adsabs/AstroCLIMB huggingface dataset:
Paper: Ubiquitous Occurrences of Multiscale Layers of Magnetic Reconnection across a Solar Wind Stream Interaction Region at 1 au
Authors: S. Eriksson, A. Chasapis, A. Mallet, M. Swisdak
Figure caption: Wind satellite observations on 2019 January 1–9: (a) B, (b) BzGSE, (c) azimuthal φB angle of ecliptic plane BGSE, (d) V, (e) Np, (f) Tp, (g) ratio of parallel to antiparallel 165 eV electron strahl energy flux, and (h) total number of obtained reconnection exhaust events in subsequent 6 hr periods with time stamps at the center of each period (03 UT for 00–06 UT interval). Vertical lines mark exhaust topt times for all 71 exhausts with color representing CS normal width from thin (blue) to thick (red). See Table 1 for color definitions. The eight days totaled 7, 2, 5, 39, 12, 3, 3, and 0 jets, respectively.
Paper: Ubiquitous Occurrences of Multiscale Layers of Magnetic Reconnection across a Solar Wind Stream Interaction Region at 1 au
Authors: S. Eriksson, A. Chasapis, A. Mallet, M. Swisdak
Figure caption: Spherical angle coordinates (azimuth 0° < φ < 360° and polar 0° < θ < 180°) corresponding to CS normal vectors NGSE for 71 exhaust events on 2019 January 1–9 (top). CS normal width (dcs) histogram (bottom left) and magnetic field shear θB-angle histogram (bottom right). Here, θB is obtained immediately adjacent to each CS using average magnetic fields in LMN also available in an ascii text file at doi:10.5281/zenodo.15367694.
Paper: Ubiquitous Occurrences of Multiscale Layers of Magnetic Reconnection across a Solar Wind Stream Interaction Region at 1 au
Authors: S. Eriksson, A. Chasapis, A. Mallet, M. Swisdak
Figure caption: Two magnetic reconnection VL exhaust cases within a shocked slow wind (case A) and a shocked fast wind (case B). Panels from the top display: Np, Tp, BL, VL (measured in black; predicted in red), BM, and BN. Data around case A cover 2019 January 4 10:45:09–11:42:39 UT. Data around case B cover 2019 January 5 00:50:46–01:01:46 UT. Solid green lines correspond to an optimum time (topt) between two Walén predictions from the leading and trailing sides of the CS with start and stop times shown as dotted vertical lines. topt times and LMN unit vectors are available at doi:10.5281/zenodo.15367694.
Paper: Binary Stars Take What They Get: Evidence for Efficient Mass Transfer from Stripped Stars with Rapidly Rotating Companions
Authors: Thibault Lechien, Selma E. de Mink, Ruggero Valli, Amanda C. Rubio, Lieke A. C. van Son, Robert Klement, Harim Jin, Onno Pols
Figure caption: Like Figure 4 but assuming complete stripping of the envelope (using Equation (B1)) and varying the assumptions of AM loss: (a) assuming isotropic reemission of the nonaccreted mass; (b) assuming 10% of the transferred mass is sent to a circumbinary disk and the rest of the nonaccreted mass is reemitted isotropically; and (c) assuming 20% of the transferred mass is sent to a circumbinary disk and the rest of the nonaccreted mass is reemitted isotropically.
Paper: Discovery of Hα Emission from a Protoplanet Candidate around the Young Star 2MASS J16120668–3010270 with MagAO-X
Authors: Jialin Li, 嘉霖 李, Laird M. Close, Feng Long, 凤 龙, Jared R. Males, Sebastiaan Y. Haffert, Alycia Weinberger, Katherine Follette, Sean Andrews, John Carpenter, Warren B. Foster, Kyle Van Gorkom, Alexander D. Hedglen, Gregory J. Herczeg, 雷歌 沈, Parker T. Johnson, Maggie Y. Kautz, Jay K. Kueny, Rixin Li, Joshua Liberman, Joseph D. Long, Jennifer Lumbres, Sebastian Marino, Luca Matrà, Eden A. McEwen, Olivier Guyon, Logan A. Pearce, Laura M. Pérez, Paola Pinilla, Lauren Schatz, Yangfan Shi, Katie Twitchell, Kevin Wagner, David Wilner, Ya-Lin Wu, Shangjia Zhang, 尚嘉 张, Zhaohuan Zhu
Figure caption: Corner plot of the orbit fitting using both the astrometric points from the SPHERE/IRDIS K-band observation and the MagAO-X Hα SDI observations in 2025. The purple lines represent the median value of each parameter of the 10,000 accepted orbits.
Paper: Discovery of Hα Emission from a Protoplanet Candidate around the Young Star 2MASS J16120668–3010270 with MagAO-X
Authors: Jialin Li, 嘉霖 李, Laird M. Close, Feng Long, 凤 龙, Jared R. Males, Sebastiaan Y. Haffert, Alycia Weinberger, Katherine Follette, Sean Andrews, John Carpenter, Warren B. Foster, Kyle Van Gorkom, Alexander D. Hedglen, Gregory J. Herczeg, 雷歌 沈, Parker T. Johnson, Maggie Y. Kautz, Jay K. Kueny, Rixin Li, Joshua Liberman, Joseph D. Long, Jennifer Lumbres, Sebastian Marino, Luca Matrà, Eden A. McEwen, Olivier Guyon, Logan A. Pearce, Laura M. Pérez, Paola Pinilla, Lauren Schatz, Yangfan Shi, Katie Twitchell, Kevin Wagner, David Wilner, Ya-Lin Wu, Shangjia Zhang, 尚嘉 张, Zhaohuan Zhu
Figure caption: The ALMA 1.3 mm data, frank model, and residual images of the disk around J1612, restored with the same tclean beam. The rightmost panel shows the radial intensity profile derived from the frank model (dashed curve) and cleaned data image (solid curve).
Paper: Black Hole Survival Guide: Searching for Stars in the Galactic Center that Endure Partial Tidal Disruption
Authors: Rewa Clark Bush, Samantha C. Wu, Rosa Wallace Everson, Ricardo Yarza, Ariadna Murguia-Berthier, Enrico Ramirez-Ruiz
Figure caption: Left panel: density profile of the remnant at several points in time after a β = 1 encounter. During the encounter, the star becomes more diffuse and forms an extended envelope. This envelope contracts over the course of its own Kelvin–Helmholtz time. Right panel: radius and luminosity as a function of time for the first 105 yr postdisruption. The dashed lines correspond to a simplified model of a contracting polytropic envelope (see text), and the solid lines are MESA output. The rough agreement between the models supports the idea that the early “transient” evolution of the remnant corresponds to the contraction of an extended envelope that formed during the disruption as a result of energy deposition close to the surface of the star.
Paper: The Potential Danger to Satellites due to Ejecta from a 2032 Lunar Impact by Asteroid 2024 YR4
Authors: Paul Wiegert, Peter Brown, Jack Lopes, Martin Connors
Figure caption: A map of the Moon showing randomly selected impact locations colored by the fraction of escaping ejecta delivered to Earth within 100 days. The current impact corridor for 2024 YR4 is shown in yellow, with the specific impact locations examined more closely in Section 4.2 labeled as clones A-D. See Sections 4.1 and 4.2 of the main text for more details.
Paper: The Potential Danger to Satellites due to Ejecta from a 2032 Lunar Impact by Asteroid 2024 YR4
Authors: Paul Wiegert, Peter Brown, Jack Lopes, Martin Connors
Figure caption: The current impact corridor for 2024 YR4 (yellow) projected on a map of the Moon’s near side from LRO (E. J. Speyerer et al. 2011).
Paper: The Potential Danger to Satellites due to Ejecta from a 2032 Lunar Impact by Asteroid 2024 YR4
Authors: Paul Wiegert, Peter Brown, Jack Lopes, Martin Connors
Figure caption: An elevation map of the Moon showing the locations of clones A through D selected for a more detailed study of their delivery efficiencies. See Section 4.2 of the main text for more details.
Paper: Carbon-rich Sub-Neptune Interiors Are Compatible with JWST Observations
Authors: Zifan Lin, Sara Seager
Figure caption: Possible interior compositions of TOI-270 d. Compositions consistent within the 1σ, 2σ, and 3σ M–R uncertainties are shown in orange, dark teal, and light teal, respectively. The red dashed and solid lines show xcarbon = 12 wt% and 24 wt%, respectively, which are the upper bounds of xcarbon assuming no volatile loss (E. A. Bergin et al. 2023). xcarbon defines the bulk carbon content of the planet and in turn defines the C/O ratio in the atmosphere, under the assumption that the atmospheric C/O ratio is the same as the bulk solid C/O ratio. (a) Carbon-envelope diagram for a 1 times solar metallicity envelope. (b) Ternary diagram for a 100 times solar metallicity envelope. (c) Ternary diagram for a 1000 times solar metallicity envelope. The 100 times solar metallicity scenario allows the widest range of interior compositions and is broadly consistent with the metallicity retrieved by B. Benneke et al. (2024).
Paper: Carbon-rich Sub-Neptune Interiors Are Compatible with JWST Observations
Authors: Zifan Lin, Sara Seager
Figure caption: Possible interior compositions of K2-18 b. Compositions consistent within the 1σ, 2σ, and 3σ M–R uncertainties are shown in orange, dark teal, and light teal, respectively. The red dashed and solid lines show xcarbon = 12 wt% and 24 wt%, respectively, which are the upper bounds of xcarbon assuming no volatile loss (E. A. Bergin et al. 2023). xcarbon defines the bulk carbon content of the planet and in turn defines the C/O ratio in the atmosphere, under the assumption that the atmospheric C/O ratio is the same as the bulk solid C/O ratio. Ternary diagrams are shown for: (a) a 1 times solar metallicity envelope scenario; (b) a 100 times solar metallicity envelope scenario; and (c) a 1000 times solar metallicity envelope scenario. The 100 times solar metallicity scenario allows the widest range of interior compositions and is consistent with previous modeling and retrieval works (N. F. Wogan et al. 2024; S. P. Schmidt et al. 2025).
Paper: Carbon-rich Sub-Neptune Interiors Are Compatible with JWST Observations
Authors: Zifan Lin, Sara Seager
Figure caption: (a) Simulated transmission spectra of sub-Neptune TOI-270 d compared with HST and JWST observations. The best-fit flat-line model, best-fit hazy model, and best-fit haze-free model are plotted, with their respective reduced ﹩{\chi }_{\nu }^{2}﹩ and σ values shown. Note that the HST/WFC3 data are shown for comparison, but the models are only fitted to the JWST data. The simulated spectra are allowed to shift, to account for baseline offsets between the different instruments/detectors. (b) Contributions to the overall transmission spectra by the individual molecules. A carbon-rich interior composition with a 100 times solar metallicity envelope is compatible with HST and JWST transmission spectra observations of TOI-270 d.
Paper: Carbon-rich Sub-Neptune Interiors Are Compatible with JWST Observations
Authors: Zifan Lin, Sara Seager
Figure caption: Possible interior compositions of 55 Cnc e. Compositions consistent within the 1σ, 2σ, and 3σ M–R uncertainties are shown in orange, dark teal, and light teal, respectively. The red dashed and solid lines show xcarbon = 12 wt% and 24 wt%, respectively, with the upper bounds of xcarbon assuming no volatile loss (E. A. Bergin et al. 2023). The blue curve shows the interior solution from N. Madhusudhan et al. (2012), to the right of which are the allowed values (1σ uncertainty). Ternary diagrams are shown for two radius assumptions—(a) a visible radius, 2.04 ± 0.15 R⊕, and (b) a gray radius, 2.20 ± 0.12 R⊕—following N. Madhusudhan et al. (2012). Our interior models with updated carbon and SiC EOSs are consistent with earlier studies.
Paper: Carbon-rich Sub-Neptune Interiors Are Compatible with JWST Observations
Authors: Zifan Lin, Sara Seager
Figure caption: (a) Simulated transmission spectra of sub-Neptune K2-18 b compared with HST and JWST observations. The best-fit flat-line model, best-fit 100 times solar metallicity model, and best-fit 1000 times solar metallicity model are shown. Note that the HST/WFC3 data are shown for comparison, but the models are only fitted to the JWST data. (b) Contributions to the overall transmission spectra by the individual molecules. The best-fit 100 times solar metallicity model is barely consistent with the data, while all other models are ruled out at >3σ. A high C/O ratio of 2.0 is favored, consistent with the retrieval work by S. P. Schmidt et al. (2025), which constrained the mixing ratio of CH4 to be ﹩{\mathrm{log}}\,({{\rm{CH}}}_{4})=-1.1{5}_{-0.52}^{+0.40}﹩. Additional CH4 and CO2 sources are needed to fully match the JWST observations.
Paper: Carbon-rich Sub-Neptune Interiors Are Compatible with JWST Observations
Authors: Zifan Lin, Sara Seager
Figure caption: Possible interior compositions of GJ 1214 b. Compositions consistent within the 1σ, 2σ, and 3σ M–R uncertainties are shown in orange, dark teal, and light teal, respectively. The red dashed and solid lines show xcarbon = 12 wt% and 24 wt%, respectively, which are the upper bounds of xcarbon assuming no volatile loss (E. A. Bergin et al. 2023). xcarbon defines the bulk carbon content of the planet and in turn defines the C/O ratio in the atmosphere, under the assumption that the atmospheric C/O ratio is the same as the bulk solid C/O ratio. (a) Carbon-envelope diagram for a 1 times solar metallicity envelope. (b) Ternary diagram for a 100 times solar metallicity envelope. The lack of a 1000 times solar metallicity solution rules out carbon-rich interiors for GJ 1214 b, because previous works favored high metallicities (see the text).
Paper: Carbon-rich Sub-Neptune Interiors Are Compatible with JWST Observations
Authors: Zifan Lin, Sara Seager
Figure caption: Mixing ratio profiles of the TOI-270 d atmosphere. The horizontal and vertical axes are the volume mixing ratio and pressure in log scales, respectively. Only five of the eight C/O ratio scenarios are shown, for clarity. The mixing ratios of reducing species (CH4 and NH3) monotonically increase as the C/O ratio increases, while the mixing ratios of oxidizing species (H2O and CO2) monotonically decrease. The CO concentration is roughly constant across all C/O ratios.
Paper: Carbon-rich Sub-Neptune Interiors Are Compatible with JWST Observations
Authors: Zifan Lin, Sara Seager
Figure caption: The same as Figure 7 but for GJ 1214 b.
Paper: Carbon-rich Sub-Neptune Interiors Are Compatible with JWST Observations
Authors: Zifan Lin, Sara Seager
Figure caption: The same as Figure 7 but for K2-18 b.
Paper: Binary Stars Take What They Get: Evidence for Efficient Mass Transfer from Stripped Stars with Rapidly Rotating Companions
Authors: Thibault Lechien, Selma E. de Mink, Ruggero Valli, Amanda C. Rubio, Lieke A. C. van Son, Robert Klement, Harim Jin, Onno Pols
Figure caption: Relationship between the initial mass and stripped-star mass. The solid black line (Relation (1)) shows the helium core mass derived from our grid of single-star MESA models, taken during the hydrogen-shell-burning phase. The light gray background shows the slight variation in the helium core mass during this phase. The helium core mass is defined as the mass coordinate where the hydrogen mass fraction drops below 0.1 and the helium mass fraction is above 0.1. The violin plots show the range of post-stripping masses in two large grids of early Case B binary MESA models (K. D. Temmink et al. 2023; H. Jin et al. 2025, in preparation), indicating that the helium core mass is a lower bound for the final mass of the stripped star. The dashed line (Relation (2)) shows the helium-core-mass relation, with an added 20% of the mass remaining, which is a good approximation of the incomplete stripping that occurs during Case B mass transfer.
Paper: Binary Stars Take What They Get: Evidence for Efficient Mass Transfer from Stripped Stars with Rapidly Rotating Companions
Authors: Thibault Lechien, Selma E. de Mink, Ruggero Valli, Amanda C. Rubio, Lieke A. C. van Son, Robert Klement, Harim Jin, Onno Pols
Figure caption: The systems in our sample are also in tension with predictions from the thermally limited model, as implemented in rapid population synthesis simulations. In the background, we show predictions for the fraction of accreted mass (β, color shading) as a function of the initial mass ratio and orbital separation. We overplot our best guess for the initial parameters for each observed system, which depend on the assumed β (indicated by color). Higher assumed values of β for the observed systems imply lower initial mass ratios, which is where this model predicts low β values and vice versa. The main region in this plot where the data and model predictions are consistent is marked in orange. We deem it unlikely that the vast majority of systems originate from such a narrow region and interpret this as tension with this model (which, here, we have taken from F. R. N. Schneider et al. 2015, their Figure 18, assuming a primary mass of 5 M⊙ as an illustration).
Paper: Binary Stars Take What They Get: Evidence for Efficient Mass Transfer from Stripped Stars with Rapidly Rotating Companions
Authors: Thibault Lechien, Selma E. de Mink, Ruggero Valli, Amanda C. Rubio, Lieke A. C. van Son, Robert Klement, Harim Jin, Onno Pols
Figure caption: Correlation between the constraints on the mass-transfer efficiency and current parameters (left) and inferred initial parameters (right). The lower bound refers to the minimum mass-transfer efficiency (βmin) that is inferred assuming the median observed masses and the conservative stripped-mass relation (Equation (B3)). The −1σ lower bound is based on the minimum mass-transfer efficiency that is inferred within the uncertainties on the observed masses. The statistically significant correlations—panels (c), (e), (g), and (h)—have a gray area in the background, indicating their trend line and the area of the parameter space that is ruled out by our lower bounds. The hashed areas in the initial-mass-ratio plots indicate where the donor was initially less massive than the accretor, which is not allowed. The mass ratio is defined here as q = Mdonor/Macc.  The hashed areas in the initial-period plots indicate Case A mass transfer.
Paper: Binary Stars Take What They Get: Evidence for Efficient Mass Transfer from Stripped Stars with Rapidly Rotating Companions
Authors: Thibault Lechien, Selma E. de Mink, Ruggero Valli, Amanda C. Rubio, Lieke A. C. van Son, Robert Klement, Harim Jin, Onno Pols
Figure caption: The inferred fractions of mass accreted for Be+sdOB binaries challenge theoretical predictions. The color bars in the main panel indicate the allowed ranges for β using our strict conservative assumptions. We use the median values for the observed masses but also show how the range increases when allowing for 1σ observational uncertainties. The black lines with triangles indicate our best-guess range, which uses a lower limit based on the median prediction of binary models and an upper limit to exclude systems that likely get into contact (see Section 2). The histograms in the top panel show theoretical predictions for early Case B mass transfer, adopting the rotationally limited approach (red; which is not consistent with most systems in our sample) and the thermally limited approach (orange; which is not ruled out here—however, see Figure 4). The first two systems marked in gray are likely the result of Case A mass transfer and cannot be directly compared with the predictions.
Paper: Binary Stars Take What They Get: Evidence for Efficient Mass Transfer from Stripped Stars with Rapidly Rotating Companions
Authors: Thibault Lechien, Selma E. de Mink, Ruggero Valli, Amanda C. Rubio, Lieke A. C. van Son, Robert Klement, Harim Jin, Onno Pols
Figure caption: The inferred initial periods for each system in our sample. The solid green horizontal line shows the current period, while the blue curved line shows the initial period. The blue dashed lines show the 1σ uncertainties of the observed masses and their effect on the initial period. We assume that 10% of the transferred mass is sent to a circumbinary disk and that the mass that is not kept by the accretor is reemitted isotropically. To infer the initial mass ratio, we use the conservative stripped-mass relation (Equation (B3)). The orange dashed line shows the initial period below which Case A mass transfer would occur (roughly). The grayed-out areas show our inferred minimum mass-transfer efficiencies using our strict estimate (Equation (B3)), assuming the median observed masses (light gray) or the lowest minimum mass-transfer efficiency within 1σ of the median observed masses (dark gray). Mass-transfer efficiencies that correspond to initial periods that are above the Case A boundary are consistent with Case B mass transfer. The asterisks next to the names of the systems show the characterization tiers, as in Table 1.
Paper: Binary Stars Take What They Get: Evidence for Efficient Mass Transfer from Stripped Stars with Rapidly Rotating Companions
Authors: Thibault Lechien, Selma E. de Mink, Ruggero Valli, Amanda C. Rubio, Lieke A. C. van Son, Robert Klement, Harim Jin, Onno Pols
Figure caption: Overview of our sample of 16 Be+sdOB binaries. We plot the present-day mass of the Be star (the rapidly spinning accretor) against that of the sdOB star (the stripped star). We also mark the estimated initial mass using Equation (B1) on the top axis. The background color gradient and contours show the minimum mass-transfer efficiencies required to explain the present-day masses of each system, using our conservative estimate (Equation (B3)). The hashed region is forbidden under our assumptions, as it requires efficiencies above 100%. The lower right side of the diagram is notably empty, even though these systems should be easier to detect.
Paper: Binary Stars Take What They Get: Evidence for Efficient Mass Transfer from Stripped Stars with Rapidly Rotating Companions
Authors: Thibault Lechien, Selma E. de Mink, Ruggero Valli, Amanda C. Rubio, Lieke A. C. van Son, Robert Klement, Harim Jin, Onno Pols
Figure caption: Illustration of the origin of a ϕ Persei–like system, shown for a conservative case (left) and a less conservative case (right). The top row shows the ZAMS configuration. The second row shows the Roche-lobe overflow, where the donor star fills its Roche lobe and transfers mass to the accretor. The third row shows the post-mass-transfer configuration, where the donor star has evolved into a stripped helium star, while the accretor has gained mass and AM to become the observed Be star. In the nonconservative case, leftover matter is ejected from the system. The bottom row shows the current observed configuration, where the donor is the sdOB star and the accretor is the Be star.
Paper: WIde Separation Planets In Time (WISPIT): A Gap-clearing Planet in a Multi-ringed Disk around the Young Solar-type Star WISPIT 2
Authors: Richelle F. van Capelleveen, Christian Ginski, Matthew A. Kenworthy, Jake Byrne, Chloe Lawlor, Dan McLachlan, Eric E. Mamajek, Tomas Stolker, Myriam Benisty, Alexander J. Bohn, Laird M. Close, Carsten Dominik, Sebastiaan Haffert, Rico Landman, Jie Ma, Ignas Snellen, Ryo Tazaki, Nienke van der Marel, Lukas Welzel, Yapeng Zhang
Figure caption: SPHERE/IRDIS observations of the WISPIT 2 system are shown here. The gray, hashed disk in the image center indicates the size of the coronagraphic mask. The differential imaging method and observed wave band for each image are indicated in the top-left corner. Blue-hued images reduced with the ADI or RDI (50 principal components) methods are showing total intensity, sensitive to disk scattered light and thermal emission from embedded planets. The gray-hued images are Qϕ images (reduced with the PDI method) showing linearly polarized scattered light, not sensitive to thermal emission.
Paper: WIde Separation Planets In Time (WISPIT): A Gap-clearing Planet in a Multi-ringed Disk around the Young Solar-type Star WISPIT 2
Authors: Richelle F. van Capelleveen, Christian Ginski, Matthew A. Kenworthy, Jake Byrne, Chloe Lawlor, Dan McLachlan, Eric E. Mamajek, Tomas Stolker, Myriam Benisty, Alexander J. Bohn, Laird M. Close, Carsten Dominik, Sebastiaan Haffert, Rico Landman, Jie Ma, Ignas Snellen, Ryo Tazaki, Nienke van der Marel, Lukas Welzel, Yapeng Zhang
Figure caption: All detections of the embedded planet WISPIT 2b in the various observation epochs and filters are shown. We indicate the embedded planet position with a white, dotted circle. The coronagraph position is indicated with a gray, hashed mask. For the 2025 Ks-band data, we show that the embedded planet is recovered with classical and PCA-based ADI as well as in iRDI.