, Benjamin R. Setterholm
Figure caption: We plot the best-fit inner orbits due to the newly detected companions from wobble motion, after subtracting out the outer binary motion shown in Figure 11. For HD 48581 we plot the two convincing period peaks in the periodogram, though the solution at 4.8 days is preferred. We see a median residual ≤30 μas in these newly detected systems, though further information is required to solve for individual masses in these cases. This can be accomplished with RV monitoring, a better outer orbit, or a better distance from future Gaia releases. The gray shaded regions show that inner orbit errors are higher in cases that do not have any RV data or flux detected from the inner companion.
Paper: ARMADA. II. Further Detections of Inner Companions to Intermediate-mass Binaries with Microarcsecond Astrometry at CHARA and VLTI
Authors: Tyler Gardner, John D. Monnier, Francis C. Fekel, Jean-Baptiste Le Bouquin, Adam Scovera, Gail Schaefer, Stefan Kraus, Fred C. Adams, Narsireddy Anugu, Jean-Philippe Berger, Theo Ten Brummelaar, Claire L. Davies, Jacob Ennis, Douglas R. Gies, Keith J. C. Johnson, Pierre Kervella, Kaitlin M. Kratter, Aaron Labdon, Cyprien Lanthermann, Johannes Sahlmann, Benjamin R. Setterholm
Figure caption: We plot the best-fit inner orbits due to the newly detected companions for the systems in Figure 7. In these cases we see the flux from both inner components, so we plot the motion of each one around its center of mass. The median residuals to the orbit fits are a bit higher for HD 1976 and HD 220278, which are likely due to higher measurement uncertainties on low-flux inner companions. In the case of HD 220278, there is likely a fourth component in the system that has a yet-unconstrained orbit. The gray shaded regions depict 100 random orbits from the MCMC chains, though for HD 1976 we only show the MCMC orbits for the inner component for clarity since the two orbits overlap.
Paper: ARMADA. II. Further Detections of Inner Companions to Intermediate-mass Binaries with Microarcsecond Astrometry at CHARA and VLTI
Authors: Tyler Gardner, John D. Monnier, Francis C. Fekel, Jean-Baptiste Le Bouquin, Adam Scovera, Gail Schaefer, Stefan Kraus, Fred C. Adams, Narsireddy Anugu, Jean-Philippe Berger, Theo Ten Brummelaar, Claire L. Davies, Jacob Ennis, Douglas R. Gies, Keith J. C. Johnson, Pierre Kervella, Kaitlin M. Kratter, Aaron Labdon, Cyprien Lanthermann, Johannes Sahlmann, Benjamin R. Setterholm
Figure caption: We show the outer binary orbits for systems where we directly detect the flux from inner visual components in our interferometric data. We combine our new high-precision ARMADA epochs with historical speckle data published in WDS. We show the final fitted outer orbit, taking into account the “wobbles” from newly detected companions in these systems. In the case of HD 220278, the “wobble” from its newly detected companion is at the 10 mas level, which makes it extremely obvious even at the wide scale.
Paper: ARMADA. II. Further Detections of Inner Companions to Intermediate-mass Binaries with Microarcsecond Astrometry at CHARA and VLTI
Authors: Tyler Gardner, John D. Monnier, Francis C. Fekel, Jean-Baptiste Le Bouquin, Adam Scovera, Gail Schaefer, Stefan Kraus, Fred C. Adams, Narsireddy Anugu, Jean-Philippe Berger, Theo Ten Brummelaar, Claire L. Davies, Jacob Ennis, Douglas R. Gies, Keith J. C. Johnson, Pierre Kervella, Kaitlin M. Kratter, Aaron Labdon, Cyprien Lanthermann, Johannes Sahlmann, Benjamin R. Setterholm
Figure caption: After our initial guess at the best-fit outer orbit, we search for additional astrometric companions on a grid over inner orbital period for the systems in Figure 7. These systems all show rather obvious inner orbital periods, with HD 1976 being confirmed with RV data to be on the correct peak. HD 220278 is a new detection, with a long period and large “wobble” amplitude.
Paper: ARMADA. II. Further Detections of Inner Companions to Intermediate-mass Binaries with Microarcsecond Astrometry at CHARA and VLTI
Authors: Tyler Gardner, John D. Monnier, Francis C. Fekel, Jean-Baptiste Le Bouquin, Adam Scovera, Gail Schaefer, Stefan Kraus, Fred C. Adams, Narsireddy Anugu, Jean-Philippe Berger, Theo Ten Brummelaar, Claire L. Davies, Jacob Ennis, Douglas R. Gies, Keith J. C. Johnson, Pierre Kervella, Kaitlin M. Kratter, Aaron Labdon, Cyprien Lanthermann, Johannes Sahlmann, Benjamin R. Setterholm
Figure caption: Left: we combined published RV data from McSwain et al. (2007), Abt et al. (1990), and Blaauw & van Albada (1963) with five new epochs taken at Fairborn Observatory. The single-line RV curve is noisy here, due to the wide and blended profiles of this B-type system. Middle and right: we combined our new astrometry of HD 173093 with the triple RV orbit from Horch et al. (2021). For the Aa,Ab orbit, we subtract the long-period motion, and we subtract the Aa,Ab short-period motion to plot the long-period variation for A+B.
Paper: ARMADA. II. Further Detections of Inner Companions to Intermediate-mass Binaries with Microarcsecond Astrometry at CHARA and VLTI
Authors: Tyler Gardner, John D. Monnier, Francis C. Fekel, Jean-Baptiste Le Bouquin, Adam Scovera, Gail Schaefer, Stefan Kraus, Fred C. Adams, Narsireddy Anugu, Jean-Philippe Berger, Theo Ten Brummelaar, Claire L. Davies, Jacob Ennis, Douglas R. Gies, Keith J. C. Johnson, Pierre Kervella, Kaitlin M. Kratter, Aaron Labdon, Cyprien Lanthermann, Johannes Sahlmann, Benjamin R. Setterholm
Figure caption: Unlike GRAVITY, which calibrates to an absolute wavelength scale, our MIRC-X data rely on an internally consistent wavelength calibration scheme. Therefore, we need to fit for an extra scale factor when combining MIRC-X+GRAVITY data sets. We show the “wobble” fit for GRAVITY data alone (left), MIRC-X data alone (middle), and the combined data with a fitted scale factor of 1.00495 ± 0.00017 between the instruments (right). In all cases, the inner orbit does not change significantly.
Paper: ARMADA. II. Further Detections of Inner Companions to Intermediate-mass Binaries with Microarcsecond Astrometry at CHARA and VLTI
Authors: Tyler Gardner, John D. Monnier, Francis C. Fekel, Jean-Baptiste Le Bouquin, Adam Scovera, Gail Schaefer, Stefan Kraus, Fred C. Adams, Narsireddy Anugu, Jean-Philippe Berger, Theo Ten Brummelaar, Claire L. Davies, Jacob Ennis, Douglas R. Gies, Keith J. C. Johnson, Pierre Kervella, Kaitlin M. Kratter, Aaron Labdon, Cyprien Lanthermann, Johannes Sahlmann, Benjamin R. Setterholm
Figure caption: Same as Figure 5, but for HD 29573. We show the fit to the inner companion with GRAVITY alone (left), MIRC-X alone (middle), and the combined fit with a fitted scale factor of 1.00505 (right). This value agrees well with that obtained on HD 199766.
Paper: Galactic Chemical Evolution of Exoplanet Hosting Stars: Are High-mass Planetary Systems Young?
Authors: C. Swastik, Ravinder K. Banyal, Mayank Narang, P. Manoj, T. Sivarani, S. P. Rajaguru, Athira Unni, Bihan Banerjee
Figure caption: Observed trends for α-element abundances of host stars and planet mass for the HARPS-GTO, CKS, and CPS samples. The colors red, yellow, and blue represent small planets, giant planets, and super-Jupiters, respectively. The black line shows the Huber regression fit, and the gray shaded region represents the 95th percentile confidence interval. The slope value for the best-fit line is shown in each panel. The last row is the arithmetic mean of the α-element abundance from the above four rows.
Paper: Galactic Chemical Evolution of Exoplanet Hosting Stars: Are High-mass Planetary Systems Young?
Authors: C. Swastik, Ravinder K. Banyal, Mayank Narang, P. Manoj, T. Sivarani, S. P. Rajaguru, Athira Unni, Bihan Banerjee
Figure caption: Host star chemical abundances for iron-peak (Mn, Cr, and Ni) elements and metallicity ([Fe/H]) as a function of planet mass for the HARPS-GTO, CKS, and CPS samples. Symbols and colors are the same as in Figure 5.
Paper: Galactic Chemical Evolution of Exoplanet Hosting Stars: Are High-mass Planetary Systems Young?
Authors: C. Swastik, Ravinder K. Banyal, Mayank Narang, P. Manoj, T. Sivarani, S. P. Rajaguru, Athira Unni, Bihan Banerjee
Figure caption: Exoplanet host stars from the HARPS-GTO (red), CPS (blue), and CKS (yellow) surveys. The dashed black line separates the main-sequence stars lying below the line from the evolved stars lying above (Brewer & Fischer 2018). In this paper, we study only the main-sequence stars.
Paper: Galactic Chemical Evolution of Exoplanet Hosting Stars: Are High-mass Planetary Systems Young?
Authors: C. Swastik, Ravinder K. Banyal, Mayank Narang, P. Manoj, T. Sivarani, S. P. Rajaguru, Athira Unni, Bihan Banerjee
Figure caption: Top row: host star chemical abundances for light s-process elements as a function of planet mass for the HARPS-GTO sample. Middle row: host star chemical abundances for heavy s-process elements as a function of planet mass for the HARPS-GTO sample. The color scheme is the same as that in Figure 5. Bottom row: light s-process element (Y) abundances as a function of planet mass for the HARPS-GTO, CKS, and CPS samples.
Paper: Galactic Chemical Evolution of Exoplanet Hosting Stars: Are High-mass Planetary Systems Young?
Authors: C. Swastik, Ravinder K. Banyal, Mayank Narang, P. Manoj, T. Sivarani, S. P. Rajaguru, Athira Unni, Bihan Banerjee
Figure caption: Metallicity distribution for the HARPS-GTO, CKS, and CPS samples. The colors red, yellow, and blue represent small planets, giant planets, and super-Jupiters, respectively. The vertical lines represent the mean of the distribution.
Paper: Galactic Chemical Evolution of Exoplanet Hosting Stars: Are High-mass Planetary Systems Young?
Authors: C. Swastik, Ravinder K. Banyal, Mayank Narang, P. Manoj, T. Sivarani, S. P. Rajaguru, Athira Unni, Bihan Banerjee
Figure caption: Distribution of planet mass and semimajor axis (on log scale) for the RV and transit planets used in this study. Corresponding histograms are also shown in the top and right panels.
Paper: Galactic Chemical Evolution of Exoplanet Hosting Stars: Are High-mass Planetary Systems Young?
Authors: C. Swastik, Ravinder K. Banyal, Mayank Narang, P. Manoj, T. Sivarani, S. P. Rajaguru, Athira Unni, Bihan Banerjee
Figure caption: Stellar abundances for iron-peak elements (Co, Cu and Zn) as a function of planet mass exclusively for the HARPS-GTO sample. The Co, Cu, and Zn abundances were not available for the CKS and CPS samples. Once again, the color scheme and the black line representation are the same as in Figure 5.
Paper: Galactic Chemical Evolution of Exoplanet Hosting Stars: Are High-mass Planetary Systems Young?
Authors: C. Swastik, Ravinder K. Banyal, Mayank Narang, P. Manoj, T. Sivarani, S. P. Rajaguru, Athira Unni, Bihan Banerjee
Figure caption: Top row: comparison of elemental abundances of Fe, Mg, and Mn for stars that are common between the CPS and HARPS-GTO samples. Bottom row: comparison of Fe, Mg, and Mn abundance for stars that are common between the CPS and CKS samples. The solid red curve represents the x = y line.
Paper: Galactic Chemical Evolution of Exoplanet Hosting Stars: Are High-mass Planetary Systems Young?
Authors: C. Swastik, Ravinder K. Banyal, Mayank Narang, P. Manoj, T. Sivarani, S. P. Rajaguru, Athira Unni, Bihan Banerjee
Figure caption: Variation of Eu abundance (r-process element) as a function of planet mass for the HARPS-GTO sample. The color scheme is the same as that in Figure 5.
Paper: Galactic Chemical Evolution of Exoplanet Hosting Stars: Are High-mass Planetary Systems Young?
Authors: C. Swastik, Ravinder K. Banyal, Mayank Narang, P. Manoj, T. Sivarani, S. P. Rajaguru, Athira Unni, Bihan Banerjee
Figure caption:  α-element abundances as a function of planet mass for the multiplanetary systems that host at least one planet each in low-mass and Jupiter- and/or super-Jupiter-mass regimes. The last row is the arithmetic mean of the α-element abundance from the above four rows.
Paper: Galactic Chemical Evolution of Exoplanet Hosting Stars: Are High-mass Planetary Systems Young?
Authors: C. Swastik, Ravinder K. Banyal, Mayank Narang, P. Manoj, T. Sivarani, S. P. Rajaguru, Athira Unni, Bihan Banerjee
Figure caption: Abundance ratios [X/Fe] vs. [Fe/H] for iron-peak elements for stars belonging to all three samples: HARPS-GTO, CKS, and CPS. The blue circles represent SWPs, while the color bar represents stars hosting planets of different mass.
Paper: Galactic Chemical Evolution of Exoplanet Hosting Stars: Are High-mass Planetary Systems Young?
Authors: C. Swastik, Ravinder K. Banyal, Mayank Narang, P. Manoj, T. Sivarani, S. P. Rajaguru, Athira Unni, Bihan Banerjee
Figure caption: The distribution of numerical slope (between α-element abundances of host star and planet mass) generated from Monte Carlo simulations for the HARPS-GTO, CKS, and CPS samples. The solid black line represents the mean of the distribution, and the dotted color lines represent the measured slope from Figure 5.
Paper: Galactic Chemical Evolution of Exoplanet Hosting Stars: Are High-mass Planetary Systems Young?
Authors: C. Swastik, Ravinder K. Banyal, Mayank Narang, P. Manoj, T. Sivarani, S. P. Rajaguru, Athira Unni, Bihan Banerjee
Figure caption: Heat map of 1σ scatter from Figures 5 and 6 for the abundance dispersion of the host stars of small planets, Jupiters, and super-Jupiters. A linear detrending was applied to the original abundance data to compute the 1σ scatter for each mass bin.
Paper: Galactic Chemical Evolution of Exoplanet Hosting Stars: Are High-mass Planetary Systems Young?
Authors: C. Swastik, Ravinder K. Banyal, Mayank Narang, P. Manoj, T. Sivarani, S. P. Rajaguru, Athira Unni, Bihan Banerjee
Figure caption: Abundance ratios [X/Fe] vs. [Fe/H] for heavy elements (A > 30) for stars belonging to all three samples: HARPS-GTO, CKS, and CPS. The blue circles represent SWPs, while the color bar represents stars hosting planets of different mass.
Paper: Galactic Chemical Evolution of Exoplanet Hosting Stars: Are High-mass Planetary Systems Young?
Authors: C. Swastik, Ravinder K. Banyal, Mayank Narang, P. Manoj, T. Sivarani, S. P. Rajaguru, Athira Unni, Bihan Banerjee
Figure caption: Abundance ratios [X/Fe] vs. [Fe/H] for α-elements for stars belonging to all three samples: HARPS-GTO, CKS, and CPS. The blue circles represent SWPs, while the color bar represents stars hosting planets of different mass.
Paper: Galactic Chemical Evolution of Exoplanet Hosting Stars: Are High-mass Planetary Systems Young?
Authors: C. Swastik, Ravinder K. Banyal, Mayank Narang, P. Manoj, T. Sivarani, S. P. Rajaguru, Athira Unni, Bihan Banerjee
Figure caption: Left: the observed distribution of exoplanet mass (in log scale) taken from the NASA exoplanet archive. Right: a uniform distribution assumed for α-element abundances of PHSs.
Paper: Galactic Chemical Evolution of Exoplanet Hosting Stars: Are High-mass Planetary Systems Young?
Authors: C. Swastik, Ravinder K. Banyal, Mayank Narang, P. Manoj, T. Sivarani, S. P. Rajaguru, Athira Unni, Bihan Banerjee
Figure caption: Age distribution of PHSs derived using isochrone fitting. The vertical lines represent the median for each of the distributions.
Paper: The Von Zeipel–Lidov–Kozai Effect inside Mean Motion Resonances with Applications to Trans-Neptunian Objects
Authors: Hanlun Lei, Jian Li, Xiumin Huang, Muzi Li
Figure caption: Time histories of the critical argument σ = 5λ − 2λ 8 − 3ϖ and argument of perihelion ω for the orbits of 2018 VO137 numerically propagated under the full N-body model (left panel) and the semi-secular model (right panel). The portions in circulation are shaded. The results produced in the semi-secular model agree well with the ones under the full N-body model. In simulations, the initial epoch is fixed on 2020 December 17. Under the full N-body model, the initial state of 2018 VO137 is provided by the osculating elements a = 55.381 au, e = 0.184, I = 39.°0, Ω = 42.°7, ω = 135.°599997, and M = 234.°799997 (refer to https://minorplanetcenter.net to retrieve the elements). Under the semi-secular model, the initial state of 2018 VO137 is provided by the associated averaged elements, which are given in Table 2.
Paper: Orbital Characterization of Superbolides Observed from Space: Dynamical Association with Near-Earth Objects, Meteoroid Streams, and Identification of Hyperbolic Meteoroids
Authors: Eloy Peña-Asensio, Josep M. Trigo-Rodríguez, Albert Rimola
Figure caption: Tensile strength as a function of the Tisserand parameter for the CNEOS events. The radii of the circles are arbitrarily scaled with the diameter of the object. Impacts corresponding to the asteroid 2022 EB5, 2019 MO, 2018 LA, the Chelyabinsk event, and the first interstellar meteoroid are annotated.
Paper: The Von Zeipel–Lidov–Kozai Effect inside Mean Motion Resonances with Applications to Trans-Neptunian Objects
Authors: Hanlun Lei, Jian Li, Xiumin Huang, Muzi Li
Figure caption: Definition of the adiabatic invariant, S, corresponding to the area surrounded by isolines of the resonant Hamiltonian in the phase space (σ, Σ) for the case of 2:5 resonance (holding symmetric libration centers). The left panel is for the resonant case (i.e., ﹩{ \mathcal H }\gt {{ \mathcal H }}_{U}﹩) and the right panel is for the circulation case (i.e., ﹩{ \mathcal H }\lt {{ \mathcal H }}_{U}﹩). In both panels, the dynamical separatrices with ﹩{ \mathcal H }={{ \mathcal H }}_{U}﹩ are shown by red dashed lines.
Paper: Orbital Characterization of Superbolides Observed from Space: Dynamical Association with Near-Earth Objects, Meteoroid Streams, and Identification of Hyperbolic Meteoroids
Authors: Eloy Peña-Asensio, Josep M. Trigo-Rodríguez, Albert Rimola
Figure caption: Variation of associations by criterion and events with association when modifying the threshold of the criteria by ±25%. The number of associations by criterion are presented stacked; however, they do have multiples overlapping.