adsabs/AstroCLIMB huggingface dataset:
Paper: Constraining the Mass Loss and the Kinetic Energy of Stellar Coronal Mass Ejections with Solar Far-ultraviolet Flares
Authors: Nuri Park, Evgenya L. Shkolnik, Joe Llama
Figure caption: The FUV flare peak flux [W m–2] plotted against the X-ray flare peak flux [W m–2] (left) and the FUV flare energy [erg] along the X-ray flare energy [erg] (right) during the simultaneous operation time of SDO and GOES (2010 May–2019 December). CME-associated X-ray flares recorded in the SDO AIA1600 instrument are plotted as open gray circles, and halo CME-associated flares are plotted as black cross markers. We binned the data with respect to the X-ray flare peak flux and derived a linear correlation. Each bin, ordered from the lowest to highest flare peak flux and energy, contains 20, 84, 269, 190, 100, and 80 samples for FUV–X-ray flux correlation and 23, 164, 276, 166, 80, and 34 for the FUV–X-ray energy correlation. The median values of the bins are presented as red dots. The error bars on the bins show the interquartile range (IQR) of the samples in the corresponding bins. The red line is the linear correlation derived by the bins, whereas the shaded region around each best-fit line represents the 1σ confidence interval of the regression model, which reflects the uncertainty in the slope and intercept estimates.
Paper: Constraining the Mass Loss and the Kinetic Energy of Stellar Coronal Mass Ejections with Solar Far-ultraviolet Flares
Authors: Nuri Park, Evgenya L. Shkolnik, Joe Llama
Figure caption: The mass of the paired LASCO CMEs without halo CMEs plotted along the GOES X-ray energy of associated flares that occurred during Cycles 23 and 24 (a), Cycle 23 (b), and Cycle 24 (c); the kinetic energy of the paired CMEs along the X-ray flare energy during Cycles 23 and 24 (d), Cycle 23 (e), and Cycle 24 (f); and the linear speed of the CMEs along the X-ray flare energy during Cycles 23 and 24 (g), Cycle 23 (h), and Cycle 24 (i). The green solid line in (a), (b), and (c) shows the correlation derived from A. N. Aarnio et al. (2012). Each bin, ordered from the lowest to highest flare energy, contains 113, 491, 741, 562, 216, and 42 samples for Cycles 23 and 24; 82, 302, 423, 399, 160, and 30 for Cycle 23; and 31, 189, 318, 163, 56, and 12 for Cycle 24. The median values of the bins are presented as blue dots. The error bars indicate the interquartile range (IQR) of the samples in the respective bins.
Paper: Wakes from Companion Interactions in Type Ia Supernovae Nebular Emission Line Profiles
Authors: Kathlynn Simotas, Lars Bildsten, Logan J. Prust
Figure caption: The first two velocity-binned passive scalar quantities (in fraction from 0 to 1 with 0 being none of that bin material present and 1 being ejecta entirely made of that bin’s material) multiplied by the mass density. The top shows the lowest velocity bin, which is less than 7000 km s−1 and the innermost region of the ejecta. The bottom shows the second (and first shell-like) velocity bin from 7000 to 9000 km s−1. The scalar or tracer fractions are multiplied by density to emphasize the amount of material present.
Paper: Constraining the Mass Loss and the Kinetic Energy of Stellar Coronal Mass Ejections with Solar Far-ultraviolet Flares
Authors: Nuri Park, Evgenya L. Shkolnik, Joe Llama
Figure caption: The mass of the paired LASCO CMEs with halo CMEs plotted along the GOES X-ray flare energy of associated flares that occurred during Cycles 23 and 24 (a), Cycle 23 (b), and Cycle 24 (c); the kinetic energy of the paired CMEs along the X-ray flare energy during Cycles 23 and 24 (d), Cycle 23 (e), and Cycle 24 (f); and the linear speed of the CMEs along the X-ray flare energy during Cycles 23 and 24 (g), Cycle 23 (h), and Cycle 24 (i). The green solid line in (a), (b), and (c) shows the correlation derived from A. N. Aarnio et al. (2012). Each bin, ordered from the lowest to highest flare energy, contains 117, 508, 796, 620, 294, and 125 samples for Cycle 23 and 24; 85, 312, 458, 440, 209, and 89 for Cycle 23; and 32, 196, 338, 180, 85, and 36 for Cycle 24. The median values of the bins are presented as blue dots. The error bars indicate the interquartile range (IQR) of the samples in the respective bins.
Paper: Constraining the Mass Loss and the Kinetic Energy of Stellar Coronal Mass Ejections with Solar Far-ultraviolet Flares
Authors: Nuri Park, Evgenya L. Shkolnik, Joe Llama
Figure caption: The mass of X-ray-flare-associated CMEs plotted along the FUV flare peak flux during Cycles 23 and Cycle 24 (a), Cycle 23 (b), and Cycle 24 (c); the kinetic energy of paired CMEs along the FUV flare peak flux during Cycles 23 and Cycle 24 (d), Cycle 23 (e), and Cycle 24 (f); and the linear speed of the CMEs along the FUV flare peak flux during Cycles 23 and 24 (g), Cycle 23 (h), and Cycle 24 (i). The FUV flare peak flux of CME-associated flares during Solar Cycle 23 is calculated by equating the FUV flare peak flux and the X-ray flare peak flux correlation derived from Figure 9. We binned the data with respect to the FUV flare peak flux to derive a linear correlation. Each bin, ordered from the lowest to highest flare peak flux, contains 157, 607, 842, 533, 219, and 102 samples for Cycles 23 and 24; 108, 364, 519, 380, 150, and 73 for Cycle 23; and 50, 243, 323, 153, 69, and 29 for Cycle 24. The median values of the bins are presented as blue dots. The error bars indicate the interquartile range (IQR) of the samples in the respective bins. The blue line is the linear correlation derived by the bins, whereas the uncertainty of the best fit is presented as a shaded region around the best fit.
Paper: Wakes from Companion Interactions in Type Ia Supernovae Nebular Emission Line Profiles
Authors: Kathlynn Simotas, Lars Bildsten, Logan J. Prust
Figure caption: The ejecta properties of the simulation at ϕ = 0 which is representative of the average ejecta properties. The top color bar and half of the polar plot display the density at 500 s postexplosion. The bottom color bar and lower half of the polar plot show the log of the ratio of radiation and gas pressure. The low-density wake is present in both density and pressure space, and the bow shock is clearly visible as an overdensity and the border between gas- and radiation-pressure-dominated regions of the ejecta.
Paper: Constraining the Mass Loss and the Kinetic Energy of Stellar Coronal Mass Ejections with Solar Far-ultraviolet Flares
Authors: Nuri Park, Evgenya L. Shkolnik, Joe Llama
Figure caption: The mass of the flare-associated LASCO CMEs without halo CMEs plotted along the X-ray peak flux of associated GOES X-ray flares that occurred during Cycles 23 and 24 (a), Cycle 23 (b), and Cycle 24 (c); the kinetic energy of the CMEs along the X-ray peak flux during Cycles 23 and 24 (d), Cycle 23 (e), and Cycle 24 (f); and the linear speed of the CMEs along the X-ray peak flux during Cycles 23 and 24 (g), Cycle 23 (h), and Cycle 24 (i). The green solid line in (a), (b), and (c) shows the correlation derived from A. N. Aarnio et al. (2011). Each bin, ordered from the lowest to highest flare flux, contains 92, 311, 698, 592, 316, and 156 samples for Cycles 23 and 24; 63, 208, 397, 389, 228, and 111 for Cycle 23; and 29, 103, 301, 203, 88, and 45 for Cycle 24. The median values of the bins are presented as blue dots. The error bars indicate the interquartile range (IQR) of the samples in the respective bins.
Paper: Constraining the Mass Loss and the Kinetic Energy of Stellar Coronal Mass Ejections with Solar Far-ultraviolet Flares
Authors: Nuri Park, Evgenya L. Shkolnik, Joe Llama
Figure caption: The mass of X-ray-flare-associated CMEs plotted along the FUV flare energy [erg] during Cycle 23 and Cycle 24 (a), Cycle 23 (b), and Cycle 24 (c); the kinetic energy of paired CMEs along the FUV flare energy during Cycle 23 and Cycle 24 (d), Cycle 23 (e), and Cycle 24 (f); and the linear speed of the CMEs along the FUV flare energy during Cycle 23 and Cycle 24 (g), Cycle 23 (h), and Cycle 24 (i). Each bin, ordered from the lowest to highest flare energy, contains 167, 641, 816, 560, 199, and 76 samples for Cycles 23 and 24; 123, 377, 500, 402, 139, and 52 for Cycle 23; and 44, 264, 316, 158, 60, and 24 for Cycle 24. The median values of the bins are presented as blue dots. The error bars indicate the interquartile range (IQR) of the samples in the respective bins.
Paper: The Gradient of Mean Molecular Weight across the Radius Valley
Authors: Kevin Heng, James E. Owen, Meng Tian
Figure caption: Outgassing calculations informed by data-driven radius-valley constraints. Left column: reduced conditions corresponding to ﹩{\mathrm{log}}\,{f}_{{{\rm{O}}}_{2}}﹩ and ﹩{\mathrm{log}}\,{f}_{{{\rm{S}}}_{2}}﹩ being uniformly sampled between −11 and −1 (cgs units; corresponding to 10−17 to 10−7 bar). Right column: oxidized conditions corresponding to ﹩{\mathrm{log}}\,{f}_{{{\rm{O}}}_{2}}﹩ and ﹩{\mathrm{log}}\,{f}_{{{\rm{S}}}_{2}}﹩ being uniformly sampled between −1 and 2 (cgs units; corresponding to 10−7 to 10−4 bar). The top row shows the distributions of mean molecular weight, while the bottom row shows the corresponding oxygen fugacities relative to the iron-wüstite (IW) buffer (which is temperature- and pressure-dependent). The elemental abundance of carbon is assumed to be solar (see text for more details).
Paper: The Gradient of Mean Molecular Weight across the Radius Valley
Authors: Kevin Heng, James E. Owen, Meng Tian
Figure caption: Outgassing calculations for sub-Neptune-like (﹩{P}_{{{\rm{H}}}_{2}}=10﹩ kbar; top row) and Earth-like (﹩{P}_{{{\rm{H}}}_{2}}=1﹩ bar; bottom row) surface pressures. For illustration, we have assumed the oxygen and sulfur fugacities to be equal and have the value ﹩{f}_{{{\rm{O}}}_{2}}={f}_{{{\rm{S}}}_{2}}=1{0}^{-1}﹩ dyne cm−2 = 10−7 bar. The elemental carbon abundance is set to its solar value (C/H = 2.5 × 10−4), while the silicon-to-oxygen ratio is set to Si/O = 0.3. The melt mass fraction has been set to χmelt = 100. The dotted curves are additional calculations that assume ideal gas behavior (ϕi = 1) wherever possible (for H2, H2O, CO, CO2, and CH4), while the dashed curves ignore the solubility laws (for H2 and H2O). Left column: volume mixing ratios of various molecules as functions of melt temperature. Nonideal gas behavior is only relevant for the sub-Neptune-like surface pressure. Right column: mean molecular weight as a function of melt temperature. For the sub-Neptune-like case study, the ﹩{\mathrm{log}}\,{f}_{{{\rm{O}}}_{2}}-\,\rm{IW}\,﹩ values range from −8.7 to −0.2 across the temperature range of 2000–6000 K. For the Earth-like case study, it ranges from −8.5 to 0.1.
Paper: The Gradient of Mean Molecular Weight across the Radius Valley
Authors: Kevin Heng, James E. Owen, Meng Tian
Figure caption: Distributions of mean molecular weight as a function of the sulfur fugacity (top row) and oxygen fugacity (bottom row). The left and right columns correspond to reduced and oxidized conditions, respectively (see text for more details). These distributions are another way to visualize the calculations in Figure 7.
Paper: The Gradient of Mean Molecular Weight across the Radius Valley
Authors: Kevin Heng, James E. Owen, Meng Tian
Figure caption: Left panel: Gibbs free energies of formation for the six net chemical reactions stated in Equations (5) and (7), as constructed using the JANAF database. The dotted curves are fits performed using Chebyshev polynomials (see text for details) for 0 ≤ T ≤ 6000 K. The dashed curves are the same fits extrapolated to 6100 ≤ T ≤ 104 K, except for ΔG3, where we assume its value to be constant (and equal to the value at 6000 K). Right panel: equilibrium constants constructed using the Chebyshev polynomial fits, where the curves beyond 6000 K are extrapolations. The dotted curves are the equilibrium constants constructed using the original JANAF data.
Paper: The Gradient of Mean Molecular Weight across the Radius Valley
Authors: Kevin Heng, James E. Owen, Meng Tian
Figure caption: Data-driven radius valley constraints from matching the observed distributions of planetary radius and orbital period, based on and extending calculations from J.G. Rogers & J.E. Owen (2021). The top left, top right, and bottom left panels show the logarithm of the surface pressure (in bar), logarithm of the melt temperature (in K), and core mass (in Earth masses), respectively, as a color scale. The bottom right panel shows the temperature–pressure relationship with the core mass as a color scale.
Paper: The Gradient of Mean Molecular Weight across the Radius Valley
Authors: Kevin Heng, James E. Owen, Meng Tian
Figure caption: Distributions of mean molecular weight as a function of the elemental abundance of carbon (C/H; left panel) and oxygen fugacity (right panel).
Paper: The Gradient of Mean Molecular Weight across the Radius Valley
Authors: Kevin Heng, James E. Owen, Meng Tian
Figure caption: Distribution of ﹩{M}_{{\rm{core}}}/{M}_{{\rm{atm}}}﹩ (the reciprocal of the atmospheric mass fraction), where we have included only models with R < 2R⊕, a nonzero atmospheric mass, and a melt temperature of T > 2000 K. This curated sample corresponds to 3758 simulated exoplanets. The maximum value of ﹩{M}_{{\rm{core}}}/{M}_{{\rm{atm}}}﹩ in this distribution is about 9462.
Paper: The Gradient of Mean Molecular Weight across the Radius Valley
Authors: Kevin Heng, James E. Owen, Meng Tian
Figure caption: Ratios of molecular abundances (by number) corresponding to the calculations in Figure 7, where the left and right columns correspond to reduced and oxidized conditions, respectively (see text for more details). The top and bottom row are for the ratios of methane (CH4) to carbon dioxide (CO2) and molecular hydrogen (H2) to water (H2O), respectively.
Paper: The Gradient of Mean Molecular Weight across the Radius Valley
Authors: Kevin Heng, James E. Owen, Meng Tian
Figure caption: The oxygen fugacity (in bar) of the IW buffer using the empirical formulae of C. Ballhaus et al. (1991) and M.M. Hirschmann (2021), which are shown as dotted and solid curves, respectively.
Paper: Turbulent Gas-rich Disks at High Redshift: Origin of Thick Stellar Disks Through 3D “Baryon Sloshing”
Authors: Joss Bland-Hawthorn, Thor Tepper-Garcia, Oscar Agertz, Christoph Federrath, Misha Haywood, Paola di Matteo, Timothy R. Bedding, Takafumi Tsukui, Emily Wisnioski, Melissa Ness, Ken Freeman
Figure caption: Nexus simulations in the presence of halo accretion for an fdisk = 0.5 stellar disk for different values of fgas, as indicated. Left panel: x − y (left column) and x − z (right column) projections of the sloshing action. Note that the physical scale of each plot is growing with increasing fgas. Right panel: x − y (left column) and x − z (right column) projections of the sloshing action. Note that the physical scale of each plot is fixed for all fgas. The baryon sloshing is defined in terms of the separation of the minimum of the total gravitational potential Φtot(0, 0, 0) (indicated by a cross) and the baryon gravitational potential, Φbary(0, 0, 0). The color coding indicates the passage of time, as indicated by the RHS bar, extending from z ≈ 3.3 to z ≈ 1.5. Internal to each plot, the horizontal and vertical scales are always matched.
Paper: Turbulent Gas-rich Disks at High Redshift: Origin of Thick Stellar Disks Through 3D “Baryon Sloshing”
Authors: Joss Bland-Hawthorn, Thor Tepper-Garcia, Oscar Agertz, Christoph Federrath, Misha Haywood, Paola di Matteo, Timothy R. Bedding, Takafumi Tsukui, Emily Wisnioski, Melissa Ness, Ken Freeman
Figure caption: Nexus simulation for an fdisk = 0.5 stellar disk with no cold gas component (fgas = 0%). The top left and bottom left panels are the x − y and x − z slosh projections, respectively, at a fixed timestep. The baryon sloshing is defined in terms of the separation of the minimum of the total gravitational potential (Φtot(0, 0) indicated by the cross at the origin) and the baryon potential (Φbary(0, 0)). (The boxed information concerns the disk asymmetry and concentration, a topic discussed in our companion paper, J. Bland-Hawthorn et al. 2025, in preparation). The physical scales of the three circles are indicated in the lower key). The top right and bottom right panels are the x − y and x − z slosh projections, respectively, but highly magnified compared to the LHS panels. A small amount of “baryon sloshing” (≲50 pc) is expected due to the discreteness of the disk, as demonstrated. The color coding indicates the baryon centroid shifts with the passage of time, as indicated.
Paper: Turbulent Gas-rich Disks at High Redshift: Origin of Thick Stellar Disks Through 3D “Baryon Sloshing”
Authors: Joss Bland-Hawthorn, Thor Tepper-Garcia, Oscar Agertz, Christoph Federrath, Misha Haywood, Paola di Matteo, Timothy R. Bedding, Takafumi Tsukui, Emily Wisnioski, Melissa Ness, Ken Freeman
Figure caption: Periodograms drawn from our heavy disk (fdisk = 0.5) simulations that capture how the star formation rate (SFR) surface density (in units of M⊙ yr−1 kpc−2) evolves as a function of radius and cosmic time: (left) without halo accretion; (right) with halo accretion. The five rows correspond to different gas fractions, in order from the top, fgas = 20%, 40%, 60%, 80%, 100%. All models commence with a short-lived, disk-wide “starburst” phase that moves outwards for the first 300 Myr. These stochastic starbursts are defined by SFR surface densities that exceed the average rate by more than an order of magnitude (i.e., blue regions). The higher fgas models sustain a higher SFR surface density over a larger radial range for both models, as do the halo accretion models in general when compared to the matching nonaccreting model.
Paper: Turbulent Gas-rich Disks at High Redshift: Origin of Thick Stellar Disks Through 3D “Baryon Sloshing”
Authors: Joss Bland-Hawthorn, Thor Tepper-Garcia, Oscar Agertz, Christoph Federrath, Misha Haywood, Paola di Matteo, Timothy R. Bedding, Takafumi Tsukui, Emily Wisnioski, Melissa Ness, Ken Freeman
Figure caption: The 2D slosh projections in Figure 7 can be rendered in 3D to reveal the erratic movement. The tracks all refer to the fgas = 100% halo accretion case: (left) motion of Φtot(0, 0, 0) with respect to the inertial reference frame; (middle) motion of Φbary(0, 0, 0) with respect to the inertial reference frame; (right) motion of Φbary(0, 0, 0) with respect to Φtot(0, 0, 0). The slosh axes are in units of kiloparsecs in a comoving frame. Evidently, for the baryons, there are frequent major reversals over the 2 Gyr simulation. The color coding indicates the passage of time, from blue to red over this timespan.
Paper: Turbulent Gas-rich Disks at High Redshift: Origin of Thick Stellar Disks Through 3D “Baryon Sloshing”
Authors: Joss Bland-Hawthorn, Thor Tepper-Garcia, Oscar Agertz, Christoph Federrath, Misha Haywood, Paola di Matteo, Timothy R. Bedding, Takafumi Tsukui, Emily Wisnioski, Melissa Ness, Ken Freeman
Figure caption: The evolution of the azimuthally averaged, radial profile of the disk potential Φbary(R, t) with cosmic time, normalized to the starting potential Φbary(R, 0) encoded in color for (top) no halo accretion and (bottom) halo accretion. Blue tracks are early in cosmic time and red tracks are later times, as indicated. For fgas < 0.5, the disk potential is fairly constant but, above this limit, the loss of gas mass in circulating winds leads to a substantial weakening of the disk potential. Note that the vertical axis is a ratio of gravitational potentials, such that a curve moving downwards reflects a weaker potential.
Paper: Turbulent Gas-rich Disks at High Redshift: Origin of Thick Stellar Disks Through 3D “Baryon Sloshing”
Authors: Joss Bland-Hawthorn, Thor Tepper-Garcia, Oscar Agertz, Christoph Federrath, Misha Haywood, Paola di Matteo, Timothy R. Bedding, Takafumi Tsukui, Emily Wisnioski, Melissa Ness, Ken Freeman
Figure caption: The total gravitational potential for a Nexus galaxy simulation with fdisk = 0.5 and fgas = 0. The equipotential surfaces are shown for the inner 10 kpc (comoving) diameter.
Paper: Turbulent Gas-rich Disks at High Redshift: Origin of Thick Stellar Disks Through 3D “Baryon Sloshing”
Authors: Joss Bland-Hawthorn, Thor Tepper-Garcia, Oscar Agertz, Christoph Federrath, Misha Haywood, Paola di Matteo, Timothy R. Bedding, Takafumi Tsukui, Emily Wisnioski, Melissa Ness, Ken Freeman
Figure caption: Edge-on gas surface density maps taken from our early disk simulations at to = 1 Gyr. We adopt fdisk = 0.5 for the Milky Way progenitor at z ∼ 3. The top panels are for five different initial gas fractions (as indicated) with no halo accretion; the bottom five are the matching simulations that include halo accretion from cooling hot gas. From left to right, for both rows, the galaxy’s center falls at the right-hand side (RHS) edge in the first four panels, but is centered in the last panel, where the spatial scale is indicated. The extent of the disk–halo interaction is a reflection of the disk-wide star formation shown in Figure 2.
Paper: Turbulent Gas-rich Disks at High Redshift: Origin of Thick Stellar Disks Through 3D “Baryon Sloshing”
Authors: Joss Bland-Hawthorn, Thor Tepper-Garcia, Oscar Agertz, Christoph Federrath, Misha Haywood, Paola di Matteo, Timothy R. Bedding, Takafumi Tsukui, Emily Wisnioski, Melissa Ness, Ken Freeman
Figure caption: The upper figure in each panel shows evolution of the dark matter density profile as a function of radius R for the halo accretion models. The lower figure in each panel presents the ratio of the post-starburst to original density profiles. At the highest gas fractions, the central NFW cusp is suppressed by a factor of 2, but not destroyed. In all plots, the color coding indicates the time evolution of the density profile, as indicated, with the reddest profile indicating the end of the simulation.
Paper: Lost Sisters Found: TESS and Gaia Reveal a Dissolving Pleiades Complex
Authors: Andrew W. Boyle, Luke G. Bouma, Andrew W. Mann
Figure caption: UPK 303 and surrounding stars compared with the Pleiades. Galactocentric positions (XY, XZ, YZ; top row) show that UPK 303 lies along a continuous spatial sequence extending from the Pleiades core. The second row shows Galactocentric velocities (UVW). The color–magnitude diagram (CMD; bottom-left panel) and the rotation period-Teff plane (bottom-right panel) demonstrate that both structures lie along the same stellar sequence, consistent with a common age. Metallicity spread (bottom middle) shows that UPK 303 members differ from a random sample of nearby field stars and are comparable to stars in the Pleiades core. The bottom-right panel shows the past separation between UPK 303 and the Pleiades, computed via 5000 Monte Carlo orbit integrations. Together, the spatial, kinematic, photometric, rotational, chemical, and dynamical similarities support a physical association between UPK 303 and the Pleiades.
Paper: Lost Sisters Found: TESS and Gaia Reveal a Dissolving Pleiades Complex
Authors: Andrew W. Boyle, Luke G. Bouma, Andrew W. Mann
Figure caption: Stellar kinematics and rotation isolate the Greater Pleiades Complex. Top-left panel: stars with T < 16 and d < 500 pc (gray), highlighting those within 5 km s−1 of the Pleiades’ median 3D velocity (black). The Sun is marked by a yellow point at the origin. Top-right panel: subset of stars consistent with the Pleiades in velocity, with reliable TESS rotation periods (Prot < 12 days and reliability >0.7). Bottom-left panel: 6D clustering results from HDBSCAN applied to the velocity and rotation-selected sample. Bottom-right panel: high-confidence members (N = 1075) with 3D velocities, selected for spatiokinematic coherence, rotation consistency, and placement on the cluster CMD. These stars define a comoving and coeval population that we will argue comprises the Greater Pleiades Complex.