adsabs/AstroCLIMB huggingface dataset:
Paper: A New Brown Dwarf Orbiting an M Star and an Investigation of the Eccentricity Distribution of Transiting Long-period Brown Dwarfs
Authors: Tianjun Gan, Charles Cadieux, Shigeru Ida, Sharon X. Wang, Shude Mao, Zitao Lin, Keivan G. Stassun, Adam J. Burgasser, Steve B. Howell, Catherine A. Clark, Ivan A. Strakhov, Paul Benni, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Luc Arnold, Étienne Artigau, David Charbonneau, Karen A. Collins, Neil J. Cook, Zoë L. de Beurs, Sarah J. Deveny, John P. Doty, René Doyon, Colin Littlefield, Tyler Pritchard, Gabrielle Ross, Avi Shporer, Christopher R. Theissen, Benjamin M. Tofflemire, Andrew Vanderburg, David Watanabe
Figure caption: Left panel: the eccentricity and mass diagram of all confirmed transiting brown dwarfs and low-mass stars colored by the orbital period. Two vertical black dashed lines mark the mass range (42.5 MJ ≤ Mc ≤ 110 MJ) where the companions are more likely to have large eccentricities (see Section 3.3 for details). Right panel: same as the left but for the companion-to-host mass ratio. In both panels, TOI-5575 b is shown as a red star.
Paper: Spectral Evolution of Pickup Ions across Interplanetary Shocks in the Outer Heliosphere: Observational Constraints and Transport Simulations
Authors: Weining Wang, Jiansen He, Die Duan, Zhongwei Yang, Linghua Wang, Hui Li
Figure caption: Comparative analysis of simulated and observed PUI energy spectra of count rates. Detailed comparison of the simulated energy spectra of PUIs against observations from SWAP at various heliocentric distances: 22.75 au, 31.87 au, 36.68 au, and 40.05 au. The upstream and downstream energy spectra of ions originating from the core solar wind are depicted with blue dashed and green dashed lines, respectively, while their simulated counterparts are represented by red dashed lines. The PUIs’ energy spectra are illustrated with blue solid lines upstream and green solid lines downstream, with the corresponding simulated spectra in red solid lines. The parameters, including the perpendicular mean free path (λ⊥) and velocity diffusion coefficient (D), along with the upstream and downstream flow velocities (vsw,u, vsw,d), upstream spectral index (ηu), and upstream cooling index (αu), offer a comprehensive view of the simulation settings. The downstream spectral indices (ηd) and downstream cooling index (αd) for both observational and simulation PUI spectra are listed for comparison.
Paper: Spectral Evolution of Pickup Ions across Interplanetary Shocks in the Outer Heliosphere: Observational Constraints and Transport Simulations
Authors: Weining Wang, Jiansen He, Die Duan, Zhongwei Yang, Linghua Wang, Hui Li
Figure caption: (a) PUI temperature as a function of the solar wind speed color coded with subadiabatic index β. (b) Proportion of the suprathermal PUIs as a function of the power-law index η, color coded with subadiabatic index β. (c) Normalized energy spectra of PUI count rates with different subadiabatic indices. (d) Energy spectra of PUI count rates with different suprathermal tail spectrum indices.
Paper: Spectral Evolution of Pickup Ions across Interplanetary Shocks in the Outer Heliosphere: Observational Constraints and Transport Simulations
Authors: Weining Wang, Jiansen He, Die Duan, Zhongwei Yang, Linghua Wang, Hui Li
Figure caption: (a) Histogram depicting the ratio of the power-law index of the suprathermal energy spectrum in the upstream to that in the downstream (﹩\frac{{\eta }_{u}}{{\eta }_{d}}﹩). (b) Values of ηu/ηd, which represent the ratio of the power-law indices of the suprathermal tail energy spectra of PUIs upstream and downstream of interplanetary shocks, with different compression ratios, exhibit a correlation coefficient of 0.78. (c) Histogram showing the change in the subadiabatic index during shock crossings, with an increase in β occurring in 59% of cases and a decrease in 41% of cases. (d) Positive correlation between the change of the fraction of the suprathermal PUIs and downstream β values, with a correlation coefficient of 0.68.
Paper: Spectral Evolution of Pickup Ions across Interplanetary Shocks in the Outer Heliosphere: Observational Constraints and Transport Simulations
Authors: Weining Wang, Jiansen He, Die Duan, Zhongwei Yang, Linghua Wang, Hui Li
Figure caption: The fitted daily ion distribution on 2017 November 28–29, when NH was at 40.05 au. The solar wind proton (H+), alpha particle (He++), and He+ peaks are shown in light blue, and their respective centroids are indicated by vertical dashed lines. PUI populations of H+ (blue) and He+(yellow) are fitted according to Equation (3).
Paper: Spectral Evolution of Pickup Ions across Interplanetary Shocks in the Outer Heliosphere: Observational Constraints and Transport Simulations
Authors: Weining Wang, Jiansen He, Die Duan, Zhongwei Yang, Linghua Wang, Hui Li
Figure caption: Simulation of PUI count rate spectra under varying diffusion conditions. (a) Simulation outcomes for PUIs with distinct perpendicular mean free paths (λ⊥) when the velocity diffusion coefficient ﹩\bar{D}=1.33\times 1{0}^{-9}\,{{\rm{s}}}^{-1}﹩. (b) Simulation results for PUIs with different perpendicular mean free paths when ﹩\bar{D}=6.67\times 1{0}^{-9}\,{{\rm{s}}}^{-1}﹩. (c) Simulation results for PUIs with different velocity diffusion coefficients when λ⊥ = 3.75 × 10−3 au. (d) Simulation results for PUIs with different velocity diffusion coefficients when λ⊥ = 1.125 × 10−2 au.
Paper: Spectral Evolution of Pickup Ions across Interplanetary Shocks in the Outer Heliosphere: Observational Constraints and Transport Simulations
Authors: Weining Wang, Jiansen He, Die Duan, Zhongwei Yang, Linghua Wang, Hui Li
Figure caption: Flowchart and results of the simulation for PUIs traversing the shock at the heliocentric distance of 40.05 au. We show a 2D surface plot of the 3D isotropic PUI velocity distribution in the solar wind flow reframe upstream of the shock (a) and downstream of the shock (b) with different velocity ranges color coded by different colors. We show a 1D cut of the 3D PUI velocity distribution in the solar wind flow frame upstream of the shock (c) and downstream of the shock (d). Also shown is the integrated energy spectrum for the count rate of PUIs in the spacecraft reference frame upstream of the shock (e) and downstream of the shock (f). The fraction of each velocity range contributing to the suprathermal ions downstream of the shock is listed in panel (f).
Paper: Spectral Evolution of Pickup Ions across Interplanetary Shocks in the Outer Heliosphere: Observational Constraints and Transport Simulations
Authors: Weining Wang, Jiansen He, Die Duan, Zhongwei Yang, Linghua Wang, Hui Li
Figure caption: Four sets of fitted PUI energy spectra derived from SWAP observations, both before and after the crossing of interplanetary shocks at heliocentric distances of 22.75 au, 31.87 au, 36.68 au, and 40.05 au. Each panel contains multiple curves representing different components: SWAP data in the upstream region (blue), fitted H+ PUI components in the upstream region (green), SWAP data in the downstream region (red), and fitted H+ PUI components in the downstream region (yellow).
Paper: Spectral Evolution of Pickup Ions across Interplanetary Shocks in the Outer Heliosphere: Observational Constraints and Transport Simulations
Authors: Weining Wang, Jiansen He, Die Duan, Zhongwei Yang, Linghua Wang, Hui Li
Figure caption: Monte Carlo simulation and statistical analysis of PUI particles traversing the shock. (a) Trajectories of typical PUI particles in the (x, log(E)) space with different shock-crossing times (e.g., N = 1, 3, 5, 7, 11, 13). To separate different trajectories, we add an offset to each particle’s energy ﹩{E}_{i}^{\prime} ={E}_{i}+{E}_{{\rm{offset}}}﹩. (b) Percentage histogram for the PUI particles with different shock-crossing times.
Paper: Origins of Carbon Dust in a JWST-observed Primeval Galaxy at z ∼ 6.7
Authors: Ambra Nanni, Michael Romano, Darko Donevski, Joris Witstok, Irene Shivaei, Michel Fioc, Prasad Sawant
Figure caption: Comparison between the observed spectrum of JADES-GS-z6-0 (black points with uncertainties) and the best-fit predicted spectrum from self-consistent chemical evolution of the ISM: (left panel) spectrum predicted with fburst = 30%, ﹩{f}_{{\rm{SN}}}=10﹩%, M* = 8 × 108 M⊙ and dust growth in the ISM (red curve); (right panel) spectrum predicted with fburst = 25%, ﹩{f}_{{\rm{SN}}}=75﹩%, M* = 9 × 108 M⊙ and without dust growth in the ISM (blue curve).
Paper: Origins of Carbon Dust in a JWST-observed Primeval Galaxy at z ∼ 6.7
Authors: Ambra Nanni, Michael Romano, Darko Donevski, Joris Witstok, Irene Shivaei, Michel Fioc, Prasad Sawant
Figure caption: Left panel: time evolution normalized mass of the PAHs needed to reproduce the UV bump (black line) for the same scenario of dust evolution as in Figure 1 (left panel) compared with the total carbon dust produced by SNe (mostly Type II; dotted line), AGB stars (dashed line), and dust growth (solid line). The amount of dust is reduced by destruction by SNe (see the text). The magenta lines represent the evolution of PAHs in the ISM that does not include growth and injection from stellar sources. The star symbol represents the total carbon dust mass over stellar mass at the end point of the simulation that provides the best fit for JADES-GS-z6-0. Right panel: same as in the left panel, but for the case without growth in the ISM (see Figure 1, right panel).
Paper: Origins of Carbon Dust in a JWST-observed Primeval Galaxy at z ∼ 6.7
Authors: Ambra Nanni, Michael Romano, Darko Donevski, Joris Witstok, Irene Shivaei, Michel Fioc, Prasad Sawant
Figure caption: Redshift evolution of galaxy UV slope (β) estimated for distant galaxies observed with JWST. The green symbols represent median values of a sample from A. Saxena et al. (2024); error bars correspond to the observed scatter in the data. Overplotted are predictions from our two best models that reproduce the β slope at the redshift of JADES-GS-z6-0. Modeled tracks with and without ISM growth included are shown with red and blue lines, respectively.
Paper: Fine-tuned Supernova or Failed Explosion? Decoding the Origins of the G3425 Binary
Authors: Zsolt Regály, Viktória Fröhlich, József Vinkó
Figure caption: Analytical modeling of the G3425 progenitor system. In panel (a), the analytical solutions for the initial eccentricity, e0, as a function of the progenitor mass, M1, are shown assuming zero final eccentricity (i.e., e1 = 0). Solid and dashed lines correspond to the minimum and maximum remnant-secondary pairs for a given SN scenario, respectively. Plausible progenitor solutions are in the shaded regions for each SN scenario, which are indicated in the legend. Panel (b) shows the final eccentricity as a function of the orbital position of the secondary at the moment of the SN explosion using ﹩{M}_{1}^{{\prime} }﹩ and e0 values indicated on panel (a). Models with high or low e0 assume M2 = 3.84 M⊙ and M2 = 1.7 M⊙, respectively. The eccentricity of G3425 is shown with a red shaded region. Panels (c) and (d) show the final eccentricity as a function of the initial eccentricity of the system for SN II and SN Ib/c scenarios, respectively, assuming that the SN explosion occurs when the secondary is at the apocenter. The mass parameters for each scenario are shown in the legend. Solid lines represent models where the secondary’s mass remains constant, while dashed lines represent models where 1 M⊙ mass loss is assumed for the secondary due to interaction with the expanding SN envelope. The teal line represents the e1 = e0, meaning that eccentricity damping occurs below this line during the SN explosion.
Paper: Fine-tuned Supernova or Failed Explosion? Decoding the Origins of the G3425 Binary
Authors: Zsolt Regály, Viktória Fröhlich, József Vinkó
Figure caption: The final vs. initial eccentricity and the growth of the semimajor axis of the secondary are illustrated, under the assumption of different unseen remnant masses. The left and right plots illustrate SN-II and SN Ib/c scenarios, respectively. Blue and magenta colors represent the heaviest (﹩{M}_{1}^{{\prime} }=3.48\,{M}_{\odot }﹩, M2 = 3.84 M⊙) and lightest (﹩{M}_{1}^{{\prime} }=2.9\,{M}_{\odot }﹩, M2 = 1.7 M⊙) SN II models, respectively. Orange and black colors represent the heaviest (﹩{M}_{1}^{{\prime} }=4.4\,{M}_{\odot }﹩, M2 = 3.84 M⊙) and lightest (﹩{M}_{1}^{{\prime} }=3.48\,{M}_{\odot }﹩, M2 = 1.7 M⊙) SN II models, respectively. Dashed lines correspond to the analytical solution, while symbols represent numerical models. Open square and circle symbols represent the homologous envelope expansion model with 6000 km s−1 and 30,000 km s−1 expansion velocity, respectively. Panels illustrate scenarios where the mass loss occurs at pericenter (panels (a1), (a3), (b1), and (b3)), intermediate position (panels (a2), (a4), (b2), and (b4)), apocenter (panels (c1), (c3), (d1), and (d3)), and ±10° departure from apocenter (panels (c2), (c4), (d2), and (d4)). The teal colored line serves as a reference, with dampened and excited eccentricity indicated below and above it, respectively. The red shaded regions indicate the observed eccentricity of the secondary 0.05 ± 0.01.
Paper: Fine-tuned Supernova or Failed Explosion? Decoding the Origins of the G3425 Binary
Authors: Zsolt Regály, Viktória Fröhlich, József Vinkó
Figure caption: Ranges of initial eccentricity, e0, calculated according to Equation (A11) on the ﹩{M}_{1}^{{\prime} }-{M}_{2}﹩ plane assuming three different progenitor masses of M1 = 7.5, 14 and 25 M⊙. Plausible solutions for e0 at a given ﹩{M}_{1}^{{\prime} }﹩, M2 are in the shaded regions.
Paper: Fine-tuned Supernova or Failed Explosion? Decoding the Origins of the G3425 Binary
Authors: Zsolt Regály, Viktória Fröhlich, József Vinkó
Figure caption: The mass inside the secondary’s orbit, Min, as a function of time in the four core collapse SN scenarios. Three different progenitor masses are assumed in each scenario, as indicated by the colors in the legend. Solid and dashed lines correspond to expansion velocities of 60,000 and 300,000 km s−1, respectively.
Paper: Fine-tuned Supernova or Failed Explosion? Decoding the Origins of the G3425 Binary
Authors: Zsolt Regály, Viktória Fröhlich, József Vinkó
Figure caption: Panel (a): probability density functions given by Equation (C1) for various eccentricities shown with different colors. Panel (b): probability that the secondary is found at a given true anomaly range, as a function of orbital eccentricity.
Paper: Hydrogen Loss on Venus Driven by Photochemistry
Authors: Hao Gu, Jun Cui, Xiaoshu Wu, Xu Huang, Shiqi Wu, Wenlong Li, Jinjin Zhao, Haoyu Lu, Lei Li
Figure caption: Model inputs used in our model calculations, appropriate for the dayside averaged situation at solar maximum, median, and minimum conditions, from left to right. Panels (a)–(c): density profiles of six background species, including CO2, O, CO, N2, N, and He, along with the density profiles of Ar and H2O. Panel (d): temperature profiles of neutrals, ions, and electrons, denoted as Tn, Ti, and Te, respectively. Panel (e): solar EUV and SXR spectra imposed at the top of the Venusian atmosphere, spanning a common wavelength range of 0.05–189.95 nm with a resolution of 0.1 nm. Panel (f): photoelectron energy spectra in both upward (solid) and downward (dashed) directions within the dayside Venusian ionosphere at two representative altitudes, as specified in the figure legend. In panels (d) and (e), the solid, dashed, and dotted lines represent solar maximum, median, and minimum conditions, respectively.
Paper: Impact of Two-population α-particle Distributions on Plasma Stability
Authors: Mihailo M. Martinović, Kristopher G. Klein, Rossana De Marco, Daniel Verscharen, Roberto Bruno, Raffaella D'Amicis
Figure caption: Overview of the VDF parameters used for stability analysis on 2022 March 2. Panels(a)–(c) show the VDF parameters used as input for the stability analysis. Density normalized to npc, velocity drift normalized to vA, and temperature anisotropy T⊥/T∥ are shown for the proton core (black), proton beam (cyan), and α particles as a single population (green), α core (brown), and α beam (purple). Panels (d) and (e) show the results of PLUMAGE stability analysis—the normalized growth rates and directions of most unstable modes with respect to the magnetic field and solar wind speed in the spacecraft frame, respectively, for both models. Panel (f) shows the basis for verification of the results, as the intervals where the measured magnetic field polarization in the spacecraft frame marks a clear presence of coherent waves—σ > 0.6 or σ < −0.6 (Equation (3))—are marked in black.
Paper: Hydrogen Loss on Venus Driven by Photochemistry
Authors: Hao Gu, Jun Cui, Xiaoshu Wu, Xu Huang, Shiqi Wu, Wenlong Li, Jinjin Zhao, Haoyu Lu, Lei Li
Figure caption: The outputs of our photochemical model and TPMC simulations for solar maximum, median, and minimum conditions, from left to right. Top: the density profiles of five representative protonated species (OH+, H2O+, HN﹩{}_{2}^{+}﹩, HCO+, and HOCO+), along with H+, in the Venusian ionosphere, covering altitudes of 120–320 km. Middle: the H production rate profiles for the six most significant chemical channels, as indicated in the figure legend, as well as the total H production rate profile. It is worth noting that among these reactions, the hot H atoms generated by O+ + H2 → OH+ + H and H+ + O → O+ + H do not contribute to atmospheric escape, as their kinetic energies remain below the local escape energy. Bottom: the escape probability profiles for H atoms with four representative nascent energies (0.6, 1, 5, and 10 eV).
Paper: Hydrogen Loss on Venus Driven by Photochemistry
Authors: Hao Gu, Jun Cui, Xiaoshu Wu, Xu Huang, Shiqi Wu, Wenlong Li, Jinjin Zhao, Haoyu Lu, Lei Li
Figure caption: Top: the dayside averaged H escape fluxes as a function of the homopause H2 mixing ratio for solar maximum, median, and minimum conditions, from left to right, all driven by ionospheric chemistry on Venus. Middle: the relative contributions of different channels to the total H escape flux, as a function of the homopause H2 mixing ratio for different solar activity conditions. Bottom: the peak densities of HCO+ and OH+ as a function of the homopause H2 mixing ratio for different solar conditions.
Paper: Impact of Two-population α-particle Distributions on Plasma Stability
Authors: Mihailo M. Martinović, Kristopher G. Klein, Rossana De Marco, Daniel Verscharen, Roberto Bruno, Raffaella D'Amicis
Figure caption: Comparison of the fits of α components for the VDF in parallel sampled by SolO SWA-PAS on 2022 March 2, 16:18:13, using four-component (orange) and five-component (green, purple) models. Parallel cuts at v⊥ = 0 and two-dimensional phase space contour maps are given in the top and bottom panels. The extension of the single α-particle component in the parallel direction is evident. The VDFs are centered with respect to the proton core population (not shown), with parameters for both cases listed in Table 1.
Paper: Hydrogen Loss on Venus Driven by Photochemistry
Authors: Hao Gu, Jun Cui, Xiaoshu Wu, Xu Huang, Shiqi Wu, Wenlong Li, Jinjin Zhao, Haoyu Lu, Lei Li
Figure caption: Top: density ranges of H and H2 derived from self-consistent calculations with different bottom boundary H2 fluxes. Bottom: comparison of modeled density profiles for O﹩{}_{2}^{+}﹩, O+, and CO﹩{}_{2}^{+}﹩, along with the electron density profile, under solar maximum, median, and minimum conditions, from left to right. Solid lines represent the results from our model, while dashed lines show the corresponding profiles from the benchmark model of J. L. Fox & K. Y. Sung (2001).
Paper: Intermingled Open and Closed Magnetic Field Lines near the Radial Origin of the Heliospheric Current Sheet
Authors: F. S. Mozer, A. Voshchepynets, O. V. Agapitov, K.-E. Choi, L. Colomban, R. Sydora
Figure caption: A 1 hr interval is shown during which the radial component of the solar wind magnetic field changed sign (panel (a)), as did the strahl in Figure 2(a), indicating a crossing of the heliospheric current sheet. The electric field spectrum in panel (b) showed two regimes of the observed emissions inside and outside the heliospheric plasma sheet (HPS). Panel (c) gives the plasma density, which changed rapidly from low density outside the HPS to the high-density values inside, and panel (d) gives the angle of magnetic field deflection from the radial direction, which varied synchronously with the changes of the plasma density and electric field spectrum, suggesting a change of the magnetic field geometry. Panel (e) gives electric and magnetic field spectra during the time interval having a broadband electric field and relatively low plasma density, while panel (f) provides spectra obtained in the region of large density and missing broadband electric field. The spectra in the latter region are much more complex, although they contain less power at frequencies below about 1 kHz. The absence of magnetic field waves (the black curves in panels (e) and (f)) indicate that all the observed waves are electrostatic. The black dashed vertical line in both figures gives the electron cyclotron frequency, while the dashed red line gives the proton plasma frequency.
Paper: Intermingled Open and Closed Magnetic Field Lines near the Radial Origin of the Heliospheric Current Sheet
Authors: F. S. Mozer, A. Voshchepynets, O. V. Agapitov, K.-E. Choi, L. Colomban, R. Sydora
Figure caption: Panel (a) gives the 314 eV electron pitch angle distribution during the hour of interest, which shows the counterstreaming flow of the strahl at 12:10–12:20 and 12:42–12:55 (and to a lesser extent near 12:25 and 12:38), indicating that the spacecraft was on closed magnetic field lines during these times. The enhanced fluxes near 90° pitch angles during these times support this interpretation. Panels (b)–(d) display 1 minute velocity distributions broken down to display the core, halo, and two strahl distributions at the times of the three vertical dashed lines in panel (a). They indicate, respectively, strahl in the minus direction, strahl in both directions, and strahl in the plus direction. Panels (e)–(g) provide the proton distributions at these same time intervals.
Paper: Intermingled Open and Closed Magnetic Field Lines near the Radial Origin of the Heliospheric Current Sheet
Authors: F. S. Mozer, A. Voshchepynets, O. V. Agapitov, K.-E. Choi, L. Colomban, R. Sydora
Figure caption: Panel (a) provides an 8 s interval of the magnetic field direction relative to the Parker spiral, showing that the spacecraft passed from a closed field-line-like geometry to an open geometry. Panel (b) shows that the plasma density decreased synchronously with the changing magnetic field direction, while there was a 3.5 s burst of high-rate electric field data shown in panels (c) and (d) (the only time of such a burst during the 1 hr interval of data). The electric field spectrum from zero to 3000 Hz is displayed in panel (e) and the plasma density fluctuations from zero to 3000 Hz are illustrated in panel (f). The variations of the spectra on time scales shorter than 100 ms suggest that the spacecraft crossed the intermingled open and closed magnetic field lines of a complex magnetic field geometry that may have been near the radial origin of the heliospheric current sheet. The similarity of the electric field and density spectra again shows that all the observed waves were electrostatic.
Paper: Intermingled Open and Closed Magnetic Field Lines near the Radial Origin of the Heliospheric Current Sheet
Authors: F. S. Mozer, A. Voshchepynets, O. V. Agapitov, K.-E. Choi, L. Colomban, R. Sydora
Figure caption: The electric field spectra during the 3 hr interval surrounding the reversal of the radial magnetic field. The white curve gives the proton plasma frequency, fpp, while the three black curves display 0.1fpp, 0.2fpp, and 0.3fpp, respectively. The red curve gives the gyrofrequency, fce. The correlation between the harmonic frequencies and the fractional proton plasma frequency is emphasized because this identifies the waves as ion acoustic waves.