adsabs/AstroCLIMB huggingface dataset:
Paper: Examining AGN UV/Optical Variability beyond the Simple Damped Random Walk
Authors: Weixiang Yu, Gordon T. Richards, Michael S. Vogeley, Jackeline Moreno, Matthew J. Graham
Figure caption: Distribution of the main-sample quasars in the luminosity (absolute i-band magnitude k-corrected to a redshift of 2) and redshift space. This sample is constructed from the SDSS DR16 quasar catalog—the latest release of SDSS quasar spectra (Lyke et al. 2020); quasars in this sample either have their physical properties estimated by Shen et al. (2011) or have their C IV emission-line properties measured by Rankine et al. (2020).
Paper: Examining AGN UV/Optical Variability beyond the Simple Damped Random Walk
Authors: Weixiang Yu, Gordon T. Richards, Michael S. Vogeley, Jackeline Moreno, Matthew J. Graham
Figure caption: Distribution of SDSS light-curve statistics in g and z bands. The statistics shown are (from left to right) minimum time separation between any two observations in a light curve (﹩\mathrm{Min}\,{\rm{\Delta }}t﹩), the maximum time separation between any two observations in a light curve (﹩\mathrm{Max}\,{\rm{\Delta }}t﹩), number of epochs in a light curve, and the median photometric error for observations in a light curve.
Paper: The Internal Proper Motion Kinematics of NGC 346: Past Formation and Future Evolution
Authors: E. Sabbi, P. Zeidler, R. P. van der Marel, A. Nota, J. Anderson, J. S. Gallagher, D. J. Lennon, L. J. Smith, M. Gennaro
Figure caption: PM VPD of the PMS stars, measured in the F814W filter. The median error in the μ  x  and μ  y  directions is shown in the upper-right corner.
Paper: Deep Two-phase, Hemispherical Magma Oceans on Lava Planets
Authors: Charles-Édouard Boukaré, Nicolas B. Cowan, James Badro
Figure caption: Adiabatic and subadiabatic temperature profiles of lava planet interiors for four different surface temperatures: 1700, 1900, 2400, and 3000 K. We consider two endmember scenarios, depending on the iron core temperature. In the hot-core scenario, the temperature difference between the surface and the CMB is large enough to drive thermal convection, imposing an adiabatic temperature profile (solid black lines) in the magma ocean. In the cold-core scenario, the temperature difference between the surface and the CMB is subadiabatic, preventing heat transport by convection. We use the present-day Earth’s CMB temperature, i.e., 4000 K, as a lower bound for an Earth-sized lava planet’s CMB temperature in the cold-core case. For the hot-core scenario, the temperature increase with depth is due to the isentropic compression of the material. In regions hotter than the liquidus, the temperature follows a one-phase homogeneous isentrope (or adiabat). When the temperature is between the liquidus and the solidus, entropy conservation must account for the latent heat of fusion. In this region, the temperature follows a two-phase isentrope, akin to moist adiabats of planetary atmospheres. For a surface temperature of 3000 K in a hot-core scenario, the silicate mantle is expected to be fully molten for a planet the size of Earth or a 1.5R ⊕ super-Earth. For the same surface temperature, the magma ocean is still expected to be 1000 km deep below the substellar point for an Earth-sized lava planet, even if the CMB temperature is as low as 4000 K. For a surface temperature of 2400 K, the adiabat intersects the liquidus at a depth of about 100 km for a 1.5R ⊕ super-Earth. However, the adiabat remains very close to the liquidus at greater depth, such that the interior is still expected to be mostly molten in a hot-core case (see Figure 3).
Paper: Deep Two-phase, Hemispherical Magma Oceans on Lava Planets
Authors: Charles-Édouard Boukaré, Nicolas B. Cowan, James Badro
Figure caption: Lateral variation of the surface composition of tidally locked lava planets. Concentrations of SiO2 (yellow), FeO (red), Na2O (green), H20 (blue), and K2O (black) as a function of surface temperature (bottom axis) or distance from the substellar point on K2-141b (top axis). There is no well-defined magma ocean shore, but rather a gradual transition from the molten to the solid hemisphere. In this partially molten region, the composition of the magma changes, as precipitating minerals do not have the same composition as the melt. Depending on the style of convective dynamics, these chemical heterogeneities can be mixed back into the convective region or permanently hidden from the surface. For instance, enrichment in FeO would promote the formation of very dense melt that might sink to the bottom of the magma ocean (Kite et al. 2016). Additionally, the concentration of volatile species, such as H2O and CO2, can eventually reach the saturation limit in the melt near the solidus. When the melt is saturated, any increase in concentration results in the formation of bubbles that degas at the surface of the planet, with possible implications for transit observations of lava planets.
Paper: Deep Two-phase, Hemispherical Magma Oceans on Lava Planets
Authors: Charles-Édouard Boukaré, Nicolas B. Cowan, James Badro
Figure caption: Schematic of the interior structure and dynamics of a lava planet in the hot-core scenario (see the main text). The hemispherical magma ocean on the dayside could extend down to the CMB. The nightside mantle is solid. A partially molten region probably connects the two hemispheres. The illustrated pseudo-steady-state structure involves fluid motions. The solid–liquid interfaces are not static, rather rocky materials are expected to flow through the solid–liquid interface, melting or solidifying at these boundaries, depending on the flow direction. The surface temperature gradient drives the magma currents between the dayside and the nightside. Temperature differences between the CMB and the planetary surface are expected to drive convection of the rocky mantle. Geodynamic models are required to explore the horizontal convective dynamics, as well as the efficiency of the solid–liquid phase separation and chemical mixing.
Paper: Deep Two-phase, Hemispherical Magma Oceans on Lava Planets
Authors: Charles-Édouard Boukaré, Nicolas B. Cowan, James Badro
Figure caption: The melt fraction as a function of depth for four surface temperatures: 3000, 2400, 1900, and 1700 K. The rheological transition between solid-like and liquid-like behavior occurs at about a 50% melt fraction. For the hot-core case (see the main text), the bulk of the magma ocean therefore behaves as a sluggish fluid—not a solid—for surface temperatures as low as 1700 K. For the cold-core scenario (see the main text), the magma behaves as a liquid down to 50 GPa for a substellar temperature of 3000 K, but only a shallow magma ocean of about 100 km remains for a surface temperature of 1900 K.
Paper: Deep Two-phase, Hemispherical Magma Oceans on Lava Planets
Authors: Charles-Édouard Boukaré, Nicolas B. Cowan, James Badro
Figure caption: High-pressure liquidus (red) and solidus (blue) temperatures for Earth-like mantle compositions. Above the liquidus temperature, silicates are liquid. When the temperature lies between the liquidus and the solidus, silicates are partially molten. Silicates fully solidify when the temperature drops below the solidus. The colored symbols show recent experimental measurements (Zhang & Herzberg 1994; Fiquet et al. 2010; Andrault et al. 2011, 2014) and theoretical calculations (Usui & Tsuchiya 2010; Boukaré et al. 2015) of the liquidus and solidus temperatures at high pressures. Discrepancies among the data in the literature arise from the differences in approaches, such as the silicate compositions or melt detection techniques. For the sake of simplicity, we approximate the liquidus and solidus curves for Earth-like composition using the red and blue lines, Equations (1) and (2). On the left, pressure–depth conversions are shown for the Earth and a 1.5R ⊕ super-Earth. Note that the melting curve of pure SiO2, shown by the green asterisks, substantially overestimates the liquidus temperature of the BSE.
Paper: Constraining the Physical Properties of Stellar Coronal Mass Ejections with Coronal Dimming: Application to Far-ultraviolet Data of ϵ Eridani
Authors: R. O. Parke Loyd, James Paul Mason, Meng Jin, Evgenya L. Shkolnik, Kevin France, Allison Youngblood, Jackie Villadsen, Christian Schneider, Adam C. Schneider, Joe Llama, Tahina Ramiaramanantsoa, Tyler Richey-Yowell
Figure caption: 2015 February epoch lightcurves of the HST observations from program 13650. Point colors indicate the different methods used to measure the Fe line fluxes as demonstrated in Figures 4 and 5. The black lines are reference lightcurves from summing the flux of two of the brightest FUV lines. Possible dimming profiles explored by the Markov chain Monte Carlo (MCMC) sampler are shown as the translucent regions matched to the color of the points fit, with the best fit for Fe XXI shown as the solid green line.
Paper: Constraining the Physical Properties of Stellar Coronal Mass Ejections with Coronal Dimming: Application to Far-ultraviolet Data of ϵ Eridani
Authors: R. O. Parke Loyd, James Paul Mason, Meng Jin, Evgenya L. Shkolnik, Kevin France, Allison Youngblood, Jackie Villadsen, Christian Schneider, Adam C. Schneider, Joe Llama, Tahina Ramiaramanantsoa, Tyler Richey-Yowell
Figure caption: Two contrasting emission measure distributions (EMDs) for ϵ Eri (blue curve and orange dots) compared against the emissivity, G(T, n) (black curves), of Fe XII and Fe XXI in a solar-metallicity plasma. The EMD from Coffaro et al. (2020) is based on X-ray data obtained simultaneous with the FUV data in 2015 February. The emissivities are normalized to peak at the same level and only the top two orders of magnitude are plotted. Dotted curves show the contribution functions for each ion under the two different EMDs. Regardless of which EMD is used, the contribution functions peak very near the peak emissivity, justifying the assumption that ﹩G={G}_{\max }﹩ in our order-of-magnitude estimates.
Paper: Constraining the Physical Properties of Stellar Coronal Mass Ejections with Coronal Dimming: Application to Far-ultraviolet Data of ϵ Eridani
Authors: R. O. Parke Loyd, James Paul Mason, Meng Jin, Evgenya L. Shkolnik, Kevin France, Allison Youngblood, Jackie Villadsen, Christian Schneider, Adam C. Schneider, Joe Llama, Tahina Ramiaramanantsoa, Tyler Richey-Yowell
Figure caption: Demonstration of the three methods used to integrate the Fe XXI line. The profiles here correspond to the fifth set of points in Figure 6. The C I line shown in the bottom panel is meant only to represent the subtracted flux; no line fit was actually made. Curve thickness represents uncertainty in the top panel.
Paper: Constraining the Physical Properties of Stellar Coronal Mass Ejections with Coronal Dimming: Application to Far-ultraviolet Data of ϵ Eridani
Authors: R. O. Parke Loyd, James Paul Mason, Meng Jin, Evgenya L. Shkolnik, Kevin France, Allison Youngblood, Jackie Villadsen, Christian Schneider, Adam C. Schneider, Joe Llama, Tahina Ramiaramanantsoa, Tyler Richey-Yowell
Figure caption: Derived ejected emitting masses that could explain the data following the flare in Figure 6 if a CME occurred. Note the disparate axis scales: logarithmic on the left, linear on the right. Vertical gray lines are the 18th, 50th, and 84th percentiles.
Paper: Constraining the Physical Properties of Stellar Coronal Mass Ejections with Coronal Dimming: Application to Far-ultraviolet Data of ϵ Eridani
Authors: R. O. Parke Loyd, James Paul Mason, Meng Jin, Evgenya L. Shkolnik, Kevin France, Allison Youngblood, Jackie Villadsen, Christian Schneider, Adam C. Schneider, Joe Llama, Tahina Ramiaramanantsoa, Tyler Richey-Yowell
Figure caption: Simultaneous fit to C I and Fe XXI lines for deblending. We constrained the blended C I profile to have the same broadening as the unblended C I lines. The thickness of the model curves (blue) represents uncertainty.
Paper: Constraining the Physical Properties of Stellar Coronal Mass Ejections with Coronal Dimming: Application to Far-ultraviolet Data of ϵ Eridani
Authors: R. O. Parke Loyd, James Paul Mason, Meng Jin, Evgenya L. Shkolnik, Kevin France, Allison Youngblood, Jackie Villadsen, Christian Schneider, Adam C. Schneider, Joe Llama, Tahina Ramiaramanantsoa, Tyler Richey-Yowell
Figure caption: CME velocities at 20 R ⊙ that could explain the drop in Fe XXI emission following the flare in Figure 6, assuming constant acceleration and self-similar expansion. Variable acceleration and expansion, influenced by ambient stellar wind conditions and not probed by this technique, will modify the true velocity at 20 R ⊙. Vertical gray lines are the 18th, 50th, and 84th percentiles.
Paper: Constraining the Physical Properties of Stellar Coronal Mass Ejections with Coronal Dimming: Application to Far-ultraviolet Data of ϵ Eridani
Authors: R. O. Parke Loyd, James Paul Mason, Meng Jin, Evgenya L. Shkolnik, Kevin France, Allison Youngblood, Jackie Villadsen, Christian Schneider, Adam C. Schneider, Joe Llama, Tahina Ramiaramanantsoa, Tyler Richey-Yowell
Figure caption: Demonstration of the two methods used to integrate Fe XII. The profiles here correspond to the fifth set of points in Figure 6. Curve thickness represents uncertainty in the top panel.
Paper: Constraining the Physical Properties of Stellar Coronal Mass Ejections with Coronal Dimming: Application to Far-ultraviolet Data of ϵ Eridani
Authors: R. O. Parke Loyd, James Paul Mason, Meng Jin, Evgenya L. Shkolnik, Kevin France, Allison Youngblood, Jackie Villadsen, Christian Schneider, Adam C. Schneider, Joe Llama, Tahina Ramiaramanantsoa, Tyler Richey-Yowell
Figure caption: 2015 February epoch MCMC chains from the fit to the Fe XII data in Figure 6. Symbols are the pre-flare flux, F pre (10−15 erg s−1 cm−2); CME acceleration, a (m s−2); dimming depth, ﹩{\delta }_{\max }﹩ (relative units); and the white noise hyperparameter, σ (relative units).
Paper: Constraining the Physical Properties of Stellar Coronal Mass Ejections with Coronal Dimming: Application to Far-ultraviolet Data of ϵ Eridani
Authors: R. O. Parke Loyd, James Paul Mason, Meng Jin, Evgenya L. Shkolnik, Kevin France, Allison Youngblood, Jackie Villadsen, Christian Schneider, Adam C. Schneider, Joe Llama, Tahina Ramiaramanantsoa, Tyler Richey-Yowell
Figure caption: 2015 February epoch MCMC chains from the fit to the Fe XXI data in Figure 6. Symbols are the pre-flare flux, F pre (10−15 erg s−1 cm−2); CME acceleration, a (m s−2); dimming depth, ﹩{\delta }_{\max }﹩ (relative units); and the white noise hyperparameter, σ (relative units).
Paper: A New Census of the 0.2 < z < 3.0 Universe. II. The Star-forming Sequence
Authors: Joel Leja, Joshua S. Speagle, 佳士 沈, Yuan-Sen Ting, 源森 丁, Benjamin D. Johnson, Charlie Conroy, Katherine E. Whitaker, Erica J. Nelson, Pieter van Dokkum, Marijn Franx
Figure caption: The median shift in inferred values of logM* and logSFR between the Prospector-α model and FAST stellar masses/UV+IR SFRs for galaxies at 0.7 < z < 1.3. Only cells with N > 20 galaxies are shown. The masses increase by ∼0.2 dex due to the use of nonparametric star formation histories. The inferred SFRs decrease by 0.1–1+ dex largely due to dust heating from old stars, though other effects can contribute substantially in certain regimes (see Section 6.2 for an in-depth discussion). The ridgeline of the star-forming sequence as measured in this work is shown as a black dashed line. The color bar traces the angle of the shift in logM–logSFR space, where θ = 0 is a horizontal arrow pointing to the right.
Paper: A New Census of the 0.2 < z < 3.0 Universe. II. The Star-forming Sequence
Authors: Joel Leja, Joshua S. Speagle, 佳士 沈, Yuan-Sen Ting, 源森 丁, Benjamin D. Johnson, Charlie Conroy, Katherine E. Whitaker, Erica J. Nelson, Pieter van Dokkum, Marijn Franx
Figure caption: The median difference in the coefficients to the UV+IR SFR in Equation (11) between Prospector-α model and the fixed template-based coefficients from Bell et al. (2005) is shown for galaxies at 0.7 < z < 1.3. α parameterizes the total energy output of young stars, δ parameterizes the fraction of IR luminosity which is powered by energy from young stars, and γ parameterizes the conversion from the observed UV luminosity to the bolometric luminosity of the young stars after dust attenuation. Arrows on the color bar indicate where the data is clipped to enhance the information content of the map. The y-axis shows the SFR averaged over the most recent 100 Myr.
Paper: A New Census of the 0.2 < z < 3.0 Universe. II. The Star-forming Sequence
Authors: Joel Leja, Joshua S. Speagle, 佳士 沈, Yuan-Sen Ting, 源森 丁, Benjamin D. Johnson, Charlie Conroy, Katherine E. Whitaker, Erica J. Nelson, Pieter van Dokkum, Marijn Franx
Figure caption: This figure compares the redshift evolution of sSFR for a log(M/M ⊙) = 10 galaxy on the star-forming sequence between observations and galaxy formation simulations. The specific dark matter accretion rate from the Millennium simulation is also shown for reference (Fakhouri et al. 2010). The left panel shows previous observational star-forming sequences, which have a ∼0.4 dex offset with the simulations. The right panel shows results from this work, which resolve these systematic differences.
Paper: A New Census of the 0.2 < z < 3.0 Universe. II. The Star-forming Sequence
Authors: Joel Leja, Joshua S. Speagle, 佳士 沈, Yuan-Sen Ting, 源森 丁, Benjamin D. Johnson, Charlie Conroy, Katherine E. Whitaker, Erica J. Nelson, Pieter van Dokkum, Marijn Franx
Figure caption: Comparing the star-forming sequence derived in this work with other results from the literature. In general, the star-forming sequence inferred here has a normalization well below previous results. This is due to the methodology by which the stellar masses and SFRs are inferred—see Section 6.2 for further discussion.
Paper: DRAFT: A Method for Wave Analyses in Space Plasmas
Authors: W. Z. Zhang, H. S. Fu, J. B. Cao, Y. Y. Liu, J. S. Zhao, Z. Z. Guo, Z. Wang, T. Y. Wang
Figure caption: Overview for the plasma and magnetic field measurements from MMS 1 in case 2018 April 16 and case 2017 October 07. (a–b, j–k) The position of MMS in GSE coordinates. (c, l) The magnetic field in GSE coordinates. (d, m) The electron density. (e, n) The ion velocity. (f, o) The omnidirectional differential energy flux of ions. (g, p) The power spectral density of the magnetic field. (h, q) A close-up view of the magnetic field B  z  during 10:40:40–10:41:30 UT in case 2018 April 16 and B  x  during 14:03:20–14:03:40 UT in case 2017 October 07. (i, r) A close-up view of the power spectral density.
Paper: DRAFT: A Method for Wave Analyses in Space Plasmas
Authors: W. Z. Zhang, H. S. Fu, J. B. Cao, Y. Y. Liu, J. S. Zhao, Z. Z. Guo, Z. Wang, T. Y. Wang
Figure caption: Multispacecraft timing results of two single-frequency waves at specific time instants in two cases. (a–b, e–f) The relative position of four MMS satellites. (c, d, g, h) The waveform before and after time-shift processes. The results wave phase velocity, wavevector, and wave normal angle calculated by timing method, and the three error parameters (λ/2R  sc , CC, MOA) are given at the bottom.
Paper: DRAFT: A Method for Wave Analyses in Space Plasmas
Authors: W. Z. Zhang, H. S. Fu, J. B. Cao, Y. Y. Liu, J. S. Zhao, Z. Z. Guo, Z. Wang, T. Y. Wang
Figure caption: Wave analysis results by using our method. (a, e) The average wave power spectrum density of magnetic field from four spacecraft. (b, f) The wave phase velocity. (c, g) The wave propagation direction. (d, h) The wave normal vector. Since we used only magnetic field components, there is a 180° ambiguity in the wave normal determination, and we converted all wave normal directions into values less than 90°.
Paper: DRAFT: A Method for Wave Analyses in Space Plasmas
Authors: W. Z. Zhang, H. S. Fu, J. B. Cao, Y. Y. Liu, J. S. Zhao, Z. Z. Guo, Z. Wang, T. Y. Wang
Figure caption: Error parameters. (a, d) Ratio of half-wavelength to spacecraft separation (λ/2R sc). (b, e) CC. (c, f) MOA.
Paper: DRAFT: A Method for Wave Analyses in Space Plasmas
Authors: W. Z. Zhang, H. S. Fu, J. B. Cao, Y. Y. Liu, J. S. Zhao, Z. Z. Guo, Z. Wang, T. Y. Wang
Figure caption: Wave normal angle solved by DRAFT, SVD, and Means methods. (a, d) The wave normal angle solved by DRAFT. (b, e) The wave normal angle solved by the SVD method. (c, f) The wave normal angle solved by the Means method.
Paper: DRAFT: A Method for Wave Analyses in Space Plasmas
Authors: W. Z. Zhang, H. S. Fu, J. B. Cao, Y. Y. Liu, J. S. Zhao, Z. Z. Guo, Z. Wang, T. Y. Wang
Figure caption: The dispersion relation of the Alfvén wave solved by the DRAFT method in case 2018 April 16. (a–c) The wave power in the ion rest frame between different wave normal angles (0°–30°, 30°–60°, and 60°–90°). (d–f) The sampling counts in the ion rest frame between different wave normal angles (0°–30°, 30°–60°, and 60°–90°).
Paper: DRAFT: A Method for Wave Analyses in Space Plasmas
Authors: W. Z. Zhang, H. S. Fu, J. B. Cao, Y. Y. Liu, J. S. Zhao, Z. Z. Guo, Z. Wang, T. Y. Wang
Figure caption: Three-dimensional  K -spectrum of the Alfvén wave in case 2018 April 16. (a) Wave power spectral density drawn in three-dimensional wavevector space. (b–d) Wave power spectral density sliced respectively from k  z , k  x , and k  y  direction.
Paper: Ultrawide Black Hole—Neutron Star Binaries as a Possible Source for Gravitational Waves and Short Gamma-Ray Bursts
Authors: Erez Michaely, Smadar Naoz
Figure caption: The merger probability of a BHNS with m BH = 10 M ⊙ and m NS = 1.5 with flyby mass m  p  = 0.6 M ⊙ and v enc = 50 km s−1. The stellar density number is n * = 0.1 pc−3. The probability calculated after t = 10 Gyr since the BHNS was formed. The peak probability is achieved at a = a crit. For binaries with tighter orbits the merger probability drops because it is harder to change their orbital parameters. For binaries with a > a crit the probability decreases because of the loss cone dependency with a, see text.
Paper: Ultrawide Black Hole—Neutron Star Binaries as a Possible Source for Gravitational Waves and Short Gamma-Ray Bursts
Authors: Erez Michaely, Smadar Naoz
Figure caption: The two distance scales b kick (dashed red) and b impulse (solid black). Each flyby with b < b kick will fill the loss cone and each one with b < b impulse will interact impulsively with the wide BHNS binary. We are interested in the gray area, which insures both conditions. Calculated for binary with m BH = 10 M ⊙ and m NS = 1.5 with v enc = 60 km s−1. The stellar density number is n * = 0.1 pc−3.
Paper: No Self-shadowing Instability in 2D Radiation Hydrodynamical Models of Irradiated Protoplanetary Disks
Authors: Julio David Melon Fuksman, Hubert Klahr
Figure caption: Planck-averaged τ = 1 surfaces for vertical radiative transport (dashed red lines), frequency-dependent τ = 1 surfaces integrated along r for stellar irradiation (thin blue lines), Planck-averaged τ = 1 surfaces for stellar irradiation (thick orange lines), and pressure scale height z = H surfaces (green dashed–dotted lines) in the hydrostatic runs with t iter = 100 yr. The temperature and reduced radiation flux distributions are represented in gray scale for comparison. The alpha factor used for the transparency of the τ = 1 lines is proportional to the contribution of each frequency to the total irradiation power.
Paper: No Self-shadowing Instability in 2D Radiation Hydrodynamical Models of Irradiated Protoplanetary Disks
Authors: Julio David Melon Fuksman, Hubert Klahr
Figure caption: 2D temperature profiles in log scale for all hydrostatic runs with ﹩\hat{c}={10}^{-4}﹩. Distributions are shown after 35 iterations for t iter = 100, 10, and 1 yr (top three rows) and 400 iterations for t iter = 0.1 (bottom row). Videos made with snapshots of these runs at different iterations for t iter = 1 and 100 yr can be found in https://youtu.be/RT8IFe8W13g.
Paper: No Self-shadowing Instability in 2D Radiation Hydrodynamical Models of Irradiated Protoplanetary Disks
Authors: Julio David Melon Fuksman, Hubert Klahr
Figure caption: Hydrostatic T(θ) profiles at different radii for each f dg, computed after 35 iterations with t iter = 100 yr.