adsabs/AstroCLIMB huggingface dataset:
Paper: Early Evidence for Isotropic Planetary Obliquities in Young Super-Jupiter Systems
Authors: Michael Poon, Marta L. Bryan, Hanno Rein, Jiayin Dong, Joshua S. Speagle, 佳士 沈, Dang Pham
Figure caption: Left: inferred posterior (Equation (B3)) for the population of four super-Jupiters, using data shown in Figure 5. The shaded gray line assumes a longer rotation period for AB Pic b (16.8 hr instead of 2.1 hr, in case the observed modulation underestimates the true rotation period (Section 3.4.2 of S. Gandhi et al. 2025). This changes ip for AB Pic b, but does not affect our inference qualitatively. Right: Bayes factor BF0,5, where values greater than 1 support κ = 0 over κ = 5, for various subsets of the observed systems. Across all systems, the Bayes factor is 15. This indicates strong but not decisive evidence that super-Jupiter obliquities are consistent with an underlying isotropic distribution, suggestive of brown-dwarf-like formation.
Paper: Early Evidence for Isotropic Planetary Obliquities in Young Super-Jupiter Systems
Authors: Michael Poon, Marta L. Bryan, Hanno Rein, Jiayin Dong, Joshua S. Speagle, 佳士 沈, Dang Pham
Figure caption: We test whether a Bayes factor can correctly identify the underlying formation scenario. For each of 100,000 draws, we simulate observations for 4 or 10 systems. For each draw, we compute the Bayes factor BF5,0 if the correct scenario is κ = 5, or BF0,5 if the correct scenario is κ = 0. A ratio greater than one favors the correct scenario. Top: with four systems and 15° uncertainties, the correct scenario is recovered for 93% of the draws for κ = 5 and 77% of the draws for κ = 0. Bottom: using 10 systems and 10° uncertainties improves the accuracy to 97% and 93%, respectively.
Paper: Early Evidence for Isotropic Planetary Obliquities in Young Super-Jupiter Systems
Authors: Michael Poon, Marta L. Bryan, Hanno Rein, Jiayin Dong, Joshua S. Speagle, 佳士 沈, Dang Pham
Figure caption: Obliquity distributions for κ = 4, κ = 6, and a Weibull distribution, compared to the fiducial κ = 5 Fisher distribution used to model planet-like formation. The Weibull distribution parameters (k = 1.75, λ = 0.71) match the mode of the κ = 5 distribution, but produce a shallower tail. These alternative choices change the Bayes factor from 15 to 8, 24, and 9, respectively, still favoring a brown-dwarf-like (κ = 0) scenario with a Bayes factor of order 10.
Paper: Early Evidence for Isotropic Planetary Obliquities in Young Super-Jupiter Systems
Authors: Michael Poon, Marta L. Bryan, Hanno Rein, Jiayin Dong, Joshua S. Speagle, 佳士 沈, Dang Pham
Figure caption: Bayes factors comparing κ = 0 to various κ. Decisive evidence (BF ∼ 100) for κ = 0 is reached when the comparison model is κ ∼ 12, corresponding to an obliquity distribution peaking at 17°.
Paper: The ODYSSEUS Survey. Spatial Correlation of Magnetospheric Inclinations Points to Parsec-scale Star–Cloud Connection
Authors: Caeley V. Pittman, Catherine C. Espaillat, Thanawuth Thanathibodee, Nuria Calvet, Lee W. Hartmann, Sylvie Cabrit
Figure caption: Top panel: same as the top left panel of Figure 1, but with CTTS names labeled. Arrows again denote disk PAs. Lower panels: zoomed-in regions around Lupus I (middle left), Lupus II (middle right), Lupus III (bottom left), and Lupus IV (bottom right). Dashed white lines show the approximate orientation and extent of the primary filaments in the plane of the sky. Blue lines show the mean magnetic field direction, and the line length is 3 pc in the plane of the sky to give a broad indication of the detected correlation scale. High-resolution background images show the Herschel SPIRE 250 μm dust continuum maps from the Herschel Gould Belt Survey (P. André et al. 2010), and low resolution images show the IRIS 100 μm map (M.-A. Miville-Deschênes & G. Lagache 2005). Points are colored by imag according to the color bar in the top panel.
Paper: The ODYSSEUS Survey. Spatial Correlation of Magnetospheric Inclinations Points to Parsec-scale Star–Cloud Connection
Authors: Caeley V. Pittman, Catherine C. Espaillat, Thanawuth Thanathibodee, Nuria Calvet, Lee W. Hartmann, Sylvie Cabrit
Figure caption: Clustering procedure tests, where points are colored by cluster assignment. Filled points indicate high-probability group members (﹩{P}_{ij,{\rm{mean}}}\gt {P}_{{\rm{\min }}}﹩), whereas open points indicate lower-probability members (﹩{P}_{ij,{\rm{mean}}}\leqslant {P}_{{\rm{\min }}}﹩). Gray crosses indicate ungrouped sources marked as noise (﹩{P}_{{\rm{noise}}}\gt {P}_{{\rm{noise}},{\rm{\max }}}﹩). Top left panel: successful clustering of the four Lupus subregions achieved with HDBSCAN using min_cluster_size = 3, min_samples = 3, and cluster_selection_method = excess of mass and coherence clustering thresholds of ﹩{P}_{{\rm{\min }}}﹩ = 0.5 and ﹩{P}_{{\rm{noise}},{\rm{\max }}}﹩ = 0.3, taking only the 3D coordinates into account. These parameters are used for all clustering processes. Top right panel: groups found when assigning randomly generated imag values that are consistent with the observed imag distribution to each MC sample as the fourth dimension in HDBSCAN. Bottom panels: groups found when perturbing randomly assigned imag values by our measured ﹩{\sigma }_{{i}_{{\rm{mag}}}}﹩ values, shown for a representative set of the 100 total iterations.
Paper: The ODYSSEUS Survey. Spatial Correlation of Magnetospheric Inclinations Points to Parsec-scale Star–Cloud Connection
Authors: Caeley V. Pittman, Catherine C. Espaillat, Thanawuth Thanathibodee, Nuria Calvet, Lee W. Hartmann, Sylvie Cabrit
Figure caption: Maps of the Orion (top left), Taurus (top right), and Chamaeleon I (bottom) targets from C. V. Pittman et al. (2025a), with IRIS 100 μm maps (M.-A. Miville-Deschênes & G. Lagache 2005) shown in grayscale. The color bar shows the magnetospheric inclination found from the accretion flow model. Point sizes indicate dGaia such that more distant sources appear smaller. PAs compiled by M. Aizawa et al. (2020) are shown as colored bars. They are determined from 0° ≤ PA < 180° rather than 0° ≤ PA < 360°. The imag and PA values in Orion OB1b and Taurus may be spatially correlated, though the samples are too small to confirm.
Paper: The ODYSSEUS Survey. Spatial Correlation of Magnetospheric Inclinations Points to Parsec-scale Star–Cloud Connection
Authors: Caeley V. Pittman, Catherine C. Espaillat, Thanawuth Thanathibodee, Nuria Calvet, Lee W. Hartmann, Sylvie Cabrit
Figure caption: Inclination uniformity test. Top: ﹩\cos ({i}_{{\rm{mag}}})﹩ histogram (left) and CDF (right) for the eight SFRs in C. V. Pittman et al. (2025a). The CDF figure shows the median and 95% confidence interval of the observed ﹩\cos ({i}_{{\rm{mag}}})﹩ values, as well as those of a uniform distribution. The observed ﹩\cos ({i}_{{\rm{mag}}})﹩ values are consistent with uniformity, within uncertainties. Bottom: same as the top panels, but for the Lupus sample in this work. These ﹩\cos ({i}_{{\rm{mag}}})﹩ values are inconsistent with uniformity.
Paper: The ODYSSEUS Survey. Spatial Correlation of Magnetospheric Inclinations Points to Parsec-scale Star–Cloud Connection
Authors: Caeley V. Pittman, Catherine C. Espaillat, Thanawuth Thanathibodee, Nuria Calvet, Lee W. Hartmann, Sylvie Cabrit
Figure caption: Consensus matrix for the 3D groups found from 5000 MC iterations of HDBSCAN, using min_cluster_size = 3, min_samples = 3, and cluster_selection_method = excess of mass. Dark squares indicate groups with high pairwise comembership probabilities (Pij), and Roman numerals indicate the associated Lupus subregions. Red labels indicate CTTSs that are marked as noise in more than 30% of the MC iterations, all of which are off-cloud sources.
Paper: The ODYSSEUS Survey. Spatial Correlation of Magnetospheric Inclinations Points to Parsec-scale Star–Cloud Connection
Authors: Caeley V. Pittman, Catherine C. Espaillat, Thanawuth Thanathibodee, Nuria Calvet, Lee W. Hartmann, Sylvie Cabrit
Figure caption: New flow model fits to VLT Hα profiles from X-Shooter (XS), UVES, and ESPRESSO (ESP). Continuum-normalized Hα observations are shown in black; Gaussian components representative of the chromosphere are orange, where applicable; magnetospheric contributions are maroon; and total model fits are bright red. The x-axes span ±600 km s−1. Absorption features that cannot be attributed to a magnetospheric origin are masked out in the fitting process.
Paper: The ODYSSEUS Survey. Spatial Correlation of Magnetospheric Inclinations Points to Parsec-scale Star–Cloud Connection
Authors: Caeley V. Pittman, Catherine C. Espaillat, Thanawuth Thanathibodee, Nuria Calvet, Lee W. Hartmann, Sylvie Cabrit
Figure caption: Same as Figure 4, but for the 4D groups. Roman numerals indicate the assigned groups, and red labels indicate CTTSs that are marked as noise in more than 30% of the MC iterations.
Paper: The ODYSSEUS Survey. Spatial Correlation of Magnetospheric Inclinations Points to Parsec-scale Star–Cloud Connection
Authors: Caeley V. Pittman, Catherine C. Espaillat, Thanawuth Thanathibodee, Nuria Calvet, Lee W. Hartmann, Sylvie Cabrit
Figure caption: Hα profile dependence on imag for 6 CTTSs in our sample, with all other accretion flow model parameters fixed.
Paper: Near the Runaway: The Climate and Habitability of Teegarden’s Star b
Authors: Ryan Boukrouche, Rodrigo Caballero, Neil T. Lewis
Figure caption: Global mean surface temperature and planetary albedo as a function of instellation for all simulations. The markers without filling represent the runaway cases shown over the last 2 yr of the simulation. The clear-sky albedo values are computed using the clear-sky fluxes of the same simulations. The green markers correspond to a separate simulation with as = 0.07, where clouds were turned off.
Paper: Near the Runaway: The Climate and Habitability of Teegarden’s Star b
Authors: Ryan Boukrouche, Rodrigo Caballero, Neil T. Lewis
Figure caption: Latitude–longitude maps of surface temperature overlaid with the wind field at the bottom layer, and surface precipitation. The black contours indicate where the surface temperature is 50° Celsius.
Paper: Near the Runaway: The Climate and Habitability of Teegarden’s Star b
Authors: Ryan Boukrouche, Rodrigo Caballero, Neil T. Lewis
Figure caption: Latitude–longitude maps of surface temperature overlaid with the wind field at the bottom layer, and surface precipitation, for ISR = 1580 W m−2, which brings the climate to the onset of a runaway greenhouse effect. The minimum surface temperature between the two surface albedo cases is 345 K or 72°C.
Paper: Radiation Forces and Trajectory of Hayabusa2♯ Target 1998 KY26
Authors: Davide Farnocchia, David Vokrouhlický, Toni Santana-Ros, Przemysław Bartczak, Marco Micheli, Steven R. Chesley
Figure caption: Prior (blue) and posterior (red) cumulative distributions for 1998 KY26’s physical parameter p. The vertical dashed lines indicate the median value of the parameter, and the light gray regions show the first and last 5% of the distribution, helping thus to indicate a 90% confidence region about the median.
Paper: Near the Runaway: The Climate and Habitability of Teegarden’s Star b
Authors: Ryan Boukrouche, Rodrigo Caballero, Neil T. Lewis
Figure caption: Time series of the difference between ASR and OLR across the runaway greenhouse instellation threshold with a surface albedo of 0.07.
Paper: Near the Runaway: The Climate and Habitability of Teegarden’s Star b
Authors: Ryan Boukrouche, Rodrigo Caballero, Neil T. Lewis
Figure caption: Irradiance of an spectral energy distribution (SED) with an effective temperature of 3000 K and a log(g) of 5 log10(cm s−2) representing Teegarden’s Star. The edges of the 16 spectral bands used by SOCRATES are shown as vertical lines.
Paper: Radiation Forces and Trajectory of Hayabusa2♯ Target 1998 KY26
Authors: Davide Farnocchia, David Vokrouhlický, Toni Santana-Ros, Przemysław Bartczak, Marco Micheli, Steven R. Chesley
Figure caption: Radial (R), transverse (T), and normal (N) components of the nongravitational acceleration on 1998 KY26 based on the radiation model discussed in this Letter. The green curve shows the component projected along the spin axis (S).
Paper: Masses, Star Formation Efficiencies, and Dynamical Evolution of 18,000 H II Regions
Authors: Debosmita Pathak, Adam K. Leroy, Ashley. T. Barnes, Todd A. Thompson, Laura A. Lopez, Karin M. Sandstrom, Jiayi Sun, Simon C. O. Glover, Ralf S. Klessen, Eric W. Koch, Kirsten L. Larson, Janice Lee, Sharon Meidt, Patricia Sanchez-Blazquez, Eva Schinnerer, Zein Bazzi, Francesco Belfiore, Médéric Boquien, Ryan Chown, Dario Colombo, Enrico Congiu, Oleg V. Egorov, Cosima Eibensteiner, Sushma Kurapati, Miguel Querejeta, Daniel A. Dale, Timo Kravtsov, Mansi Padave, D. J. Pisano, Erik Rosolowsky, Sumit K. Sarbadhicary, Thomas G. Williams, Remy Indebetouw, Hsi-An Pan, Leonardo Úbeda, Amirnezam Amiri, Frank Bigiel, Guillermo A. Blanc, Kathryn Grasha
Figure caption: Top left: distribution of H II region escape velocities in galaxy centers and disks. Middle left: distribution of pressures due to H II region self-gravity for ﹩{M}_{{\rm{sh}}}=50 \% {M}_{{\rm{Mol}}}^{{\rm{init}}}﹩ (fiducial value; solid gray), ﹩60 \% {M}_{{\rm{Mol}}}^{{\rm{init}}}﹩ (dashed gray), and ﹩70 \% {M}_{{\rm{Mol}}}^{{\rm{init}}}﹩ (dotted–dashed gray); disk 〈PDE〉 (from J. Sun et al. 2023; maroon); fiducial PGrav + 〈PDE〉 (purple), and total PFeedback (green). Bottom left: distribution of H II region Rcirc (gray hatches) and the sizes at which we expect PGrav = 〈PDE〉 (maroon), PGrav = PFeedback (green), and PGrav + 〈PDE〉 = PFeedback (purple). Right: H II region overpressure (shaded blue) vs. underpressure (shaded orange) for PFeedback/PGrav (gray) and PFeedback/(PGrav + 〈PDE〉) (purple; the dashed line indicates the median, with a summary histogram to the right) with 5th/16th/25th/50th/75th/84th/95th percentile contours.
Paper: Black Hole Collisions with Thin Accretion Disks: OJ 287 and Small Mass Ratio Supermassive Black Hole Binary Candidates
Authors: Sean M. Ressler, Luciano Combi, Bart Ripperda, Xinyu Li
Figure caption: Orbits for q = 0.1 (solid purple), q = 0.05 (dashed green), and q = 0.025 (dotted black) given our chosen initial eccentricity (0.657) and binary separation (16.4rg) as determined by CBWwaves. Top: orbital trajectory of the secondary in the y–z (orbital) plane for the first 20,000M, with the central black hole shown as a black circle and one scale height of the disk shown as the orange checkered pattern. The red circle denotes the initial location of the secondary, which moves clockwise, and each orbital loop is marked sequentially. The orbit precesses by roughly 40∘ every period. Bottom: z-coordinate of the orbits as a function of time. For different q during this time period, the orbital trajectories are approximately the same, with the only significant difference being a relative time lag developing and increasing as time goes on.
Paper: A Correlation between Fast Radio Burst Dispersion Measure and Foreground Large-scale Structure
Authors: Maryam Hussaini, Liam Connor, Ralf M. Konietzka, Vikram Ravi, Jakob Faber, Kritti Sharma, Myles Sherman
Figure caption: The observed DM coming from the IGM and halos from ray tracing through the IllustrisTNG simulation (R. M. Konietzka et al. 2025) as a function of the line-of-sight galaxy number density. The yellow dots represent the halo contribution (the DM from the CGM and ICM), the red dots represent the IGM contribution, and the gray dots are the total DM observed. We observe a similar correlation between the excess DM and z-score, as we saw in our data. Halos do not seem to contribute to the correlation.
Paper: A Correlation between Fast Radio Burst Dispersion Measure and Foreground Large-scale Structure
Authors: Maryam Hussaini, Liam Connor, Ralf M. Konietzka, Vikram Ravi, Jakob Faber, Kritti Sharma, Myles Sherman
Figure caption: Statistical significance of correlation between excess foreground DM and galaxy number density as a function of sample size. The black star marks our sample size and p-value. The dotted line shows the average p-value obtained from mock samples using a ray-tracing catalog based on TNG300 (from R. M. Konietzka et al. 2025), and the yellow shaded region is the 90% interval over random draws of NFRB from the 1000 total sightlines. The y-axis is in ﹩{\mathrm{log}}_{10}﹩, and more negative values correspond to stronger correlations. Our result for our sample size of NFRB = 61 is consistent with the simulated expectations.
Paper: A Correlation between Fast Radio Burst Dispersion Measure and Foreground Large-scale Structure
Authors: Maryam Hussaini, Liam Connor, Ralf M. Konietzka, Vikram Ravi, Jakob Faber, Kritti Sharma, Myles Sherman
Figure caption: The left panel shows the stacked excess DM signal for 1000 simulated FRB sightlines from z = 0.30 in IllustrisTNG (R. M. Konietzka et al. 2025), separated into the total cosmic DM (gray), IGM DM (red), and halo DM (gold). The IGM dominates the DM contribution at all impact parameters ≳500 kpc, corresponding to one to two virial radii of typical halos. In the right panel, we show a forward model meant to mimic the observations in this paper, with random redshifts between 0.10 and 0.50, a host DM drawn from a log-normal distribution, and noise added for the Milky Way DM subtraction. Even with ∼40 events, we expect to see excess DM at lower impact parameters at the 2σ–5σ level.
Paper: A Correlation between Fast Radio Burst Dispersion Measure and Foreground Large-scale Structure
Authors: Maryam Hussaini, Liam Connor, Ralf M. Konietzka, Vikram Ravi, Jakob Faber, Kritti Sharma, Myles Sherman
Figure caption: Correlation between excess DM and z-score for: (a) the full FRB sample; and (b) the Legacy Survey subsample. The x-axis shows the z-score (number of standard deviations from the mean) of the galaxy number density, while the y-axis shows the excess DM. The gray dots represent the individual FRBs. The vertical error bars are plotted in black. The black lines show the linear best fit, and the yellow shaded region is the 1σ prediction interval of the fit. The inset text displays the p-value of the correlation and the best-fit equation. Both samples demonstrate a positive correlation between galaxy number density along the line of sight and excess DM.
Paper: A Correlation between Fast Radio Burst Dispersion Measure and Foreground Large-scale Structure
Authors: Maryam Hussaini, Liam Connor, Ralf M. Konietzka, Vikram Ravi, Jakob Faber, Kritti Sharma, Myles Sherman
Figure caption: We use the sightline of the DSA-110-discovered FRB 20230216A to demonstrate our basic approach. This source is at z = 0.53 and has a cosmological DM of 788 pc cm−3. The top panel shows a side view of the foreground galaxies, with the redshift on the x-axis and the radius of the cylinder on the y-axis. The FRB source is shown as the gold star at radius = 0 and a redshift of 0.53. The gray circles are foreground galaxies from the Legacy Survey, and their sizes in the vertical direction correspond to their virial radii (scaled to physical kiloparsecs). The bottom left panel is a histogram of galaxy counts within 5 Mpc from 500 random lines of sight at similar galactic latitudes, and to the same redshift as FRB 20230216A. The bottom right panel shows the foreground galaxies within 5 Mpc of the FRB sightline, colored by their redshift, with FRB 20230216A at the center, as the red star. The black dotted circle shows the angular extent of the 5 Mpc cylinder at z = 0.1.
Paper: A Correlation between Fast Radio Burst Dispersion Measure and Foreground Large-scale Structure
Authors: Maryam Hussaini, Liam Connor, Ralf M. Konietzka, Vikram Ravi, Jakob Faber, Kritti Sharma, Myles Sherman
Figure caption: Excess extragalactic DM vs. impact parameter after stacking FRB–galaxy pairs in the Legacy Survey footprint. The error bars are estimated via a resampling technique, in which positions are randomly shuffled. There is evidence for excess DM up to megaparsec scales at ∼2.5σ–3.8σ significance, depending on the estimator.
Paper: A Correlation between Fast Radio Burst Dispersion Measure and Foreground Large-scale Structure
Authors: Maryam Hussaini, Liam Connor, Ralf M. Konietzka, Vikram Ravi, Jakob Faber, Kritti Sharma, Myles Sherman
Figure caption: An estimate of the baryon fraction in the IGM based on a sample of FRBs that do not appear to intersect any foreground galaxy halos or clusters. The left panel shows the per-source estimate of fIGM and associated error bars, plotted as a function of redshift. The right panel shows the posterior of the joint fit to those 15 FRBs, ﹩{ \mathcal P }(\langle {{\boldsymbol{f}}}_{\mathrm{IGM}}\rangle )﹩. Our results suggest fIGM ≥ 0.69 at 95% confidence.
Paper: Induction Heating in Super-Earths: A Thermochemical Perspective
Authors: Yihang Peng, Kristina Kislyakova, Donghao Zheng, Zhongtian Zhang, Jie Deng
Figure caption: Energy release per unit mass due to induction heating as a function of depth inside HD 3167b with a surface temperature of 2000 K (the potential temperature is 2400 K). KN20 represents the previously published numerically inaccurate results (K. Kislyakova & L. Noack 2020). Corrected KN20 represents the results obtained using the original conductivity profile of K. Kislyakova & L. Noack (2020), but with an updated induction heating model.
Paper: Induction Heating in Super-Earths: A Thermochemical Perspective
Authors: Yihang Peng, Kristina Kislyakova, Donghao Zheng, Zhongtian Zhang, Jie Deng
Figure caption: The modulus of the induced current density ((a) and (b)) and energy release per unit mass due to induction heating ((c) and (d)) as a function of depth inside GJ 486b, considering different potential temperatures ((a) and (c)) and Fe fractions in mantle silicates ((b) and (d)).
Paper: Induction Heating in Super-Earths: A Thermochemical Perspective
Authors: Yihang Peng, Kristina Kislyakova, Donghao Zheng, Zhongtian Zhang, Jie Deng
Figure caption: The modulus of the time-varying magnetic field as a function of depth inside GJ 486b, considering different potential temperatures ((a) and (c)) and Fe fractions in mantle silicates ((b) and (d)) in both log scale ((a) and (b)) and linear scale ((c) and (d)).
Paper: Induction Heating in Super-Earths: A Thermochemical Perspective
Authors: Yihang Peng, Kristina Kislyakova, Donghao Zheng, Zhongtian Zhang, Jie Deng
Figure caption: The temperature profile of HD 3167b obtained with different potential temperatures, in comparison with the mantle solidus (M. M. Hirschmann 2000; M. M. Hirschmann et al. 2009; C. K. Sahu et al. 2025). The dashed lines are the extrapolations of adiabatic temperature profiles to the planetary surface.
Paper: Induction Heating in Super-Earths: A Thermochemical Perspective
Authors: Yihang Peng, Kristina Kislyakova, Donghao Zheng, Zhongtian Zhang, Jie Deng
Figure caption: The temperature profile ((a) and (c)) and energy release per unit mass due to induction heating ((b and (d)) in GJ 486b obtained from different iterations of self-consistent calculation. The potential temperature and mantle iron content are 1600 K and 11 mol%, respectively. ((a) and (b)) Fully solid mantle with melt fraction (ϕ = 0). The total energy releases of the first and last iterations are 18.5 and 12.6 W m−2, respectively. ((c) and (d)) Partially molten mantle with melt fraction (ϕ = 0.1). The total energy releases of the first and last iterations are 9.5 and 6.8 W m−2, respectively. All temperatures are truncated at the mantle solidus (M. M. Hirschmann 2000; M. M. Hirschmann et al. 2009; C. K. Sahu et al. 2025).
Paper: Induction Heating in Super-Earths: A Thermochemical Perspective
Authors: Yihang Peng, Kristina Kislyakova, Donghao Zheng, Zhongtian Zhang, Jie Deng
Figure caption: Color maps and contour plots of induction heating efficiency as a function of potential temperature and mantle Fe contents (XFe) in HD 3167b. (a) Total induction heating power inside the planet; (b) maximum depth-dependent energy release per unit mass.