adsabs/AstroCLIMB huggingface dataset:
Paper: Large-scale Spatial Cross-calibration of Hinode/SOT-SP and SDO/HMI
Authors: David F. Fouhey, Richard E. L. Higgins, Spiro K. Antiochos, Graham Barnes, Marc L. DeRosa, J. Todd Hoeksema, K. D. Leka, Yang Liu, Peter W. Schuck, Tamas I. Gombosi
Figure caption: Warped data and pointing coordinates. We show a subset of the maps for conciseness, including flux density (α B) and continuum intensity and coordinate maps and disk masks. Coordinates shown for fit values that are produced by the fit alignment with SDO/HMI and reported values that are reported in the Level 2 Hinode/SOT-SP data. The reported values show substantial disagreement with SDO/HMI data even though the alignment of continuum and field strength are close to pixel-perfect. This is most clear by examining the limb pixels on bottom. In comparison, our fit corrections align well. Top: 2011 April 30, 09:55:06 TAI. Bottom: 2013 April 3, 15:47:05 TAI.
Paper: Large-scale Spatial Cross-calibration of Hinode/SOT-SP and SDO/HMI
Authors: David F. Fouhey, Richard E. L. Higgins, Spiro K. Antiochos, Graham Barnes, Marc L. DeRosa, J. Todd Hoeksema, K. D. Leka, Yang Liu, Peter W. Schuck, Tamas I. Gombosi
Figure caption: Pointing update prediction performance. We plot the cross-validated predictions of ΔXCEN, ΔYCEN against the values fit by alignment. This plot shows the density of the region, estimated with a kernel density estimate. The predicted values are generally quite accurate. Approximately 2% of data are outliers and are not shown. Density color map: Min  Max.
Paper: Large-scale Spatial Cross-calibration of Hinode/SOT-SP and SDO/HMI
Authors: David F. Fouhey, Richard E. L. Higgins, Spiro K. Antiochos, Graham Barnes, Marc L. DeRosa, J. Todd Hoeksema, K. D. Leka, Yang Liu, Peter W. Schuck, Tamas I. Gombosi
Figure caption: Plots of ΔXCEN and ΔYCEN as a function of XCEN and YCEN locations. For each location, we plot the averaged ΔXCEN (left) and ΔYCEN (right) per location. Color map: −50″  50″. There is a strong positive bias, as indicated by the uniformly red color.
Paper: TESS Timings of 31 Hot Jupiters with Ephemeris Uncertainties
Authors: Su-Su Shan, Fan Yang, You-Jun Lu, Xing Wei, Wen-Wu Tian, Hai-Yan Zhang, Rui Guo, Xiao-Hong Cui, Ai-Yuan Yang, Bo Zhang, Ji-Feng Liu
Figure caption: TESS example images of 14 × 14 pixels. The images correspond to HAT-P-31b, HAT-P-35b, and WASP-56b, from top to bottom. The blue points refer to the planet position in the Gaia catalog (Gaia Collaboration et al. 2018) while red points present nearby source positions.
Paper: TESS Timings of 31 Hot Jupiters with Ephemeris Uncertainties
Authors: Su-Su Shan, Fan Yang, You-Jun Lu, Xing Wei, Wen-Wu Tian, Hai-Yan Zhang, Rui Guo, Xiao-Hong Cui, Ai-Yuan Yang, Bo Zhang, Ji-Feng Liu
Figure caption: Light curves of KELT-19Ab as an example: a single epoch around TOI timing (top panel), folded multiple visits at a reference epoch (bottom panel). The blue points present observations (10 minute cadence) while the green points are bins of every three points for clarity. The red line gives the transit model fit with the yellow region indicating the 1σ confidence region. The vertical blue line gives the fitted timing; the black vertical line, TOI timing; the green vertical line, previous ephemeris prediction. The timings from single-epoch fitting (folded-epoch fitting) are only 0.14 minutes earlier (0.20 minutes later) than TOI, corresponding to a negligible difference as shown in the image (overlapped blue and black lines). The observed TESS timings show an offset of ∼15 minutes, compared to the previous ephemeris prediction as shown in the vertical green line. The fitting uncertainty is 0.54 minutes for a single epoch, and 0.23 minutes for folded epochs.
Paper: TESS Timings of 31 Hot Jupiters with Ephemeris Uncertainties
Authors: Su-Su Shan, Fan Yang, You-Jun Lu, Xing Wei, Wen-Wu Tian, Hai-Yan Zhang, Rui Guo, Xiao-Hong Cui, Ai-Yuan Yang, Bo Zhang, Ji-Feng Liu
Figure caption: The timing difference of HAT-P-31b. The timing difference is the observed midtransit times minus the ephemeris predictions. The red point refers to the TESS timing difference, black points refer to timing differences of other observations from the literature (Kipping et al. 2011; Mallonn et al. 2019), the black dashed line is the reference ephemeris, the blue line is an alternative reference ephemeris, the red line is the refined ephemeris derived by combining TESS observations, the green region is a 1σ significant region of reference ephemeris, and the brown region is a 1σ significant region of alternative reference ephemeris. We note that our refined ephemeris overlaps the alternative reference ephemeris, indicating the consistency of the two ephemerides.
Paper: TESS Timings of 31 Hot Jupiters with Ephemeris Uncertainties
Authors: Su-Su Shan, Fan Yang, You-Jun Lu, Xing Wei, Wen-Wu Tian, Hai-Yan Zhang, Rui Guo, Xiao-Hong Cui, Ai-Yuan Yang, Bo Zhang, Ji-Feng Liu
Figure caption: The timing differences with corrected timings for WASP-173Ab, TOI-1333b, and TOI-628b. The symbols are similar to Figure 3. The green diamonds indicate TOI timing and the red diamonds give the timing generated from TESS raw images.
Paper: TESS Timings of 31 Hot Jupiters with Ephemeris Uncertainties
Authors: Su-Su Shan, Fan Yang, You-Jun Lu, Xing Wei, Wen-Wu Tian, Hai-Yan Zhang, Rui Guo, Xiao-Hong Cui, Ai-Yuan Yang, Bo Zhang, Ji-Feng Liu
Figure caption: KELT-19Ab timings fitted with a quadratic function. The symbols are similar to Figure 3. The red line shows the quadratic function model.
Paper: TESS Timings of 31 Hot Jupiters with Ephemeris Uncertainties
Authors: Su-Su Shan, Fan Yang, You-Jun Lu, Xing Wei, Wen-Wu Tian, Hai-Yan Zhang, Rui Guo, Xiao-Hong Cui, Ai-Yuan Yang, Bo Zhang, Ji-Feng Liu
Figure caption: Timing differences of Type II targets of which timings would be modeled by a quadratic function.
Paper: POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations
Authors: Tassos Fragos, Jeff  J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Román-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, Michael Zevin
Figure caption: View of two grid slices, for two different values of initial binary mass ratio (q = 0.3 on the left, q = 0.7 on the right), from our grid of binary-star models consisting of two H-rich stars, initially at ZAMS. The different symbols summarize the evolution of each of the models. We distinguish between models that experienced stable or no mass transfer (squares), reaching the end of the life of one of the stars, and the ones that stopped during mass transfer due to one of our conditions for dynamical instability (diamonds). Different colors distinguish the evolutionary phase of the donor star during the latest episode of mass transfer (or no RLO at all for gray). Small black dots at low initial periods depict systems that were in initial RLO at birth and red diamonds represent the models that stopped prematurely for numerical reasons.
Paper: POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations
Authors: Tassos Fragos, Jeff  J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Román-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, Michael Zevin
Figure caption: View of two slices, for two different values of initial CO masses (M CO = 1.43 M ⊙ on the left, M CO = 14.66 M ⊙ on the right), from our grid of binary-star models consisting of an H-rich star and a CO at the onset of RLO. The different symbols summarize the evolution of each of the models, as in Figure 9. Binaries that never initiated mass transfer are not shown here.
Paper: POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations
Authors: Tassos Fragos, Jeff  J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Román-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, Michael Zevin
Figure caption: Relative increase in the mass of the CO (M CO,f − M CO,i)/M CO,i due to accretion for systems where the nondegenerate star reached the end of its life. The grid slices are the same as shown in Figure 11. Although accretion is Eddington-limited, COs in binaries with pre-RLO mass ratios in the range q ∼ 1–2 (defining q = M CO,i/M 1,i) and short initial periods, which will experience long-duration mass-transfer phases, manage to accrete a significant amount of mass.
Paper: POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations
Authors: Tassos Fragos, Jeff  J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Román-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, Michael Zevin
Figure caption: For the same grid slices shown in Figure 9, and only for systems where one of the two stars reached the end of its life, we depict the final ratio of the angular velocity of the secondary star (the initially less massive) divided by its critical rotation rate, ﹩{({\omega }_{{\rm{s}}}/{\omega }_{{\rm{s}},\mathrm{crit}})}_{2}﹩. In most cases where mass transfer occurred, the secondary star accreted mass and spun up, remaining highly spinning until the end of the life of the initially more-massive star.
Paper: POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations
Authors: Tassos Fragos, Jeff  J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Román-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, Michael Zevin
Figure caption: Evolution of radius for He stars with masses between 2 and 10 M ⊙. Less-massive He stars evolve slower, but expand farther when they become giant stars. This trend implies that more-massive He stars in binary systems will undergo RLO for a relatively narrow range of orbital periods, a behavior exhibited by our binary star simulations and seen in Figure 14.
Paper: POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations
Authors: Tassos Fragos, Jeff  J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Román-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, Michael Zevin
Figure caption: Comparison of the final C/O core mass in SSE as implemented by COSMIC (magenta), MIST (green), and POSYDON (blue). Differences between MIST and POSYDON are due to the larger core overshoot parameter adopted by POSYDON. Disagreement with the SSE models is expected as these models are based on simulations that were only computed for initial masses up to 50 M ⊙; more-massive stars are an extrapolation.
Paper: POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations
Authors: Tassos Fragos, Jeff  J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Román-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, Michael Zevin
Figure caption: Final masses of the POSYDON and Woosley (2019) single He-star evolution models. Differences at M initial ≳ 20 M ⊙ are due to the stronger wind mass-loss prescription adopted by POSYDON.
Paper: POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations
Authors: Tassos Fragos, Jeff  J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Román-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, Michael Zevin
Figure caption: Hertzsprung–Russell diagram of a subsample of POSYDON single-stellar models where the different POSYDON stellar states are indicated according to the legend.
Paper: POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations
Authors: Tassos Fragos, Jeff  J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Román-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, Michael Zevin
Figure caption: Lifetimes of the POSYDON and Woosley (2019) single He-star evolution models match to within ≃0.1 dex.
Paper: POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations
Authors: Tassos Fragos, Jeff  J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Román-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, Michael Zevin
Figure caption: Interpolation scheme accuracy for 10 selected parameters when applied to our grid of two H-rich stars, as calculated using our set of validation binaries. We separate our sample by their different mass-transfer histories to independently evaluate their individual accuracy. Median relative errors (e r) indicated by the horizontal lines in each distribution are typically 1% or lower for the stable mass-transfer and unstable mass-transfer cases (top panel) and the no mass-transfer case (green; bottom panel). Improving this accuracy will be a focus of future work.
Paper: POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations
Authors: Tassos Fragos, Jeff  J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Román-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, Michael Zevin
Figure caption: The interpolation accuracy for the same 10 parameters as in Figures 24 and 25, but for our grid of He stars with CO companions. As with our other two grids, this grid has typical median errors below 1%; however, tails of the distribution extend toward larger e r, especially for the stable mass-transfer and unstable mass-transfer cases (top panel). Our no mass-transfer case (bottom panel) is much more accurate than the corresponding binaries in our grid of two H-rich stars in Figure 24. The apparent truncations in the distributions (e.g., M C/O-core, 1 and ﹩{\mathrm{log}}_{10}({J}_{1})﹩) are genuine representations of the data.
Paper: POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations
Authors: Tassos Fragos, Jeff  J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Román-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, Michael Zevin
Figure caption: Confusion matrices for each of our three binary grids. Each value at grid cell c  ij  represents the fraction of binaries that belong to class j (vertical axis) and were classified as class i (horizontal axis). Each row is normalized so that the sum of each row is 1, and the color of each cell indicates the magnitude of the value in the cell. Accuracies are all above 90%, with the exception of unstable mass transfer for the He-rich star with a CO companion.
Paper: POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations
Authors: Tassos Fragos, Jeff  J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Román-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, Michael Zevin
Figure caption: The interpolation accuracy for the same 10 parameters as in Figure 24 for our grid of H-rich stars with a CO companion. Since we never use the models from this grid that do not undergo RLO, we do not evaluate the no mass-transfer binaries. In most cases, typical errors are 1% or better, but several of the distributions have tails extending toward larger e r.
Paper: POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations
Authors: Tassos Fragos, Jeff  J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Román-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, Michael Zevin
Figure caption: Distributions of the difference between the matching point of a single-star model in the beginning of the detached step and the values from the previous step, for various physical quantities of a nondegenerate star. We show the relative difference in mass ΔM, He-core mass ﹩{\rm{\Delta }}{M}_{\mathrm{He}-\mathrm{core}}﹩, and logarithm of the radius ﹩{\rm{\Delta }}{\mathrm{log}}_{10}(R/{R}_{\odot })﹩, as well as the difference in the He central and surface abundances Y center and Y surf, respectively. Vertical, dashed lines from left to right delineate the 5th and 95th percentiles of the distributions. The distributions all suggest that the nondegenerate stars in detached binaries can be accurately matched to a single-star model.
Paper: POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations
Authors: Tassos Fragos, Jeff  J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Román-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, Michael Zevin
Figure caption: The convective envelope radius R conv.reg. and width D conv.reg. need to simultaneously agree with three separate inequalities defined in Table 8. The feasibility region (dark gray) represents the overlap of all three inequalities decomposed from the constraint. When our interpolation method proposed a point outside the feasibility region, we reassign it to a new point determined from the intersection of the border of the feasibility region and the line drawn from the centroid of the region to the constraint-violating, proposed point.
Paper: POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations
Authors: Tassos Fragos, Jeff  J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Román-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, Michael Zevin
Figure caption: The core-collapse type for the q = 0.7 slice of our binary-star model grid composed of two H-rich stars. We distinguish between WD formation, electron caption SN (ECSN) following Podsiadlowski et al. (2005), CCSN, and pair-pulsational instability SN (PPISN) following Marchant et al. (2019). Models that did not reach the end of stellar evolution are indicated in black.
Paper: POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations
Authors: Tassos Fragos, Jeff  J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Román-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, Michael Zevin
Figure caption: Evolution of λ CE parameter of POSYDON single-star models of different initial masses. For these calculations, the assumed core–envelope boundary is located at the point where the H mass fraction drops below 10%. The triangle, diamond, and star markers represent the start of shell H-burning, the start of core He-burning, and the end of core He-burning, respectively.
Paper: POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations
Authors: Tassos Fragos, Jeff  J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Román-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, Michael Zevin
Figure caption: The CO state for the q = 0.7 grid slice of HMS–HMS MESA simulations in the initial primary mass–orbital period plane. We distinguish between the COs: white dwarf (WD), neutron star (NS), and black hole (BH) according to the legend. Models that did not reach the end of the stellar evolution are indicated in black. The two panels compare the Fryer et al. (2012) delayed core-collapse mechanism (left) with the outcome of Patton & Sukhbold (2020) N20 core-collapse engine (right).
Paper: Large-scale Spatial Cross-calibration of Hinode/SOT-SP and SDO/HMI
Authors: David F. Fouhey, Richard E. L. Higgins, Spiro K. Antiochos, Graham Barnes, Marc L. DeRosa, J. Todd Hoeksema, K. D. Leka, Yang Liu, Peter W. Schuck, Tamas I. Gombosi
Figure caption: Fit scales by location. We plot a kernel regression estimate of the location, with a prior of 1. We also plot the density. The apparent bias in density toward one side of the disk is driven by the Hinode/SOT-SP observing cycle: an active region needs to have become previously visible in order for Hinode/SOT-SP to have it selected as a target. The corrections also have no trend (although there are some outliers), suggesting that the location-dependent causes such as differences in line formation height are not responsible for the change in scale.