adsabs/AstroCLIMB huggingface dataset:
Paper: Can Neptune’s Distant Mean Motion Resonances Constrain Undiscovered Planets in the Solar System? Lessons from a Case Study of the 9:1 Resonance
Authors: Matthew W. Porter, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, 省文 林, Fred C. Adams
Figure caption: Initial distribution of orbital elements resulting from the generation process. Note that while these distributions result from the case of no additional perturber, the perturber had no effect on these distributions over 10 Myr. Also note that these distributions are not the same as those given in Table 1, since all objects which did not librate in the 9:1 for at least 10 Myr were discarded.
Paper: New Polarimetric Data for the Galilean Satellites: Io and Ganymede Observations and Modeling
Authors: Nikolai Kiselev, Vera Rosenbush, Ari Leppälä, Karri Muinonen, Ludmilla Kolokolova, Aleksandr Savushkin, Nikolai Karpov
Figure caption: The phase-angle dependence of polarization for Io in the UBVRI bands obtained from observations carried out during 2018–2023 (black symbols). The data obtained by Rosenbush & Kiselev (2005; red symbols) and Kiselev et al. (2009; green symbols) are also displayed. The open circles denote data related to the leading hemisphere of the satellite (longitude L < 180°), and the filled circles, respectively, to the trailing one (longitude L > 180°). The fit shown by the solid curve consists of two parts derived within the range of phase angles from 0° to ∼2° using the inverse polynomial of the third degree and within the range of approximately 2°–11.°8 using the linear polynomial.
Paper: New Polarimetric Data for the Galilean Satellites: Io and Ganymede Observations and Modeling
Authors: Nikolai Kiselev, Vera Rosenbush, Ari Leppälä, Karri Muinonen, Ludmilla Kolokolova, Aleksandr Savushkin, Nikolai Karpov
Figure caption: The phase-angle dependence of polarization for Ganymede in the UBVRI bands obtained from observations carried out during 2019–2023 (black symbols). For comparison, the available data of similar accuracy derived by Rosenbush & Kiselev (2005) and Kiselev et al. (2009) are also shown by the red and green symbols, respectively. The open circles denote data related to the leading hemisphere of the satellite (longitude L < 180°), and the filled circles, respectively, to the trailing one (longitude L > 180°). The fit shown by the solid curve consists of two parts derived within the range of phase angles from 0° to ∼2° and in the range from ∼2° to 11.°8, using polynomials with different exponents.
Paper: New Polarimetric Data for the Galilean Satellites: Io and Ganymede Observations and Modeling
Authors: Nikolai Kiselev, Vera Rosenbush, Ari Leppälä, Karri Muinonen, Ludmilla Kolokolova, Aleksandr Savushkin, Nikolai Karpov
Figure caption: The longitude dependence of polarization for Io in the VRI bands after taking into account the correction for the linear phase-angle dependence of the polarization in the range of phase angles of ∼4°–11.°8. The fits to the data, according to the expression P(L) = P 1 + P 2 sin(L–L  o ), are shown by a solid curve.
Paper: New Polarimetric Data for the Galilean Satellites: Io and Ganymede Observations and Modeling
Authors: Nikolai Kiselev, Vera Rosenbush, Ari Leppälä, Karri Muinonen, Ludmilla Kolokolova, Aleksandr Savushkin, Nikolai Karpov
Figure caption: The longitude dependence of polarization for Ganymede in the VRI bands after taking into account the correction for the phase-angle dependence of polarization in the range of phase angles from ∼2° to 11.°8. The fits to the data performed according to the expression P(L) = P 1 + P 2 sin(L–L  o ) are shown by the solid curves.
Paper: New Polarimetric Data for the Galilean Satellites: Io and Ganymede Observations and Modeling
Authors: Nikolai Kiselev, Vera Rosenbush, Ari Leppälä, Karri Muinonen, Ludmilla Kolokolova, Aleksandr Savushkin, Nikolai Karpov
Figure caption: Shifting the inversion point with the increase of kl, in comparison to observations obtained with the V (on the left) and R (on the right) filters.
Paper: New Polarimetric Data for the Galilean Satellites: Io and Ganymede Observations and Modeling
Authors: Nikolai Kiselev, Vera Rosenbush, Ari Leppälä, Karri Muinonen, Ludmilla Kolokolova, Aleksandr Savushkin, Nikolai Karpov
Figure caption: Modeled degree of polarization for Io in the V (left) and R (right) bands.
Paper: The Effect of Salinity on Ocean Circulation and Ice–Ocean Interaction on Enceladus
Authors: Yaoxuan Zeng, Malte F. Jansen
Figure caption: (a) Zonal mean surface heat flux and (b) zonally and vertically integrated meridional ocean heat transport (see Appendix B.1 for details) in the quasi-equilibrium state of all simulations. The first to fourth columns show the results of the high-salinity simulation with high horizontal diffusivity (HS h ), the high-salinity simulation with low horizontal diffusivity (HS l ), the low-salinity simulation with high horizontal diffusivity (LS h ), and the low-salinity simulation with low horizontal diffusivity (LS l ), respectively. In (a), the black dashed line is the bottom heating (Q  b ), the blue line is the latent heating (Q LH), the red line is the conductive heat loss (Q cond), and the black solid line is the surface ocean-to-ice heat flux (Q oi). In (b), the blue line is the diffusive heat flux (F Dif), the red line is the advective heat flux (F Adv), and the black line is the total heat flux (F  Q ).
Paper: The Effect of Salinity on Ocean Circulation and Ice–Ocean Interaction on Enceladus
Authors: Yaoxuan Zeng, Malte F. Jansen
Figure caption: Simulation with the same parameters as in HS h , but with the zonal width of the domain extended from 15° to 360°. (a) Zonal mean zonal velocity u. (b) Stream function Ψ, with clockwise circulation defined as positive. (c) Surface heat budget, where the black dashed line is the bottom heating (Q  b ), the blue line is the latent heating (Q LH), the red line is the conductive heat loss (Q cond), and the black solid line is the surface ocean-to-ice heat flux (Q oi). (d) Zonal mean temperature T (the contour interval is 0.01 °C below –2.14 °C and 0.001 °C above −2.14 °C). (e) Zonal mean salinity S (a reference salinity of 34.97 g kg−1 is subtracted, and the contour interval is 10−3 g kg−1). (f) Zonally and vertically integrated meridional ocean heat transport. The blue line is the diffusive heat flux (F Dif), the red line is the advective heat flux (F Adv), and the black line is the total heat flux (F  Q ). Note that the color bar range in (b) and the vertical axis range in (f) are multiplied by 24 compared to Figure 4(b1) and Figure 5(b1) to account for the larger zonal width of the domain and allow for easier comparison.
Paper: The Effect of Salinity on Ocean Circulation and Ice–Ocean Interaction on Enceladus
Authors: Yaoxuan Zeng, Malte F. Jansen
Figure caption: Simulation with parameters in HS h , but including surface temperature variation and a temperature-dependent heat diffusion coefficient of the ice when prescribing the conductive heat loss (following Kang et al. 2022c). (a) Zonal mean zonal velocity u. (b) Stream function Ψ, with clockwise circulation defined as positive. (c) Surface heat budget, where the black dashed line is the bottom heating (Q  b ), the blue line is the latent heating (Q LH), the red line is the conductive heat loss (Q cond), and the black solid line is the surface ocean-to-ice heat flux (Q oi). (d) Zonal mean temperature T (the contour interval is 0.01 °C below −2.14 °C and 0.001 °C above −2.14 °C). (e) Zonal mean salinity S (a reference salinity of 34.97 g kg−1 is subtracted, and the contour interval is 10−3 g kg−1). (f) Zonal mean potential density ρ  σ  (a reference density of 1029.13 kg m−3 is subtracted, and the contour interval is 10−3 kg m−3 below 5 × 10−3 kg m−3 and 3 × 10−4 kg m−3 above 5 × 10−3 kg m−3).
Paper: The Effect of Salinity on Ocean Circulation and Ice–Ocean Interaction on Enceladus
Authors: Yaoxuan Zeng, Malte F. Jansen
Figure caption: Meridional temperature gradient ∂T/(r∂ϕ) in the quasi-equilibrium state of all simulations. The first to fourth columns show the results of the high-salinity simulation with high horizontal diffusivity (HS h ), the high-salinity simulation with low horizontal diffusivity (HS l ), the low-salinity simulation with high horizontal diffusivity (LS h ), and the low-salinity simulation with low horizontal diffusivity (LS l ), respectively. The black dashed lines indicate the tangent cylinder.
Paper: The Effect of Salinity on Ocean Circulation and Ice–Ocean Interaction on Enceladus
Authors: Yaoxuan Zeng, Malte F. Jansen
Figure caption: Temporal variability in the high-salinity simulation with low horizontal diffusivity (HS l ). (a) Zonal mean latent heating; (b) zonal mean surface temperature; (c) zonal mean surface salinity (a reference salinity of 34.97 g kg−1 is subtracted); (d) zonal mean surface density (a reference density of 1029.13 kg m−3 is subtracted); and (e) stream function at r = 225.375 km as a function of time and latitude. The black dashed lines are the latitudes where the tangent cylinder intersects the ocean surface in (a)–(d) and the latitudes where the tangent cylinder intersects r = 225.375 km in (e). The first 4000 yr average is used as the quasi-equilibrium state of the simulation HS l .
Paper: The Effect of Salinity on Ocean Circulation and Ice–Ocean Interaction on Enceladus
Authors: Yaoxuan Zeng, Malte F. Jansen
Figure caption: Vertical heat fluxes near the surface of the ocean (the uppermost ocean model layer in contact with the ice shell). The blue lines show the radial diffusive heat flux (including the parameterized convective heat flux) at the bottom of the surface ocean model layer, and the black line shows the ocean heat flux to the ice shell (Q oi). The thinner lines are the raw data and the thicker lines are moving averages of nine grids to smooth grid-scale variabilities. The first to fourth columns show the results of the high-salinity simulation with high horizontal diffusivity (HS h ), the high-salinity simulation with low horizontal diffusivity (HS l ), the low-salinity simulation with high horizontal diffusivity (LS h ), and the low-salinity simulation with low horizontal diffusivity (LS l ), respectively.
Paper: The Effect of Salinity on Ocean Circulation and Ice–Ocean Interaction on Enceladus
Authors: Yaoxuan Zeng, Malte F. Jansen
Figure caption: Snapshots of meridional eddy velocity ﹩v^{\prime} ﹩ (deviations from time and zonal mean) in all simulations at r = 225.375 km. The first to fourth columns show the results of the high-salinity simulation with high horizontal diffusivity (HS h ), the high-salinity simulation with low horizontal diffusivity (HS l ), the low-salinity simulation with high horizontal diffusivity (LS h ), and the low-salinity simulation with low horizontal diffusivity (LS l ), respectively. Note that the magnitude of ﹩v^{\prime} ﹩ in (a) is 104 times smaller than in (b)–(d).
Paper: The Effect of Salinity on Ocean Circulation and Ice–Ocean Interaction on Enceladus
Authors: Yaoxuan Zeng, Malte F. Jansen
Figure caption: Simulation with the same parameters as in HS l , but using the “mirrored” salinity field of the quasi-equilibrium state in HS l  as the initial condition. (a) Zonal mean latent heating; (b) zonal mean surface temperature; (c) zonal mean surface salinity (a reference salinity of 34.97 g kg−1 is subtracted); (d) zonal mean surface density (a reference density of 1029.13 kg m−3 is subtracted); and (e) stream function at r = 225.375 km as a function of time and latitude. The black dashed lines are the latitudes where the tangent cylinder intersects the ocean surface in (a)–(d) and the latitudes where the tangent cylinder intersects r = 225.375 km in (e).
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: Viewing geometry of Psyche at the time of observation for Matter et al. (2013), Sanchez et al. (2016), Landsman et al. (2018), and Flight 821. The shape model is from Viikinkoski et al. (2018) and was accessed using the Interactive Service for Asteroid Models.
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: Spectra from all sets with (left) and without (right) the equatorial surface features in Figure 1.
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: Same as Figure 8, but each emissivity spectrum has been divided by the average spectrum of all nights to isolate differences in rotation.
Paper: Can Neptune’s Distant Mean Motion Resonances Constrain Undiscovered Planets in the Solar System? Lessons from a Case Study of the 9:1 Resonance
Authors: Matthew W. Porter, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, 省文 林, Fred C. Adams
Figure caption: Left: computed eccentricity time derivative for a zero-inclination 9:1 resonator with q = 45 au, in the presence of a perturbing planet (m = 8.4 M ⊕, a = 400 au, q = 240 au, i = 16°, ω = 150°, Ω = 97°), as a function of ϖ. Right: computed contribution to the secular eccentricity time derivative for a 9:1 resonator with i = 5° from Neptune (black), and a zero-e, zero-i planet with a = 240 au. The computation was done using Equation (5). Note that the contribution to de/dt from this “Planet 9” is much higher than that from Neptune, even though both orbits are circular and coplanar. This is due to the much larger size of this planet’s orbit.
Paper: Can Neptune’s Distant Mean Motion Resonances Constrain Undiscovered Planets in the Solar System? Lessons from a Case Study of the 9:1 Resonance
Authors: Matthew W. Porter, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, 省文 林, Fred C. Adams
Figure caption: Illustration of the approximate, semi-analytic method for computing Δe during a precession through one of the de/dt peaks. Left: comparison of calculated eccentricity evolution (red curve) and N-body integration output (blue dots) over 150 Myr. Note that the perihelion distance ticks on the right side of this panel assume a = 130.1 au, which only holds while the object is still in resonance prior to t = 100 Myr. Right: illustration of the integrated portion of the de/dt curve; the object starts at ϖ = 225°, and exits resonance after 100 Myr at ϖ = 123°. The integral (Equation (6)) was performed assuming a constant ϖ precession rate that was obtained from the N-body integration.
Paper: Can Neptune’s Distant Mean Motion Resonances Constrain Undiscovered Planets in the Solar System? Lessons from a Case Study of the 9:1 Resonance
Authors: Matthew W. Porter, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, 省文 林, Fred C. Adams
Figure caption: Calculated characteristic perihelion deviation range (black bar) vs. actual perihelion change from N-body integration output (blue dots) for all integrated objects. Far left: control simulation. Center: m = 6.2 M ⊕, q = 240 au perturber, aggregated over all nine eccentricity–inclination combinations. Far right: m = 8.4 M ⊕, q = 240 au perturber, aggregated over all nine eccentricity–inclination combinations. Δq values were calculated using the e = 0.3, i = 16° planet for each m–q combination shown, with the process outlined in Section 5.
Paper: Can Neptune’s Distant Mean Motion Resonances Constrain Undiscovered Planets in the Solar System? Lessons from a Case Study of the 9:1 Resonance
Authors: Matthew W. Porter, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, 省文 林, Fred C. Adams
Figure caption: Heat maps showing how resonators occupy the (a, ϕ) parameter space during the the final 100 Myr of the simulations involving the 8.4 M ⊕ planets, in the case of (top left) no planet, (top right) q = 385 au, (bottom left) q = 300 au, and (bottom right) q = 240 au. For each case, we group the nine different eccentricity–inclination combinations together as one sample to reduce noise, as these parameters have less impact than q and mass. Note we only included objects with q < 50 au, to remove contamination from dynamically detached objects.
Paper: Can Neptune’s Distant Mean Motion Resonances Constrain Undiscovered Planets in the Solar System? Lessons from a Case Study of the 9:1 Resonance
Authors: Matthew W. Porter, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, 省文 林, Fred C. Adams
Figure caption: Perihelion evolution during the 100 Myr prior to exiting the interval 129.1 au < a < 131.1 au, for all interval-leaving objects in one of the control simulations (left), and in the simulation with the M = 8.4 M ⊕, q = 240 au, e = 0.3, i = 11° (right). Clear negative trends feature in both plots, illustrating that the ejected objects are those driven into the low-q scattering region. Far more objects leave resonance in the latter case, primarily because the perturber causes more objects to enter this unstable region.
Paper: Can Neptune’s Distant Mean Motion Resonances Constrain Undiscovered Planets in the Solar System? Lessons from a Case Study of the 9:1 Resonance
Authors: Matthew W. Porter, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, 省文 林, Fred C. Adams
Figure caption: Initial inclination of integrated objects vs. signed change in perihelion distance after 100 Myr. Left: control simulations. Right: m = 8.4 M ⊕ q = 240 au perturber, aggregated over all nine eccentricity–inclination combinations.
Paper: Can Neptune’s Distant Mean Motion Resonances Constrain Undiscovered Planets in the Solar System? Lessons from a Case Study of the 9:1 Resonance
Authors: Matthew W. Porter, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, 省文 林, Fred C. Adams
Figure caption: Left: computed de/dt curves for the central-value Planet 9 claimed by Brown & Batygin (2022) for four different resonances. For each resonance, a zero-inclination object with q = 45 au was used. Right: libration amplitudes and precession rates of the generated 9:1 resonators that we used to determine the appropriate mean precession rate to use when calculating Δq over the peaks in the curves shown in the left panel.
Paper: Can Neptune’s Distant Mean Motion Resonances Constrain Undiscovered Planets in the Solar System? Lessons from a Case Study of the 9:1 Resonance
Authors: Matthew W. Porter, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, 省文 林, Fred C. Adams
Figure caption: Deviation of perihelion distance from initial value for 1000 objects in one of the control simulations (left), and in the simulation with the m = 8.4 M ⊕, q = 240 au, e = 0.3, i = 11° perturber (right). Objects with semimajor axes within 1 au of the center of the 9:1 resonance at t = 100 Myr are colored in blue, while those with semimajor axes more than 1 au distant from the resonance center at this time are colored in orange. Perihelion distances diffuse much faster in the latter case due to the perturber.
Paper: Can Neptune’s Distant Mean Motion Resonances Constrain Undiscovered Planets in the Solar System? Lessons from a Case Study of the 9:1 Resonance
Authors: Matthew W. Porter, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, 省文 林, Fred C. Adams
Figure caption: Final semimajor axis and eccentricity of objects after 1 Gyr, for all 10,000 objects in the control simulation (left) and all 9000 objects in simulations involving an 8.4 M ⊕, q = 240 au perturber (right). Colors indicate final inclination, and the black contours are curves of constant perihelion. In the control case, most objects that exit the 9:1 resonance remain at low-inclination perihelion distances, while objects affected by a perturber are raised to high q and i.
Paper: 3 μm Phase Curves of Main-belt Asteroids from NEOWISE Photometry
Authors: Matthew Varakian, Nancy Chanover, Joseph Masiero, Dagmara Oszkiewicz
Figure caption: Left: W1 phase slopes of asteroids with 3 μm spectra from the AKARI mission vs. their 2.7 μm band depth as measured by Usui et al. (2019). Right: W1 phase slopes of asteroids with 3 μm spectra from the AKARI mission vs. their 3.1 μm band depth as measured by Usui et al. (2019). The colors and shapes of the points correspond to the Tholen spectral classification of that asteroid.
Paper: 3 μm Phase Curves of Main-belt Asteroids from NEOWISE Photometry
Authors: Matthew Varakian, Nancy Chanover, Joseph Masiero, Dagmara Oszkiewicz
Figure caption: W1 phase slope vs. diameter (km) for Themis-family objects, Flora-family objects, and AKARI objects.
Paper: 3 μm Phase Curves of Main-belt Asteroids from NEOWISE Photometry
Authors: Matthew Varakian, Nancy Chanover, Joseph Masiero, Dagmara Oszkiewicz
Figure caption: Left: W1 phase slopes of asteroids with 3 μm spectra from the AKARI mission vs. their visible albedo. Right: W1 phase slopes of asteroids with 3 μm spectra from the AKARI mission vs. their W1 albedo. The colors and shapes of the points correspond to the Tholen spectral classification of that asteroid. The bold points represent the mean phase slope vs. the mean albedo of the C, M, and S spectral types within our sample.
Paper: 3 μm Phase Curves of Main-belt Asteroids from NEOWISE Photometry
Authors: Matthew Varakian, Nancy Chanover, Joseph Masiero, Dagmara Oszkiewicz
Figure caption: W1 phase curve of (222) Lucia. This phase curve was produced using thermally and rotationally corrected observations from all phases of the NEOWISE mission. Blue points use observations from the reactivation phase, while the black points are from the four-band, full cryo phase of the mission. The orange line is the linear fit from which a slope is derived.
Paper: 3 μm Phase Curves of Main-belt Asteroids from NEOWISE Photometry
Authors: Matthew Varakian, Nancy Chanover, Joseph Masiero, Dagmara Oszkiewicz
Figure caption: Composite lightcurve of asteroid (222) Lucia, a member of the Themis dynamical family. Orange points are the simulated V-band lightcurve from ISAM, while blue points are W1 observations from NEOWISE. The red line is a sixth-order Fourier fit used to estimate the synodic rotation period and determine the rotation correction.
Paper: 3 μm Phase Curves of Main-belt Asteroids from NEOWISE Photometry
Authors: Matthew Varakian, Nancy Chanover, Joseph Masiero, Dagmara Oszkiewicz
Figure caption: Left: raw observations of Themis-family asteroid (222) Lucia and the thermal flux estimates that were subtracted off. At most, the thermal flux accounted for roughly 4% of the total observed flux for (222) Lucia at the largest phase angles. Right: raw observations of C-type asteroid (46) Hestia, showing larger thermal flux contributions. Near 30°, the thermal flux accounted for roughly 35% of the total observed flux.
Paper: 3 μm Phase Curves of Main-belt Asteroids from NEOWISE Photometry
Authors: Matthew Varakian, Nancy Chanover, Joseph Masiero, Dagmara Oszkiewicz
Figure caption: Left: W1 phase slope vs. phase angle coverage for Themis-family objects. Right: diameter vs. phase angle coverage for Themis-family objects. The orange line is a linear fit to the data.
Paper: 3 μm Phase Curves of Main-belt Asteroids from NEOWISE Photometry
Authors: Matthew Varakian, Nancy Chanover, Joseph Masiero, Dagmara Oszkiewicz
Figure caption: W1 phase slopes of asteroids with 3 μm spectra from the AKARI mission vs. their 3 μm spectral slope. The colors and shapes of the points correspond to the Tholen spectral classification of that asteroid.
Paper: 3 μm Phase Curves of Main-belt Asteroids from NEOWISE Photometry
Authors: Matthew Varakian, Nancy Chanover, Joseph Masiero, Dagmara Oszkiewicz
Figure caption: Filter response functions for WISE bandpasses. From left to right: W1, W2, W3, and W4. The W1 filter covers roughly the wavelengths from 3 to 4 μm.
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: Spectra from IRSA (light gray) are normally adjusted to photometric points (blue) to scale the spectrum to absolute flux. The photometry for G227 was off owing to a light leak in the filter, so we scaled the G227 data to match the TPM (red) at a wavelength that is not expected to have significant MIR features (19 μm) (dark gray).