adsabs/AstroCLIMB huggingface dataset:
Paper: Electron Injection via Modified Diffusive Shock Acceleration in High-Mach-number Collisionless Shocks
Authors: A. Grassi, H. G. Rinderknecht, G. F. Swadling, D. P. Higginson, H.-S. Park, A. Spitkovsky, F. Fiuza
Figure caption: (a) Magnetic field B  z  at ﹩{t}_{\mathrm{sel}}\simeq 2.5\times {10}^{3}\,{\omega }_{{pi}}^{-1}﹩. The shock front positions and their propagation direction are highlighted by the black lines and arrows. (b) Energy spectrum of the electrons in a downstream region extending for ≃ ±100 c/ω  pi  at ﹩{t}_{\mathrm{sel}}\simeq 2.5\times {10}^{3}\,{\omega }_{{pi}}^{-1}﹩ (blue plain line) and ﹩t=5\times {10}^{3}\,{\omega }_{{pi}}^{-1}﹩ (orange plain line). The thermal component given by the Maxwellian fit (black dashed line) and the nonthermal components (obtained by subtracting the thermal component from the full distribution) are shown at both times (blue and orange dotted lines, respectively). (c) Magnetic power spectrum in the shock downstream −22 < x ω  pi /c < 22 at ﹩t\simeq 1260\,{\omega }_{{pi}}^{-1}﹩ (plain lines) and inverse gyroradii for downstream electrons with energy ε NT ≃ 4k B T  e  (dashed vertical lines), considering the average B-field amplitude in the downstream, for simulations using m  i /(m  e  Z) = 128 (blue lines) and 512 (orange lines).
Paper: Electron Injection via Modified Diffusive Shock Acceleration in High-Mach-number Collisionless Shocks
Authors: A. Grassi, H. G. Rinderknecht, G. F. Swadling, D. P. Higginson, H.-S. Park, A. Spitkovsky, F. Fiuza
Figure caption: (a) Typical particle energization trajectory as a function of its longitudinal position (i.e., along the x-axis) and time (color bar), magnetic field amplitude (red plain line), and flow velocity (red dotted line) averaged along the transverse y-direction at ﹩t\simeq 7125\,{\omega }_{{pe}}^{-1}﹩. (b) Evolution in time of the electron energy (black line), of the work done by the electric field, assuming the particle motion to be described by the gradient drift approximation (green line), and of the magnetic moment (red line) averaged over the local gyroperiod, during a typical energization event. (c) Evolution of the average particle energy (black line) and the average work within the gradient drift approximation (green line). Shaded gray lines correspond to the energy evolution in time of all particles.
Paper: Formation and Dynamics in an Observed Preeruptive Filament
Authors: Jing Huang, Yin Zhang, Baolin Tan, Xianyong Bai, Leping Li, Zhenyong Hou, Xiao Yang, Kaifan Ji, Yongliang Song, Ziyao Hu, Yuanyong Deng
Figure caption: The multiwavelength observations of the emerged hot loop (L1, denoted by green arrows in the left panel), the new-formed filament (F1, denoted by yellow arrows in the right panel) and the preexisting stable filament (F0). After coordinate transforming, the images at 195 Å of EUVI and 465 Å of SUTRI show the same spatial location as the AIA images. The boxes B1 (black) and B2 (white) are the selected regions to calculate the temperature of L1 at 14:22 UT and the emission light curve of L1 and F1 from 14:18 to 14:34 UT. The white dotted line in (i) is the slice AB, which follows the rising direction of L1.
Paper: Formation and Dynamics in an Observed Preeruptive Filament
Authors: Jing Huang, Yin Zhang, Baolin Tan, Xianyong Bai, Leping Li, Zhenyong Hou, Xiao Yang, Kaifan Ji, Yongliang Song, Ziyao Hu, Yuanyong Deng
Figure caption: (a) The time–distance plot of slice AB at 1600 Å. The bright emission along slice AB emerges and moves upward. (b) The DEM result of B1 in L1 at 14:22 UT. The typical temperature of L1 is about 6.5 MK. (c) The normalized flux of B2 of L1 and F1 at 131 Å (blue), 171 Å (green), 193 Å (red), 211 Å (orange), 304 Å (black), and 465 Å (blue dotted line). The first impulsive peak from 14:19 to 14:24 UT corresponds to the emergence of L1. During the second smooth peak, F1 is formed after the cooling and expansion of L1. The emission at 304 Å presents a slower decay than that of 465 Å.
Paper: Formation and Dynamics in an Observed Preeruptive Filament
Authors: Jing Huang, Yin Zhang, Baolin Tan, Xianyong Bai, Leping Li, Zhenyong Hou, Xiao Yang, Kaifan Ji, Yongliang Song, Ziyao Hu, Yuanyong Deng
Figure caption: Material transfer from the north root to the whole body of the new large-scale filament (F4). F2 and F3 are denoted by yellow arrows in EUVI images at 304 Å. The EUVI images at 304 Å, SUTRI images at 465 Å are transformed into the AIA coordinate system and they cover the same region. Left panel: in the 1600 Å image, a bright tiny jet (denoted by the green arrow) appears near the north root of F4. Middle panel: part of F4 is built of a bright structure at 304, 465, and 1600 Å and a dark one at 193 Å. Right panel: the whole structure of F4 is formed. The slice CDE (red dotted line) is along the north leg and the main body of F4.
Paper: Formation and Dynamics in an Observed Preeruptive Filament
Authors: Jing Huang, Yin Zhang, Baolin Tan, Xianyong Bai, Leping Li, Zhenyong Hou, Xiao Yang, Kaifan Ji, Yongliang Song, Ziyao Hu, Yuanyong Deng
Figure caption: Observations of the recombination of filaments F2 and F4, the new emerging loop L2, and the eruptive twisted filament F5 in multiwavelengths. The EUVI/STEREO images at 304 and 195 Å are transformed into the the Earth-based coordinate, which show the same spatial location as AIA at 211 and 1600 Å. Left panel: F4 and F2 expand to a larger size. Middle panel: a new loop (L2, denoted by green arrows) emerges under the filaments F2 and F4, and three structures interact with each other. Right panel: the eruptive filament (F5) has a twisted structure mainly visible in emission. In 304 Å we note some dispersive looplike dark structures.
Paper: Formation and Dynamics in an Observed Preeruptive Filament
Authors: Jing Huang, Yin Zhang, Baolin Tan, Xianyong Bai, Leping Li, Zhenyong Hou, Xiao Yang, Kaifan Ji, Yongliang Song, Ziyao Hu, Yuanyong Deng
Figure caption: (a) Time–distance plot of slice CD at 1600 Å. The jet and material injections are denoted by white and yellow arrows, respectively. (b) Time–distance plot of slice DE at 1600 Å. Two branches of bright shifting structure are denoted by I and II. (c) Time–distance plot of slice DE at 304 Å. Bright shifting structures are shown in F4 and the shifting speed is about 82 km s−1. (d)–(e) Time–distance plot of slice DE at 193 and 211 Å. Many tiny dark channels appear intermittently in F4 and shift at the speed of about 82 km s−1.
Paper: Formation and Dynamics in an Observed Preeruptive Filament
Authors: Jing Huang, Yin Zhang, Baolin Tan, Xianyong Bai, Leping Li, Zhenyong Hou, Xiao Yang, Kaifan Ji, Yongliang Song, Ziyao Hu, Yuanyong Deng
Figure caption: The reconnection between filaments F0 and F1 at 195 Å of EUVI. (a) The S-shaped filament (F0) and large archlike filament (F1) before reconnection. (b) and (c) Bright emission appears along the filament F0 (denoted by white solid arrows) during the reconnection process. (d) The new-formed small archlike filament (F2) and large sigmoid filament (F3) after reconnection.
Paper: A Unified Picture of Short and Long Gamma-Ray Bursts from Compact Binary Mergers
Authors: Ore Gottlieb, Brian D. Metzger, Eliot Quataert, Danat Issa, Tia Martineau, Francois Foucart, Matthew D. Duez, Lawrence E. Kidder, Harald P. Pfeiffer, Mark A. Scheel
Figure caption: The jet power evolution of postmerger accretion disks for varying levels of magnetic flux ranging from non-MAD to MAD. Dark gray lines show the postmerger mass accretion rate evolution (right vertical axis) obtained for four BH–NS merger simulations (Gottlieb et al. 2023a) and the five BNS merger simulations presented here, all of which generate massive disks, M  d  ≈ 0.1 M ⊙. Light gray lines delineate the postmerger accretion rates from five BH–NS merger simulations that result in disk masses M  d  ≈ 0.007 M ⊙. The dark (light) purple lines mark the logarithmic averages of the mass accretion rates for M  d  ≈ 0.1 M ⊙ (M  d  = 0.007 M ⊙), which constitute the maximum jet power assuming η  a  = 1 corresponding to a BH spin a ≈ 0.87 (left vertical axis). Black (for low-mass disks) and orange (for high-mass disks) lines schematically illustrate the jet power evolution for different assumptions about the dimensional magnetic flux threading the BH, Φ, and the corresponding total jet energy, E  j , for the case of the massive disk. Since the magnetic flux on the BH is likely accumulated early and hence remains nearly constant before the disk transitions to MAD, the jet power, P  j , is also predicted to be roughly constant at these times, powering the prompt emission. Once the dimensionless magnetic flux saturates in the MAD state, the jet power saturates at ﹩{P}_{j}=\dot{M}{c}^{2}﹩ and thus follows the mass accretion rate ﹩\dot{M}\propto {t}^{-2}﹩ thereafter, powering the EE (we have extrapolated P  j  by a dashed line to later times). The yellow (blue) region outlines the estimated average jet power and duration T 90 (T 50) of the sbGRB (lbGRB) population based on prompt emission and afterglow observations (see text). While the jets from massive disks (orange lines) are either too powerful or operate for too long, compared to the prompt sbGRB population, BH accretion from massive disks nicely matches the observed properties of prompt lbGRBs. Jets from less massive disks (black lines) fit the luminosity and duration of sbGRBs and are unable to give rise to lbGRBs (see Figures 4 and 5 for the jet power evolution in simulations).
Paper: A Unified Picture of Short and Long Gamma-Ray Bursts from Compact Binary Mergers
Authors: Ore Gottlieb, Brian D. Metzger, Eliot Quataert, Danat Issa, Tia Martineau, Francois Foucart, Matthew D. Duez, Lawrence E. Kidder, Harald P. Pfeiffer, Mark A. Scheel
Figure caption: Time evolution on the BH horizon for different models. Panel (a): The mass accretion rate in all models follows ﹩\dot{M}\approx {(t/0.01\,\,{\rm{s}})}^{-2}﹩. Panel (b): The dimensionless magnetic flux ﹩\phi ={\rm{\Phi }}/\sqrt{\dot{M}{{cr}}_{g}^{2}}﹩ shows a gradual increase until entering the MAD state at ϕ ≈ 50 (vertical dashed lines), after which it remains roughly constant. Panel (c): The jet launching efficiency η ≡ η  ϕ  η  a  increases gradually with ϕ until it reaches the maximum launching efficiency η ≈ 0.4 in the MAD state. Panel (d): The jet power, ﹩{P}_{j}=\eta \dot{M}{c}^{2}﹩, is roughly constant due to constant dimensional magnetic flux threading the BH. Once the disk becomes MAD, η saturates, and the jet power drops as ﹩{P}_{j}\sim \dot{M}\sim {t}^{-2}﹩ (vertical dashed lines).
Paper: A Unified Picture of Short and Long Gamma-Ray Bursts from Compact Binary Mergers
Authors: Ore Gottlieb, Brian D. Metzger, Eliot Quataert, Danat Issa, Tia Martineau, Francois Foucart, Matthew D. Duez, Lawrence E. Kidder, Harald P. Pfeiffer, Mark A. Scheel
Figure caption: The outcomes of compact object mergers and their ability to power various cbGRB subclasses as a function of the binary mass ratio (vertical axis) and total mass (horizontal axis). lbGRBs occur in high-M tot and high-q BNS mergers that form a massive BH disk of M  d  ∼ 10−1 M ⊙ or in high premerger BH spin and low mass ratio BH–NS mergers (blue region). sbGRBs may arise either from equal mass ratio BNS mergers (bottom yellow region) and low premerger BH spin/high mass ratio BH–NS mergers (top yellow region) or by HMNSs formed in BNS mergers with M tot ≲ 2.8 M ⊙ (left yellow region). If BH-powered jets are different than HMNS-powered jets, then the absence of evidence for distinct subclasses of sbGRBs suggests that either BHs or HMNSs are likely to be the sole origin of these events; i.e., only one of the proposed sbGRB scenarios is correct. The Galactic BNS mass distribution, the bimodal GRB duration distribution, and GW170817 observations favor HMNSs as the engine of sbGRB jets.
Paper: A Unified Picture of Short and Long Gamma-Ray Bursts from Compact Binary Mergers
Authors: Ore Gottlieb, Brian D. Metzger, Eliot Quataert, Danat Issa, Tia Martineau, Francois Foucart, Matthew D. Duez, Lawrence E. Kidder, Harald P. Pfeiffer, Mark A. Scheel
Figure caption: An illustration of how the underlying physics of the merger product (orange) in the hybrid and all-BH scenarios (red) translates into different phases in the cbGRB light curves: sbGRBs (yellow), lbGRBs (blue), and preceding and succeeding phases (green). The precursor flare (Section 5.1) can be generated either by the accumulation of a stochastic magnetic field on a BH (Gottlieb et al. 2023a) or by an HMNS (Most & Quataert 2023). An sbGRB can be powered either by a BH surrounded by a nonmassive disk before it transitions to a MAD state (Section 4.1) or by a long-lived HMNS (Section 4.2). On the other hand, an lbGRB emerges from BHs with massive disks before they enter the MAD state (Section 2), whether the BH formed promptly in the all-BH scenario or followed an HMNS collapse in the hybrid scenario. Finally, the BH disk becomes MAD and follows P  j  ∼ t −2 to power the EE. Representations of the light curves of the lbGRB 211211A (Rastinejad et al. 2022) and sbGRB 160821B (Stanbro & Meegan 2016) are shown in black and gray, respectively, in a log-log scale. Both are confirmed to be cbGRBs by their detected kilonova counterparts (Lamb et al. 2019; Rastinejad et al. 2022).
Paper: A Unified Picture of Short and Long Gamma-Ray Bursts from Compact Binary Mergers
Authors: Ore Gottlieb, Brian D. Metzger, Eliot Quataert, Danat Issa, Tia Martineau, Francois Foucart, Matthew D. Duez, Lawrence E. Kidder, Harald P. Pfeiffer, Mark A. Scheel
Figure caption: Same as Figure 4 but for the BH–NS merger simulations.
Paper: Deciphering Solar Coronal Heating: Energizing Small-scale Loops through Surface Convection
Authors: D. Nóbrega-Siverio, F. Moreno-Insertis, K. Galsgaard, K. Krikova, L. Rouppe van der Voort, R. Joshi, M. S. Madjarska
Figure caption: Heating in our CBP model. (a), (b) Heating per unit mass averaged over ∼4.5 hr for the Joule (﹩\overline{{Q}_{J}/\rho }﹩ ) and viscous (﹩\overline{{Q}_{V}/\rho }﹩ ) terms, respectively, at z = [8, 5, 2] Mm. (c), (d) Heating per unit mass averaged horizontally within the CBP at z = [5, 2] Mm, respectively, for the Joule (〈Q  J /ρ〉CBP, black) and viscous (〈Q  V /ρ〉CBP, orange) terms as a function of time. The Pearson correlation coefficient r between the curves is shown in red in the upper left corner of the plot frame. (e) Time average of the horizontal mean vertical Poynting flux (﹩\overline{\langle {S}_{z}\rangle }﹩) within the CBP (blue) and in the coronal hole surroundings (red).
Paper: Deciphering Solar Coronal Heating: Energizing Small-scale Loops through Surface Convection
Authors: D. Nóbrega-Siverio, F. Moreno-Insertis, K. Galsgaard, K. Krikova, L. Rouppe van der Voort, R. Joshi, M. S. Madjarska
Figure caption: Initial condition. (a) Initial horizontal average stratification for the temperature T and density ρ. (b) Imposed nullpoint magnetic field configuration (red lines) embedded within a coronal-hole-like magnetic field (blue). The yellow isosurface at B = 1 G delimits the nullpoint location. Other features of this configuration are also highlighted following the 3D nullpoint terminology (Priest & Titov 1996). The solar granulation pattern of the initial model is shown through the vertical velocity u  z  at z = 0. The red–green–blue coordinate system indicates the orientation of the x–y–z-axis.
Paper: Deciphering Solar Coronal Heating: Energizing Small-scale Loops through Surface Convection
Authors: D. Nóbrega-Siverio, F. Moreno-Insertis, K. Galsgaard, K. Krikova, L. Rouppe van der Voort, R. Joshi, M. S. Madjarska
Figure caption: Observations of a representative CBP on 2022 July 1 at 08:08:52 UT. (a), (b) Hot coronal response in EUV detected by SDO/AIA 193 Å and SDO/AIA 171 Å, respectively. (c) Cool chromospheric structure of the CBP in the Hα line core observed with SST/CRISP. (d) Photospheric line-of-sight (LOS) magnetic field (BLOS) from SST/CRISP. (e) Hα profiles for different regions of the dark fibrils (cool colors) and core brightenings (warm colors) marked in panel (c). The average profile over the whole field of view is shown as a black dashed line. The intensity of the profiles has been normalized to the intensity value at 50 km s−1.
Paper: Tidal Dissipation Regimes among the Short-period Exoplanets
Authors: Emma M. Louden, Gregory P. Laughlin, Sarah C. Millholland
Figure caption: Dependence of normalized tidal dissipation rate on eccentricity and obliquity. The map shows the contours of the normalized tidal dissipation rate (﹩\dot{E}(e,\epsilon )/{K}_{p}﹩ from Equation (4)). Dissipation is enhanced by several orders of magnitude for a given eccentricity as obliquity increases. Marked on the plot is the scale parameter, σ = 0.05, which provides the best-fit Rayleigh distribution modeling the eccentricity distribution of compact multitransiting multiplanet systems (Mills et al. 2019).
Paper: Tidal Dissipation Regimes among the Short-period Exoplanets
Authors: Emma M. Louden, Gregory P. Laughlin, Sarah C. Millholland
Figure caption: Simulated evolution of period ratios for a synthetic planet population. Top: time evolution of a population of planets initially uniformly distributed in Δ due to the action of the model encapsulated by Equation 3 from Lithwick & Wu (2012), which assumes a fiducial Q of 10. Bottom: the time evolution over 2 billion years of four populations parameterized by Q, and spaced initially uniformly in Δ. Systems with lower Q are more dissipative than those with higher Q and evacuate the region near Δ = 0 more rapidly.
Paper: Tidal Dissipation Regimes among the Short-period Exoplanets
Authors: Emma M. Louden, Gregory P. Laughlin, Sarah C. Millholland
Figure caption: Systems with multiple transiting planets displaying period ratios near 2:1. Symbol sizes are proportional to reported planetary radii, and the systems are ordered by increasing stellar mass (printed on the right axis). The navy shaded planets are both near 2:1 mean motion resonance and have inferred dissipation factors ﹩3\lt {\mathrm{log}}_{10}Q\lt 6﹩. The light-pink-shaded points with gray borders represent planets near the 2:1 commensurability but with a ﹩{\mathrm{log}}_{10}Q﹩ outside of 3–6.
Paper: Tidal Dissipation Regimes among the Short-period Exoplanets
Authors: Emma M. Louden, Gregory P. Laughlin, Sarah C. Millholland
Figure caption: Fractional distance from resonance for planet pairs near first-order mean-motion resonances. Multitransiting exoplanetary systems near the 3:2 and 2:1 commensurabilities tend to accumulate just wide of the exact resonances (which occur for Δ = 0). There is both an overdensity at ratios Δ > 0 and a paucity for Δ < 0.
Paper: Tidal Dissipation Regimes among the Short-period Exoplanets
Authors: Emma M. Louden, Gregory P. Laughlin, Sarah C. Millholland
Figure caption: Top: inferred Q values when inner (left)/outer (right) planets are assumed to drive resonant repulsion. Dashed lines mark Q values estimated for Earth, Neptune, and Jupiter. The solid magenta vertical lines for each bin corresponds to the 1σ bounds on the count of each bin observed in N = 5000 bootstrap trials. Bottom: the distribution of inferred Q values within near-resonant short-period planets when randomly selecting one planet from each pair to contribute. The 1σ confidence intervals are as in the top panels.
Paper: The Aligned Orbit of the Eccentric Proto Hot Jupiter TOI-3362b 
Authors: Juan I. Espinoza-Retamal, Rafael Brahm, Cristobal Petrovich, Andrés Jordán, Guđmundur Stefánsson, Elyar Sedaghati, Melissa J. Hobson, Diego J. Muñoz, Gavin Boyle, Rodrigo Leiva, Vincent Suc
Figure caption: TESS and ground-based transit photometry of TOI-3362b overplotted with the best-modeled light curves. Residuals are shown for all transits. TESS light curves of different years are shown all together. Observatoire Moana–ES light curve is also shown with 10 minute binned data in black, and they are available as the data behind the figure.(The data used to create this figure are available.)
Paper: The Aligned Orbit of the Eccentric Proto Hot Jupiter TOI-3362b 
Authors: Juan I. Espinoza-Retamal, Rafael Brahm, Cristobal Petrovich, Andrés Jordán, Guđmundur Stefánsson, Elyar Sedaghati, Melissa J. Hobson, Diego J. Muñoz, Gavin Boyle, Rodrigo Leiva, Vincent Suc
Figure caption: Mass vs. semimajor axis diagram for the possible coplanar outer companions to TOI-3362b. Red regions indicate zones where we can rule out the companion at 1σ and 2σ confidence levels. The black dashed line shows the mass of TOI-3362b. The red dashed line shows ϵ gr = 1 (Equation (2)), demarking the regions where secular excitation is quenched by relativistic precession (ϵ gr > 1). Since the companion might lie in the region where secular eccentricity excitation is forbidden, we discard it as responsible for the current high eccentricity of TOI-3362b.
Paper: The Aligned Orbit of the Eccentric Proto Hot Jupiter TOI-3362b 
Authors: Juan I. Espinoza-Retamal, Rafael Brahm, Cristobal Petrovich, Andrés Jordán, Guđmundur Stefánsson, Elyar Sedaghati, Melissa J. Hobson, Diego J. Muñoz, Gavin Boyle, Rodrigo Leiva, Vincent Suc
Figure caption: Left: out-of-transit radial velocities of TOI-3362 taken with different instruments. The red curve shows the best model. Residuals are shown at the bottom. Right: out-of-transit radial-velocity curve in phase. The red curve shows the best model, and the red regions show 1σ, 2σ, and 3σ models. FEROS data are available as the data behind the figure.(The data used to create this figure are available.)
Paper: The Aligned Orbit of the Eccentric Proto Hot Jupiter TOI-3362b 
Authors: Juan I. Espinoza-Retamal, Rafael Brahm, Cristobal Petrovich, Andrés Jordán, Guđmundur Stefánsson, Elyar Sedaghati, Melissa J. Hobson, Diego J. Muñoz, Gavin Boyle, Rodrigo Leiva, Vincent Suc
Figure caption: ESPRESSO observations of the RM effect of TOI-3362b with the Keplerian signal removed. The red line shows the best fit, and the red areas show 1σ, 2σ, and 3σ models. The bottom panel shows the residuals. The ESPRESSO RVs of this figure without the Keplerian signal removed are available as data behind the figure.(The data used to create this figure are available.)
Paper: The Aligned Orbit of the Eccentric Proto Hot Jupiter TOI-3362b 
Authors: Juan I. Espinoza-Retamal, Rafael Brahm, Cristobal Petrovich, Andrés Jordán, Guđmundur Stefánsson, Elyar Sedaghati, Melissa J. Hobson, Diego J. Muñoz, Gavin Boyle, Rodrigo Leiva, Vincent Suc
Figure caption: Sky-projected obliquity vs. the eccentricity of all giant planets (M  p  > 0.2 M J and R  p  > 8 R ⊕) with e > 0.1 colored by their final semimajor axes a final = a(1 − e 2) from TEPCat (Southworth 2011). TOI-677b was also measured using ESPRESSO (Sedaghati et al. 2023). The left panel shows single stars, while the right panel shows known binary systems. All planets, excepting Kepler-420b, are or will be hot Jupiters with enough time.
Paper: The Aligned Orbit of the Eccentric Proto Hot Jupiter TOI-3362b 
Authors: Juan I. Espinoza-Retamal, Rafael Brahm, Cristobal Petrovich, Andrés Jordán, Guđmundur Stefánsson, Elyar Sedaghati, Melissa J. Hobson, Diego J. Muñoz, Gavin Boyle, Rodrigo Leiva, Vincent Suc
Figure caption: Joint posterior distributions and histograms of the posteriors for the physical parameters of our model.
Paper: Tidal Dissipation Regimes among the Short-period Exoplanets
Authors: Emma M. Louden, Gregory P. Laughlin, Sarah C. Millholland
Figure caption: Systems with multiple transiting planets displaying period ratios near 3:2. The features are exactly analogous to Figure 4, except for 3:2.