adsabs/AstroCLIMB huggingface dataset:
Paper: The 2025 Failed Outburst of IGR J17091−3624: Spectral Evolution and the Role of Ionized Absorbers
Authors: Oluwashina K. Adegoke, Javier A. García, Guglielmo Mastroserio, Elias Kammoun, Riley M. T. Connors, James F. Steiner, Fiona A. Harrison, Douglas J. K. Buisson, Joel B. Coley, Benjamin M. Coughenour, Thomas Dauser, Melissa Ewing, Adam Ingram, Erin Kara, Edward Nathan, Maxime Parra, Daniel Stern, John A. Tomsick
Figure caption: Variation of the 0.1–100 keV X-ray flux irradiating the companion star as a function of the system’s intrinsic X-ray luminosity, quantified by the distance to the system. Curves are plotted for three orbital period values for the total system mass M in the 3–10 M⊙ range. For each color shade, the solid and the dashed lines denote the curves for 3 M⊙ and 10 M⊙, respectively. The horizontal gray shade, at 1011–1012 erg cm−2 s−1, represents the flux range where the effect of ablation on the companion star is considered significant, as estimated by P. Podsiadlowski (1991).
Paper: The 2025 Failed Outburst of IGR J17091−3624: Spectral Evolution and the Role of Ionized Absorbers
Authors: Oluwashina K. Adegoke, Javier A. García, Guglielmo Mastroserio, Elias Kammoun, Riley M. T. Connors, James F. Steiner, Fiona A. Harrison, Douglas J. K. Buisson, Joel B. Coley, Benjamin M. Coughenour, Thomas Dauser, Melissa Ewing, Adam Ingram, Erin Kara, Edward Nathan, Maxime Parra, Daniel Stern, John A. Tomsick
Figure caption: Variation of black hole mass as a function of distance to the IGR J17091−3624 system. The shaded band depicts the possible range of distance to the system for a given mass and vice versa. This is based on the Γ–LX/LEdd correlation reported in Q.-X. Yang et al. (2015) for BHXBs.
Paper: Curious Case of CGRaBS J0211+1051: Observational Evidence of the Lepto-hadronic Origin of High-energy Emission?
Authors: Sunil Chandra, Pankaj Kushwaha, Pranjupriya Goswami, Michael Zacharias
Figure caption: (a) Multiepoch SEDs (Q in magenta, F1 in red, and F2 in cyan) with the best-fit pure leptonic model indicated by the correspondingly colored lines (solid: total emission without EBL absorption; densely dotted extension of the same: with EBL absorption of A. Franceschini & G. Rodighiero 2017). The shaded colored regions in the γ-ray regime of the SEDs (E:1022–1026 Hz) of 12 yr averaged (gray), F1 (red), and F2 (cyan) refer to the 1σ uncertainty interval around the respective best-fit LogParabola models. (b) Same as (a) but using a hadro-leptonic model. In case of (a) , the dotted, dashed, dotted–dashed, double dotted–dashed, and densely dotted–dashed magenta curves represent the BLR spectrum synchrotron, SSC, EC-BLR, and EC-DT components of Q, respectively. The inset shows the data and model for Q. These components are not plotted for F1 and F2 to keep the clarity in the figures. (c) The injection of leptons of various origins plotted with γ (i.e., energy) derived from the solutions of the Fokker–Planck equation. (d) The predicted neutrino (νμ, νe, ντ) spectra corresponding to Q, F1, and F2 for the hadro-leptonic model used in (b). The IceCube Gen-2 sensitivity is shown by the dashed curve in olive color.
Paper: Curious Case of CGRaBS J0211+1051: Observational Evidence of the Lepto-hadronic Origin of High-energy Emission?
Authors: Sunil Chandra, Pankaj Kushwaha, Pranjupriya Goswami, Michael Zacharias
Figure caption: (a) 10.5 yr long multiwavelength lightcurves of CGRaBS J0211+1051 during UTC 2010 October 31 to 2021 March 27. Top panel: photon flux in γ-rays (≥100 MeV), with black points being 5 day averaged fluxes derived from our analysis and gray points being 7 day averaged fluxes obtained from the LAT lightcurve repository: https://fermi.gsfc.nasa.gov/ssc/data/access/lat/LightCurveRepository/. Middle panel: count rate in X-rays (0.3–10.0 keV). Bottom panel: magnitudes in optical and UV bands (Swift-UVOT, CRTS, Steward Observatory, and ZTF). (b) A zoom-in on 950 days enclosing F2 and Q. (c) A zoom-in on F1. (d) A zoom-in on F2. The red and blue solid lines respectively represent the γ-ray flares F1 and F2 modeled using Equation (1).
Paper: Discovery of a Debris Disk around TWA 20
Authors: Skyler Palatnick, Maxwell A. Millar-Blanchaer, Jingwen Zhang, Kellen Lawson, Briley L. Lewis, Katie A. Crotts, Aarynn L. Carter, Beth Biller, Julien H. Girard, Sebastian Marino, Raphaël Bendahan-West, Giovanni M. Strampelli, Andrew D. James, Klaus Subbotina Stephenson, Rodrigo Ferrer-Chavez, Mark Booth, Ben J. Sutlieff, Aniket Sanghi, Clémence Fontanive, Emily Rickman, Isabel Rebollido, Kielan Hoch, William O. Balmer
Figure caption: Left: disk-subtracted RDI image of the TWA 20 system in the F444W filter. Each off-axis point source is identified by a circle and a label. Middle: disk-subtracted RDI image of the TWA 20 system in the F444W filter zoomed in to the F200W FOV. Right: disk-subtracted RDI image of the TWA 20 system in the F200W filter.
Paper: Discovery of a Debris Disk around TWA 20
Authors: Skyler Palatnick, Maxwell A. Millar-Blanchaer, Jingwen Zhang, Kellen Lawson, Briley L. Lewis, Katie A. Crotts, Aarynn L. Carter, Beth Biller, Julien H. Girard, Sebastian Marino, Raphaël Bendahan-West, Giovanni M. Strampelli, Andrew D. James, Klaus Subbotina Stephenson, Rodrigo Ferrer-Chavez, Mark Booth, Ben J. Sutlieff, Aniket Sanghi, Clémence Fontanive, Emily Rickman, Isabel Rebollido, Kielan Hoch, William O. Balmer
Figure caption: Optimized analytical disk model (left) and the optimized convolved disk model (right) constructed via forward modeling the data in the F200W filter.
Paper: Discovery of a Debris Disk around TWA 20
Authors: Skyler Palatnick, Maxwell A. Millar-Blanchaer, Jingwen Zhang, Kellen Lawson, Briley L. Lewis, Katie A. Crotts, Aarynn L. Carter, Beth Biller, Julien H. Girard, Sebastian Marino, Raphaël Bendahan-West, Giovanni M. Strampelli, Andrew D. James, Klaus Subbotina Stephenson, Rodrigo Ferrer-Chavez, Mark Booth, Ben J. Sutlieff, Aniket Sanghi, Clémence Fontanive, Emily Rickman, Isabel Rebollido, Kielan Hoch, William O. Balmer
Figure caption: Calibrated contrast curves (left) and mass-sensitivity limits (right) for the TWA 20 system in each filter as a function of projected separation. At separations of 1″, equivalent to 80 au, 2 × 10−5 (3 × 10−6) contrasts are achievable with JWST NIRCam in the F444W (F200W) filter, corresponding to planetary masses of 0.3 MJ (2 MJ). The F444W filter is sensitive to lower planetary masses than the F200W filter despite achieving worse contrasts due to the fact that planets are often much brighter at the wavelengths of the F444W filter. The dashed vertical line corresponds to the disk peak radius (r0). The dashed horizontal line corresponds to the mass of Saturn.
Paper: Discovery of a Debris Disk around TWA 20
Authors: Skyler Palatnick, Maxwell A. Millar-Blanchaer, Jingwen Zhang, Kellen Lawson, Briley L. Lewis, Katie A. Crotts, Aarynn L. Carter, Beth Biller, Julien H. Girard, Sebastian Marino, Raphaël Bendahan-West, Giovanni M. Strampelli, Andrew D. James, Klaus Subbotina Stephenson, Rodrigo Ferrer-Chavez, Mark Booth, Ben J. Sutlieff, Aniket Sanghi, Clémence Fontanive, Emily Rickman, Isabel Rebollido, Kielan Hoch, William O. Balmer
Figure caption: Comparison of the forwarded modeled disk and MCRDI image in each filter. Residuals in the F200W filter show some slight oversubtraction, indicating potential overfitting of the disk to the data. Given how faint the disk is in the F444W image, it is unclear how good of a fit the model is to the data. The smoothness of the model compared to the data is simply because the model is constructed (and displayed) without any noise, while the data has various noise sources.
Paper: Discovery of a Debris Disk around TWA 20
Authors: Skyler Palatnick, Maxwell A. Millar-Blanchaer, Jingwen Zhang, Kellen Lawson, Briley L. Lewis, Katie A. Crotts, Aarynn L. Carter, Beth Biller, Julien H. Girard, Sebastian Marino, Raphaël Bendahan-West, Giovanni M. Strampelli, Andrew D. James, Klaus Subbotina Stephenson, Rodrigo Ferrer-Chavez, Mark Booth, Ben J. Sutlieff, Aniket Sanghi, Clémence Fontanive, Emily Rickman, Isabel Rebollido, Kielan Hoch, William O. Balmer
Figure caption: Final MCRDI data reductions for TWA 20 in the F200W (left) and F444W (right) filters. The images are rotated with north up, and the “+” represents the star location. Gaussian smoothing is applied to each image. Each tick represents 1″ (∼80 au). The flux is log scaled in these images.
Paper: Discovery of a Debris Disk around TWA 20
Authors: Skyler Palatnick, Maxwell A. Millar-Blanchaer, Jingwen Zhang, Kellen Lawson, Briley L. Lewis, Katie A. Crotts, Aarynn L. Carter, Beth Biller, Julien H. Girard, Sebastian Marino, Raphaël Bendahan-West, Giovanni M. Strampelli, Andrew D. James, Klaus Subbotina Stephenson, Rodrigo Ferrer-Chavez, Mark Booth, Ben J. Sutlieff, Aniket Sanghi, Clémence Fontanive, Emily Rickman, Isabel Rebollido, Kielan Hoch, William O. Balmer
Figure caption: Color–magnitude diagram depicting the off-axis point source identified in both filters as well as the expected color–magnitude relationship for Jupiter-mass planets of a similar age to the TW Hydrae association (computed with SPECIES with planetary isochrone data from E. F. Linder et al. 2019; M. W. Phillips et al. 2020). The point source clearly does not follow this trend, indicating it is likely a background source.
Paper: Dynamical Masses and Radiative Transfer Modeling of HD 698: A Be Binary in Evolutionary Transition
Authors: Ilfa A. Gabitova, Alex C. Carciofi, Tajan H. de Amorim, Mark Suffak, Anatoly S. Miroshnichenko, Sergey V. Zharikov, Amanda C. Rubio, Steve Danford, Alicia N. Aarnio, Peter Prendergast, Richard J. Rudy, Richard C. Puetter, R. Brad Perry, Aldiyar T. Agishev, Nadezhda L. Vaidman, Serik A. Khokhlov
Figure caption: Corner plots of the MCMC posteriors for the model with disk base density ρ0 = 30.0 × 10−12 g cm−3.
Paper: Dynamical Masses and Radiative Transfer Modeling of HD 698: A Be Binary in Evolutionary Transition
Authors: Ilfa A. Gabitova, Alex C. Carciofi, Tajan H. de Amorim, Mark Suffak, Anatoly S. Miroshnichenko, Sergey V. Zharikov, Amanda C. Rubio, Steve Danford, Alicia N. Aarnio, Peter Prendergast, Richard J. Rudy, Richard C. Puetter, R. Brad Perry, Aldiyar T. Agishev, Nadezhda L. Vaidman, Serik A. Khokhlov
Figure caption: Corner plots of the MCMC posteriors for the model with disk base density ρ0 = 20.0 × 10−12 g cm−3.
Paper: Dynamical Masses and Radiative Transfer Modeling of HD 698: A Be Binary in Evolutionary Transition
Authors: Ilfa A. Gabitova, Alex C. Carciofi, Tajan H. de Amorim, Mark Suffak, Anatoly S. Miroshnichenko, Sergey V. Zharikov, Amanda C. Rubio, Steve Danford, Alicia N. Aarnio, Peter Prendergast, Richard J. Rudy, Richard C. Puetter, R. Brad Perry, Aldiyar T. Agishev, Nadezhda L. Vaidman, Serik A. Khokhlov
Figure caption: Corner plots of the MCMC posteriors for the model with disk base density ρ0 = 15.0 × 10−12 g cm−3.
Paper: Dynamical Masses and Radiative Transfer Modeling of HD 698: A Be Binary in Evolutionary Transition
Authors: Ilfa A. Gabitova, Alex C. Carciofi, Tajan H. de Amorim, Mark Suffak, Anatoly S. Miroshnichenko, Sergey V. Zharikov, Amanda C. Rubio, Steve Danford, Alicia N. Aarnio, Peter Prendergast, Richard J. Rudy, Richard C. Puetter, R. Brad Perry, Aldiyar T. Agishev, Nadezhda L. Vaidman, Serik A. Khokhlov
Figure caption: Corner plots of the MCMC posteriors for the model with disk base density ρ0 = 10.0 × 10−12 g cm−3.
Paper: A Visibility-based 21 cm Bispectrum Estimator for Radio-interferometric Data
Authors: Sukhdeep Singh Gill, Somnath Bharadwaj
Figure caption: Triangle parameterization. The left panel shows a closed triangle k1 + k2 + k3 = 0 with k1 ≥ k2 ≥ k3. The line ﹩\overline{ES}﹩ is the perpendicular bisector of the side k1, and the arc EO represents part of a circle having radius k1. For a fixed k1, the vertex V is restricted to lie within the shaded region that covers triangles of all possible shapes. The same shaded region is also depicted in the (μ, t) plane in the right panel, where it denotes the allowed parameter range. The parameters (μ, t) uniquely parameterize all possible triangle shapes. The shapes corresponding to different parameter values are also indicated.
Paper: A Visibility-based 21 cm Bispectrum Estimator for Radio-interferometric Data
Authors: Sukhdeep Singh Gill, Somnath Bharadwaj
Figure caption: Considering all the estimated 3D BS monopole ﹩\bar{B}({k}_{1},\mu ,t)﹩ without flagging, this shows ﹩{{\rm{\Delta }}}_{\sigma }=| \bar{B}-{[\bar{B}]}_{d}/\sigma ﹩, which is the deviation from ﹩{[\bar{B}]}_{d}﹩ the analytical prediction, relative to σ the expected statistical fluctuations. Each panel considers a different k1. We have estimates for only a few (μ, t) (shapes) at some k1, whereas for others, the entire allowed range (2 μt ≥ 1 black dashed line) is available.
Paper: A Visibility-based 21 cm Bispectrum Estimator for Radio-interferometric Data
Authors: Sukhdeep Singh Gill, Somnath Bharadwaj
Figure caption: The left column shows the estimated 3D BS monopole ﹩\bar{B}({k}_{1},\mu ,t)﹩ as a function of (μ, t) at fixed k1 = 0.078 Mpc−1. The allowed values of (μ, t), which quantifies the triangle shape, satisfy the constraint 2 μt ≥ 1, indicated by a black dashed line. The right panels show the corresponding ﹩{{\rm{\Delta }}}_{B}=| \bar{B}-{[\bar{B}]}_{d}| /{[\bar{B}]}_{d}﹩, which quantifies the fractional deviations relative to ﹩{[\bar{B}]}_{d}﹩ the analytical predictions. Here, μ and t, respectively, vary along the horizontal and vertical directions, exactly as in Figure 5.
Paper: A Visibility-based 21 cm Bispectrum Estimator for Radio-interferometric Data
Authors: Sukhdeep Singh Gill, Somnath Bharadwaj
Figure caption: Same as Figure 7, but with flagging.
Paper: On the Orbital Evolution of Multiple Wide Super-Jupiters: How Disk Migration and Dispersal Shape the Stability of the PDS 70 System
Authors: Clarissa R. Do Ó, Jaehan Bae, Quinn M. Konopacky, Jayke S. Nguyen, Patrick Diamond, Krzysztof Goździewski, Dawid Jankowski
Figure caption: Resonant structure of the system for the case where Mc = 4 MJup (top panel) and Mc = 10 MJup (bottom panel). Shaded red regions correspond to semianalytical resonance widths obtained with the algorithm proposed by T. Gallardo et al. (2021). Purple zones correspond to numerically stable regions, where the system is expected to remain dynamically stable for 1 Myr in our numerical simulations within this parameter space. The FARGO output is marked in a black and white circle. Numbered points correspond to initial conditions for which libration of the critical angle was tested for the 2:1 resonance. Green points correspond to initial conditions with libration of one of the critical angles, while orange points correspond to libration mixed with circulation of all critical angles. The Reversibility Error Method (REM) integrations were conducted for 10,000 outermost periods, and in the rectangular, shaded region in the lower plot, for 500,000 outer orbits. White contours represent semiamplitude of the critical angle θ for the inner planet. Note that contours for large semiamplitudes reaching 180° tend to be steep beyond ≃100°.
Paper: On the Orbital Evolution of Multiple Wide Super-Jupiters: How Disk Migration and Dispersal Shape the Stability of the PDS 70 System
Authors: Clarissa R. Do Ó, Jaehan Bae, Quinn M. Konopacky, Jayke S. Nguyen, Patrick Diamond, Krzysztof Goździewski, Dawid Jankowski
Figure caption: Evolution of the system using the MEGNO chaos indicator. For stable configurations, the value must converge to ≃2. The different panels show the MEGNO evolution for different disk photoevaporation rates κ (different columns) and planet c masses Mc (top row) and viscosity parameter α (bottom row).
Paper: On the Orbital Evolution of Multiple Wide Super-Jupiters: How Disk Migration and Dispersal Shape the Stability of the PDS 70 System
Authors: Clarissa R. Do Ó, Jaehan Bae, Quinn M. Konopacky, Jayke S. Nguyen, Patrick Diamond, Krzysztof Goździewski, Dawid Jankowski
Figure caption: Planet parameter evolution for PDS 70 b, c, and “d” in a photoevaporating disk with ﹩\kappa =\frac{1}{10}﹩ (left) and κ = 1 (right). The planets get locked into a Laplace resonance within 0.1 Myr for ﹩\kappa =\frac{1}{10}﹩, but fail to migrate fully into the resonance for κ = 1.
Paper: On the Orbital Evolution of Multiple Wide Super-Jupiters: How Disk Migration and Dispersal Shape the Stability of the PDS 70 System
Authors: Clarissa R. Do Ó, Jaehan Bae, Quinn M. Konopacky, Jayke S. Nguyen, Patrick Diamond, Krzysztof Goździewski, Dawid Jankowski
Figure caption: Final migration contour of the inner planet (left panel) and outer planet (right panel), as a function of photoevaporation rate κ (x-axis) and mass of the outer planet Mc (y-axis).
Paper: On the Orbital Evolution of Multiple Wide Super-Jupiters: How Disk Migration and Dispersal Shape the Stability of the PDS 70 System
Authors: Clarissa R. Do Ó, Jaehan Bae, Quinn M. Konopacky, Jayke S. Nguyen, Patrick Diamond, Krzysztof Goździewski, Dawid Jankowski
Figure caption: Evolution of the system’s period ratio. The different panels show the period ratio evolution for different disk photoevaporation rates κ (different columns) and planet c masses Mc (top row) and α (bottom row).
Paper: On the Orbital Evolution of Multiple Wide Super-Jupiters: How Disk Migration and Dispersal Shape the Stability of the PDS 70 System
Authors: Clarissa R. Do Ó, Jaehan Bae, Quinn M. Konopacky, Jayke S. Nguyen, Patrick Diamond, Krzysztof Goździewski, Dawid Jankowski
Figure caption: Minimum period ratio timescales for each case divided by the disk lifetimes. We find that the system is less likely to meet the center of the resonance location before the disk dissipates if these timescales are comparable, which shows why the resonance locking is stronger if the disk is present for a longer time.
Paper: On the Orbital Evolution of Multiple Wide Super-Jupiters: How Disk Migration and Dispersal Shape the Stability of the PDS 70 System
Authors: Clarissa R. Do Ó, Jaehan Bae, Quinn M. Konopacky, Jayke S. Nguyen, Patrick Diamond, Krzysztof Goździewski, Dawid Jankowski
Figure caption: Contour plot of the migration of PDS 70 b (left) and c (right) as a function of disk photoevaporation rate κ and viscosity parameter α. Red colors represent outward migration while blue colors represent inward migration. Very small migration values, near 0, appear gray. In this simulation, the mass of planet c was set to 4 MJup.
Paper: On the Orbital Evolution of Multiple Wide Super-Jupiters: How Disk Migration and Dispersal Shape the Stability of the PDS 70 System
Authors: Clarissa R. Do Ó, Jaehan Bae, Quinn M. Konopacky, Jayke S. Nguyen, Patrick Diamond, Krzysztof Goździewski, Dawid Jankowski
Figure caption: Disk density for different α and κ values at t ∼ 0.6 Myr. Note how the gap is not as deep for larger α, while it is significantly depleted for smaller α. In the κ = 1/10 case, the gap depth varies by about 3 orders of magnitude.
Paper: On the Orbital Evolution of Multiple Wide Super-Jupiters: How Disk Migration and Dispersal Shape the Stability of the PDS 70 System
Authors: Clarissa R. Do Ó, Jaehan Bae, Quinn M. Konopacky, Jayke S. Nguyen, Patrick Diamond, Krzysztof Goździewski, Dawid Jankowski
Figure caption: Evolution of the planets’ b and c orbits over 5 Myr (κ = 1, ﹩\frac{1}{10}﹩) and 2 Myr (κ = 1, 10) under different photoevaporation rates κ for the protoplanetary disk. Here, Mc is set to 4 MJup and α is set to 0.
Paper: On the Orbital Evolution of Multiple Wide Super-Jupiters: How Disk Migration and Dispersal Shape the Stability of the PDS 70 System
Authors: Clarissa R. Do Ó, Jaehan Bae, Quinn M. Konopacky, Jayke S. Nguyen, Patrick Diamond, Krzysztof Goździewski, Dawid Jankowski
Figure caption: Same as Figure 7, but with α set to 10−2.
Paper: On the Orbital Evolution of Multiple Wide Super-Jupiters: How Disk Migration and Dispersal Shape the Stability of the PDS 70 System
Authors: Clarissa R. Do Ó, Jaehan Bae, Quinn M. Konopacky, Jayke S. Nguyen, Patrick Diamond, Krzysztof Goździewski, Dawid Jankowski
Figure caption: Demonstration of the convergence of MEGNO to the value of ∼2 for a regular (stable) system, which is what we find in our hydrodynamic simulation outputs. For chaotic systems, we can calculate the Lyapunov timescale using the slope of the MEGNO evolution line. We find in this case that increasing the eccentricity of the outer planet by just 0.03 (from 0.06 to 0.09) leads to a chaotic solution, where the Lyapunov timescale is ∼90,000 yr.
Paper: On the Orbital Evolution of Multiple Wide Super-Jupiters: How Disk Migration and Dispersal Shape the Stability of the PDS 70 System
Authors: Clarissa R. Do Ó, Jaehan Bae, Quinn M. Konopacky, Jayke S. Nguyen, Patrick Diamond, Krzysztof Goździewski, Dawid Jankowski
Figure caption: Histograms show the posteriors in the orbit fit that remain stable for 100 Myr timescales. Top: coplanar case, where 4.2%–4.5% of cases are stable. The semimajor axis of b and c (left and middle) lead to a period ratio between ∼2 and 3 for both planets (right panel). Bottom: non-coplanar case, where 0.7%–0.9% of configurations are stable. The semimajor axis values for b and c lead to stable configurations that favor period ratios between 2 and 6 (right panel), which is significantly different from our FARGO outputs.
Paper: On the Orbital Evolution of Multiple Wide Super-Jupiters: How Disk Migration and Dispersal Shape the Stability of the PDS 70 System
Authors: Clarissa R. Do Ó, Jaehan Bae, Quinn M. Konopacky, Jayke S. Nguyen, Patrick Diamond, Krzysztof Goździewski, Dawid Jankowski
Figure caption: Orbit plots for the unconstrained (left) and coplanar (right) for PDS 70 b and c. The top image traces 100 possible orbits on the plane of the sky, while the bottom images’ panels represent the separation (sep; in mas), position angle (PA; in degrees), and relative radial velocities (RVs; in km s−1) as a function of epoch (in MJD) for both planets. Planet b’s fits are shown in orange, while planet c’s fits are shown in blue.
Paper: On the Orbital Evolution of Multiple Wide Super-Jupiters: How Disk Migration and Dispersal Shape the Stability of the PDS 70 System
Authors: Clarissa R. Do Ó, Jaehan Bae, Quinn M. Konopacky, Jayke S. Nguyen, Patrick Diamond, Krzysztof Goździewski, Dawid Jankowski
Figure caption: Orbit plots for the unconstrained (left) and coplanar (right) for PDS 70 b, c, and d. The top image traces 100 possible orbits on the plane of the sky, while the bottom images’ panels represent the separation (sep; in mas), position angle (PA; in degrees), and relative radial velocities (RVs; in km s−1) as a function of epoch (in MJD) for all planets. Planet b’s fits are shown in orange, while planet c’s fits are shown in blue and planet d’s fits are shown in green.
Paper: On the Orbital Evolution of Multiple Wide Super-Jupiters: How Disk Migration and Dispersal Shape the Stability of the PDS 70 System
Authors: Clarissa R. Do Ó, Jaehan Bae, Quinn M. Konopacky, Jayke S. Nguyen, Patrick Diamond, Krzysztof Goździewski, Dawid Jankowski
Figure caption: The PDS 70 b, c, and d orbital evolution for ﹩\kappa =\frac{1}{10}﹩ and κ = 1. The system becomes unstable, with ejections and scattering, in the higher photoevaporation case where the planets do not have enough time to migrate to the center of the MMR before the disk dissipates.
Paper: On the Orbital Evolution of Multiple Wide Super-Jupiters: How Disk Migration and Dispersal Shape the Stability of the PDS 70 System
Authors: Clarissa R. Do Ó, Jaehan Bae, Quinn M. Konopacky, Jayke S. Nguyen, Patrick Diamond, Krzysztof Goździewski, Dawid Jankowski
Figure caption: Comparison of the 2D density for the disk at t ∼ 0.6 Myr for different κ values. The planets’ Hill circles are marked in yellow.