adsabs/AstroCLIMB huggingface dataset:
Paper: Gravitational Instability and Fragmentation in Collapsar Disks Supports the Formation of Subsolar Neutron Stars
Authors: Yi-Xian Chen, Brian D. Metzger
Figure caption: Approximate gravitational waveform showing the combined strain htot(t) produced by the chirp hNS(t) from a binary composed of two 0.1 M⊙ NSs in orbit around a 3 M⊙ BH starting at r = 200 Rg and NSs at Hill radius separation, calculated by adding two point-mass waveforms in the first-order post-Newtonian limit for an observer with an optimal orientation perpendicular to the angular momentum axes of both mergers. The top panel shows a zoom-out version starting from t = 0 and ends at the final BH–NS coalescence, with a vertical dashed line showing the termination of the NS–NS merger. The bottom panel shows a zoomed-in version of htot(t), as well as a comparison with the effects of including Doppler modulation of the NS–NS merger signal due to the binary’s orbital motion (Equation (B14)). Our calculation neglects several other effects, including Doppler modulation of the strain amplitude and the Shapiro time delay.
Paper: Gravitational Instability and Fragmentation in Collapsar Disks Supports the Formation of Subsolar Neutron Stars
Authors: Yi-Xian Chen, Brian D. Metzger
Figure caption: Solid contours show the approximate dimensionless cooling timescale due to α-particle dissociation, τcool,α (Section 4.1), in the same parameter space of disk surface density and angular frequency shown in Figure 1. We have very roughly estimated the α-particle cooling rate for a contracting clump by assuming that Xα drops by an order-unity factor from its initial midplane value over one neutrino cooling timescale (see Equation (17) and surrounding text). A comparison of these contours to those in Figure 1 from neutrino cooling alone indicates the importance of α-particle cooling, particularly for disks that begin rich in α particles (Xα ≃ 1; below the dotted red line).
Paper: Gravitational Instability and Fragmentation in Collapsar Disks Supports the Formation of Subsolar Neutron Stars
Authors: Yi-Xian Chen, Brian D. Metzger
Figure caption: Snapshots show the vertical profiles of Xα through a ﹩y={\rm{Const}}﹩ slice comparing the initial state to that after fragmentation, as well as the Xα distribution in the midplane in the fragmentation state. The upper and lower panels are for case O16T1.5e10 and case O8T1e10, respectively.
Paper: Gravitational Instability and Fragmentation in Collapsar Disks Supports the Formation of Subsolar Neutron Stars
Authors: Yi-Xian Chen, Brian D. Metzger
Figure caption: Upper panel: mass histogram (in units of the Jeans mass) of self-bound clumps similar to those shown in Figures 6 and 9 but for the broader suite of simulations. A black line shows the average of all six fragmenting simulations. Lower panel: average Ye and associated local Chandrasekhar mass MCh using the clump-averaged electron fraction (Equation (1)). Filled circles indicate those clumps that exceed MCh and are therefore expected to continue collapsing to form NSs.
Paper: Gravitational Instability and Fragmentation in Collapsar Disks Supports the Formation of Subsolar Neutron Stars
Authors: Yi-Xian Chen, Brian D. Metzger
Figure caption: Equilibrium electron fraction Ye,eq, α-particle mass fraction Xα, and electron chemical potential μ/kT in the space of ρ and T. A red dotted line shows the contour ﹩{ \mathcal G }=1﹩ (Equation (A10)) separating the regions of parameter space where all nucleons are free from that where most protons are trapped in α particles.
Paper: Gravitational Instability and Fragmentation in Collapsar Disks Supports the Formation of Subsolar Neutron Stars
Authors: Yi-Xian Chen, Brian D. Metzger
Figure caption: Same as Figure 6 but illustrating the bound clump properties for model O8T1e10, corresponding to an initially α-rich disk.
Paper: Gravitational Instability and Fragmentation in Collapsar Disks Supports the Formation of Subsolar Neutron Stars
Authors: Yi-Xian Chen, Brian D. Metzger
Figure caption: Snapshot of the (x, y) profiles through the midplane (z = 0) of density, temperature, dimensionless cooling time, electron fraction Ye, and μ/kT for the fragmenting simulation O8T1e10. Lengths are expressed in units of the vertical scale height H.
Paper: Which Solar Latitude Follows the Sunspot Cycle Exactly?
Authors: K. P. Raju
Figure caption: Cross correlation of lane widths (pink) and intensities (black) with sunspot cycle as a function of lag (year) at different latitudes. The panels on the right give a magnified view of the central region (−5 < lag < 5) at selected latitudes.
Paper: Which Solar Latitude Follows the Sunspot Cycle Exactly?
Authors: K. P. Raju
Figure caption: Maximum correlation coefficient of lane width (pink) and intensity (black) with sunspot cycle at different latitudes (top). The continuous line represents a five-point smoothing average. The horizontal dashed line represents the 99% confidence level. Lag (year) of lane width (pink) and intensity (black) with solar cycle at different latitudes (bottom). Only those points with a correlation coefficient above 0.29 (99% confidence level) are shown.
Paper: Which Solar Latitude Follows the Sunspot Cycle Exactly?
Authors: K. P. Raju
Figure caption: Yearly averaged supergranular lane widths (pink) and Ca K intensity (black) as a function of time for different latitudes from 60°N to 60°S with an interval of 10°. The y-axis on the right gives the normalized intensity. The bottom panel shows the variation of the yearly averaged sunspot number with time. Sunspot data from the World Data Center SILSO, Royal Observatory of Belgium, Brussels.
Paper: Parallel and Perpendicular Diffusion of Energetic Particles in the Near-Sun Solar Wind Observed by Parker Solar Probe
Authors: Nibuna S. M. Subashchandar, Lingling Zhao, Andreas Shalchi, Gary Zank, Jakobus Le Roux, Hui Li, Xingyu Zhu, Ashok Silwal, Juan G. Alonso Guzman
Figure caption: PSD of the transverse magnetic field fluctuations from PSP orbit E1–E19 observations with quasi-parallel (θBV < 15°) sampling. Each PSD is calculated with a 5 hr interval and color-coded by the radial distance r from the Sun. Inertial range Kolmogorov-like f−5/3 and Iroshnikov–Kraichnan f−3/2 spectra are shown for reference. fmid represents the frequency separating the energy-containing range and the inertial range and is determined as the statistical midpoint containing 50% of the total fluctuation power.
Paper: Parallel and Perpendicular Diffusion of Energetic Particles in the Near-Sun Solar Wind Observed by Parker Solar Probe
Authors: Nibuna S. M. Subashchandar, Lingling Zhao, Andreas Shalchi, Gary Zank, Jakobus Le Roux, Hui Li, Xingyu Zhu, Ashok Silwal, Juan G. Alonso Guzman
Figure caption: Panel (a) shows the PSP/IS⊙IS EPI-Lo observed ion differential intensity (dots) over a 15 minute interval upstream of the shock on 2023 October 28. The black lines represent least-squares fits to the particle time-intensity profile to obtain the exponential rise time Δt in minutes for each energy bin. The right panel shows the comparison between the parallel diffusion coefficient calculated from QLT with assumptions (green and blue curves) and SOQLT (red curve) and the particle time-intensity profile (black open circles).
Paper: Parallel and Perpendicular Diffusion of Energetic Particles in the Near-Sun Solar Wind Observed by Parker Solar Probe
Authors: Nibuna S. M. Subashchandar, Lingling Zhao, Andreas Shalchi, Gary Zank, Jakobus Le Roux, Hui Li, Xingyu Zhu, Ashok Silwal, Juan G. Alonso Guzman
Figure caption: Radial evolution of the parallel and perpendicular diffusion coefficients, κ∥ (SOQLT) and κ⊥ (UNLT), derived from the observed turbulence spectra. (a) κ∥ as a function of radial distance from the Sun (10–60 R⊙), color-coded by particle kinetic energy (500 keV–1 GeV). (b) κ⊥ displayed similarly. In both panels, black dashed lines represent power-law fits obtained via linear least-squares regression of the scatters.
Paper: Parallel and Perpendicular Diffusion of Energetic Particles in the Near-Sun Solar Wind Observed by Parker Solar Probe
Authors: Nibuna S. M. Subashchandar, Lingling Zhao, Andreas Shalchi, Gary Zank, Jakobus Le Roux, Hui Li, Xingyu Zhu, Ashok Silwal, Juan G. Alonso Guzman
Figure caption: Dependence of the diffusion coefficient ratio κ⊥/κ∥ on (a) heliocentric distance r and (b) the relative fluctuation amplitude δB/B0. Scatter points are derived from PSP E1–E19 observations, and the black dashed curves show power-law fits for five distinct particle energy ranges.
Paper: Parallel and Perpendicular Diffusion of Energetic Particles in the Near-Sun Solar Wind Observed by Parker Solar Probe
Authors: Nibuna S. M. Subashchandar, Lingling Zhao, Andreas Shalchi, Gary Zank, Jakobus Le Roux, Hui Li, Xingyu Zhu, Ashok Silwal, Juan G. Alonso Guzman
Figure caption: Radial evolution of the diffusion coefficients κ∥ (SOQLT) and κ⊥ (UNLT) as functions of the turbulence amplitude δB/B0. Panels (a) and (b) show κ∥ and κ⊥, respectively, with data points color-coded by particle energy (500 keV–1 GeV). Black dashed lines indicate power-law trends obtained by linear least-squares fitting.
Paper: Parallel and Perpendicular Diffusion of Energetic Particles in the Near-Sun Solar Wind Observed by Parker Solar Probe
Authors: Nibuna S. M. Subashchandar, Lingling Zhao, Andreas Shalchi, Gary Zank, Jakobus Le Roux, Hui Li, Xingyu Zhu, Ashok Silwal, Juan G. Alonso Guzman
Figure caption: Overview of the SEP event observed by PSP on 2023 October 28. The top panel shows the differential intensity of energetic protons across multiple energy channels. The bottom panel shows a spectrogram of differential intensity for all analyzed protons, with energy on the vertical axis and intensity indicated by the color bar. The vertical dashed line marks the arrival of the interplanetary shock.
Paper: Effect of Galactic Chemical Evolution on Exoplanet Properties
Authors: Jason H. Steffen, Cody Shakespeare, Robert Royer, David Rice, Allona Vazan
Figure caption: Left: the initial percent masses of ﹩{Z}_{0}^{* }/{X}_{0}﹩, iron over total elements, and iron over hydrogen. ﹩{Z}_{0}^{* }﹩ is the sum of all metals used in our dust condensation program. The exclusion of the other metals results in our solar ﹩{Z}_{0}^{* }/{X}_{0}=1.9 \% ﹩, compared with the K. Lodders (2003) value of Z0/X0 = 2.1%. Right: the initial percent cosmological abundances of select elemental ratios.
Paper: Effect of Galactic Chemical Evolution on Exoplanet Properties
Authors: Jason H. Steffen, Cody Shakespeare, Robert Royer, David Rice, Allona Vazan
Figure caption: The elemental ratios of solid materials after chemical condensation around a 1 M⊙ star of varying age. The elemental ratio represents the total sum of those elements over the entire disk. Some areas of the disk can experience significant differences from the ratios shown. Disks around 2 M⊙ stars show small differences that are imperceptible. The upward triangles represent the corresponding fast-material-enriched simulations. The downward triangles represent the slow-material-enriched simulations. The base of each triangle indicates the enriched material ratios.
Paper: Effect of Galactic Chemical Evolution on Exoplanet Properties
Authors: Jason H. Steffen, Cody Shakespeare, Robert Royer, David Rice, Allona Vazan
Figure caption: Radius vs. mass for planets formed at different times and selected orbital radii. The color indicates the time at which the planet was formed, from 1 to 13 Gyr. The left panel shows three orbital radii around a 1 solar mass star. The right panel shows the same orbital radii around a 2 solar mass star.
Paper: Effect of Galactic Chemical Evolution on Exoplanet Properties
Authors: Jason H. Steffen, Cody Shakespeare, Robert Royer, David Rice, Allona Vazan
Figure caption: The percent change in initial cosmochemical abundance for select metals, normalized to Silicon and to the solar abundances at t = 8 Gyr, for each odd time step.
Paper: Effect of Galactic Chemical Evolution on Exoplanet Properties
Authors: Jason H. Steffen, Cody Shakespeare, Robert Royer, David Rice, Allona Vazan
Figure caption: The stellar age and CMF (%) of planets from A. Weeks et al. (2025) with 1σ uncertainties. The CMF is found with MAGRATHEA, given the masses and radii in A. Weeks et al. (2025). The planet’s equilibrium temperature is represented by the color and the planet’s mass by the size of the circle. The three gold lines of the CMF with age from our results are shown measured at 1 au around a solar mass star (note that this distance is exterior to most detected exoplanets, thus there is an implicit assumption that the observed planets migrated inward after formation). “Norm.” is when elemental abundances are normalized to the solar system, while “+HM” is enriched in high-mass material, and “+LM” has increased low-mass material. Earth and Mercury are also shown for reference. Note that the x-axis in this case is the age of the star and thus the inverse of the previous plots.
Paper: Effect of Galactic Chemical Evolution on Exoplanet Properties
Authors: Jason H. Steffen, Cody Shakespeare, Robert Royer, David Rice, Allona Vazan
Figure caption: The final solid surface densities of various elements in disks around 1 M⊙ stars. Select elements are shown using three different units and with four different stellar abundances. From left to right, the columns show the results of a star formed with the elements present at 1 Gyr, 3 Gyr, 8 Gyr, and 13 Gyr. Top row: surface density on a linear y-axis, with units of moles per square centimeter. Middle row: percent solid mass of each element’s solid phase (i.e., ﹩\tfrac{{\mathrm{Oxygen}}_{\mathrm{Solid}}}{{\mathrm{Total}}_{\mathrm{Solid}}}\ast 100﹩). The “Sum” line is the sum of all elements shown in the plot. Bottom row: surface density on a logarithmic y-axis, with units of grams per square centimeter.
Paper: Effect of Galactic Chemical Evolution on Exoplanet Properties
Authors: Jason H. Steffen, Cody Shakespeare, Robert Royer, David Rice, Allona Vazan
Figure caption: The final solid surface densities of various elements in disks around 2 M⊙ stars. The columns and rows are the same as in Figure A3.
Paper: Effect of Galactic Chemical Evolution on Exoplanet Properties
Authors: Jason H. Steffen, Cody Shakespeare, Robert Royer, David Rice, Allona Vazan
Figure caption: The fractional change in the initial cosmochemical abundances of all metals included in dust condensation, normalized to solar at t = 8 Gyr, for each odd time step. Top: C–Ge. Bottom: Mo–Au.
Paper: Effect of Galactic Chemical Evolution on Exoplanet Properties
Authors: Jason H. Steffen, Cody Shakespeare, Robert Royer, David Rice, Allona Vazan
Figure caption: The amount of normalized material produced through fast processes and slow processes at each time step, using the empirical SFR from O. Snaith et al. (2015) and the IMF from Equation (1).
Paper: Quantifying the Distribution of Europium in the Milky Way Disk: Its Connection to Planetary Habitability and the Source of the r-process
Authors: Evan M. Carrasco, Matthew Shetrone, Francis Nimmo, Enrico Ramirez-Ruiz, Joel Primack, Natalie M. Batalha, Brady Lobmeyer
Figure caption: (a) The top panel shows [Eu/α] independent of the temperature bias as a function of [α/H]. Small orange triangles represent data from DM, and small green triangles represent data from BB. The cross-matched sample of 68 stars described in Section 3.1 is shown with big red squares. Stars from the solar twins analysis by M. Bedell et al. (2018) and L. Spina et al. (2018) are shown as big blue circles. A black star is used to represent the solar abundance value. The red dashed line at [Eu/α] = 0.06 represents the critical value for an extended dynamo failure given by the model from F. Nimmo et al. (2020). Outliers in [Eu/H] abundances discussed in Appendix A.2 are outlined in black. (b) The bottom panel shows [Eu/Fe] independent of the temperature bias as a function of [Fe/H]. The legend is the same as in (a).
Paper: Quantifying the Distribution of Europium in the Milky Way Disk: Its Connection to Planetary Habitability and the Source of the r-process
Authors: Evan M. Carrasco, Matthew Shetrone, Francis Nimmo, Enrico Ramirez-Ruiz, Joel Primack, Natalie M. Batalha, Brady Lobmeyer
Figure caption: Dynamo failure duration for an Earth-like planet as a function of terrestrial radiogenic element concentrations (U and Th) relative to α elements. A value of [0] indicates an Earth-like ratio. See F. Nimmo et al. (2020) for details on model parameters. A scaled radiogenic fraction of 0.06 dex (red dashed line) results in a dynamo failure of ∼40 Myr, long enough to presumably have devastating effects on surface conditions. This scaled radiogenic fraction threshold corresponds to a stellar abundance of [Eu/α] = 0.06 dex.
Paper: Preferential Energization of Solar Wind Ions Below the Alfvénic Surface
Authors: Parisa Mostafavi, V. K. Jagarlamudi, N. E. Raouafi, J. C. Palacios, R. C. Allen, M. E. Hill, L. Ofman, G. C. Ho
Figure caption: (a) Profiles of temperature anisotropies, T⊥/T∥, for protons (red) and alpha particles (blue) as a function of heliocentric distance in solar radii, based on data from the pre-perihelia of three PSP encounters. (b) Temperature anisotropies as a function of local Alfvén Mach number. Both anisotropies display a more systematic dependence on MA. Median values and the error bars are shown at each bin. Here, radial bin and MA bin widths are 0.14 Rs and 0.05, respectively. The error bars represent the standard error of data in each bin.
Paper: Preferential Energization of Solar Wind Ions Below the Alfvénic Surface
Authors: Parisa Mostafavi, V. K. Jagarlamudi, N. E. Raouafi, J. C. Palacios, R. C. Allen, M. E. Hill, L. Ofman, G. C. Ho
Figure caption: (a) Total alpha-to-proton temperature ratio (Tα/Tp) as a function of the Alfvén Mach number (MA). The temperature ratio is elevated in the sub-Alfvénic regime, peaking near the Alfvén critical point (MA ∼ 1), and declines thereafter, indicating stronger preferential heating of alpha particles below the Alfvén surface. (b) Normalized differential velocity between alpha particles and protons to the local Alfvén velocity (Vαp/VA) as a function of MA. The differential speed increases steadily with MA, consistent with preferential acceleration of alpha particles. Then it saturates in the super-Alfvénic medium. The vertical red dashed line marks the nominal location of the Alfvénic surface (MA = 1) in both panels. The error bars correspond to standard errors.
Paper: Preferential Energization of Solar Wind Ions Below the Alfvénic Surface
Authors: Parisa Mostafavi, V. K. Jagarlamudi, N. E. Raouafi, J. C. Palacios, R. C. Allen, M. E. Hill, L. Ofman, G. C. Ho
Figure caption: (a) Parallel (Tp∣∣, maroon) and perpendicular (Tp⊥, orange) proton temperatures in eV as a function of Alfvén Mach number, MA. (b) Parallel (Tα∣∣, blue) and perpendicular (Tα⊥, cyan) alpha temperatures as a function of MA. (c) Ratio of alpha-to-proton temperatures in the parallel direction (purple) and perpendicular direction (green) as functions of MA. All panels show median values in each MA bin with standard error bars. Median values and the error bars are shown at each MA bin. The error bars correspond to standard errors. The vertical red dashed line marks the nominal location of the Alfvénic surface (MA = 1) in both panels.
Paper: The Light Echo of a High-redshift Quasar Mapped with Lyα Tomography
Authors: Anna-Christina Eilers, Minghao Yue, Jorryt Matthee, Joseph F. Hennawi, Frederick B. Davies, Robert A. Simcoe, Richard Teague, Rongmon Bordoloi, Gabriel Brammer, Yi Kang, Daichi Kashino, Ruari Mackenzie, Rohan P. Naidu, Benjamín Navarrete
Figure caption: Stacked galaxy spectra. The top panel shows the two-dimensional unweighted mean stack of all 12 galaxy spectra colored by the flux. The bottom panel shows the unweighted stack over the same wavelength range of the continuum normalized one-dimensional galaxy spectra binned to 500 km s−1 pixels around the quasar’s systemic redshift, which is indicated by the vertical black dashed lines at d∥ = 0 pMpc or λLyα ≈ 8907 Å. The horizontal dashed line indicates the spectral trace in the top panel, while it denotes the zero flux level in the bottom panel. Note that the two-dimensional spectra are not normalized by the galaxies’ continuum emission before stacking, while we did normalize the one-dimensional spectra to show the stacked Lyα transmitted flux.
Paper: The Light Echo of a High-redshift Quasar Mapped with Lyα Tomography
Authors: Anna-Christina Eilers, Minghao Yue, Jorryt Matthee, Joseph F. Hennawi, Frederick B. Davies, Robert A. Simcoe, Richard Teague, Rongmon Bordoloi, Gabriel Brammer, Yi Kang, Daichi Kashino, Ruari Mackenzie, Rohan P. Naidu, Benjamín Navarrete
Figure caption: Observations. The middle panel shows a color image of the quasar field with the central quasar circled in red, constructed via NIRCam images in the filters F115W, F200W, and F356W, showing the spatial locations of the 12 analyzed background galaxies, circled in white. The top and bottom panels show the two-dimensional and one-dimensional spectra of two galaxies, which show a clear detection of the transverse proximity effect at the systemic redshift of the quasar zQSO indicated by the red dashed line. The yellow dashed line shows the galaxies’ redshift as determined from the [O III]-emission line, zgal, while the blue dashed–dotted line demonstrates the power-law fit to the unabsorbed galaxy continuum at λrest > λLyα, which is used to calculate the flux transmission and the optical depth within the Lyα forest.
Paper: The Light Echo of a High-redshift Quasar Mapped with Lyα Tomography
Authors: Anna-Christina Eilers, Minghao Yue, Jorryt Matthee, Joseph F. Hennawi, Frederick B. Davies, Robert A. Simcoe, Richard Teague, Rongmon Bordoloi, Gabriel Brammer, Yi Kang, Daichi Kashino, Ruari Mackenzie, Rohan P. Naidu, Benjamín Navarrete
Figure caption: Sample of [O III]-emitting galaxies in the quasar field J0100+2802. A total of 213 [O III]-emitters (gray points) were previously discovered via NIRCam WFSS observations (D. Kashino et al. 2023) in this quasar field. For 35 of them (blue stars), we obtained deep NIRSpec/MSA spectroscopic observations, and 12 of those (red stars) were used in this analysis. Left and right panels show the observed magnitude in NIRCam’s F115W filter and the galaxies’ continuum signal-to-noise ratio per pixel as a function of redshift z, respectively.
Paper: The Light Echo of a High-redshift Quasar Mapped with Lyα Tomography
Authors: Anna-Christina Eilers, Minghao Yue, Jorryt Matthee, Joseph F. Hennawi, Frederick B. Davies, Robert A. Simcoe, Richard Teague, Rongmon Bordoloi, Gabriel Brammer, Yi Kang, Daichi Kashino, Ruari Mackenzie, Rohan P. Naidu, Benjamín Navarrete
Figure caption: Galaxy spectra. Two-dimensional (top) and one-dimensional (bottom) spectra of 10 out of the 12 analyzed galaxies in the quasar field (the remaining two galaxy spectra are shown in Figure 2). The red and yellow dashed lines indicate the systemic redshift of the quasar zQSO as well as the galaxy’s redshift zgal, respectively. Blue dashed–dotted lines show the power-law fit to the unabsorbed galaxy continuum emission.