adsabs/AstroCLIMB huggingface dataset:
Paper: Accurately Estimating Redshifts from CSST Slitless Spectroscopic Survey Using Deep Learning
Authors: Xingchen Zhou, Yan Gong, Xin Zhang, Nan Li, Xian-Min Meng, Xuelei Chen, Run Wen, Yunkun Han, Hu Zou, Xian Zhong Zheng, Xiaohu Yang, Hong Guo, Pengjie Zhang
Figure caption: Upper: weighted mean uncertainty ﹩\overline{E}﹩ with respect to the true redshift. The value over the whole redshift range is also displayed in a black dashed line. Lower: weighted uncertainty E with respect to SNR in the GI band.
Paper: Accurately Estimating Redshifts from CSST Slitless Spectroscopic Survey Using Deep Learning
Authors: Xingchen Zhou, Yan Gong, Xin Zhang, Nan Li, Xian-Min Meng, Xuelei Chen, Run Wen, Yunkun Han, Hu Zou, Xian Zhong Zheng, Xiaohu Yang, Hong Guo, Pengjie Zhang
Figure caption: Reliability diagram for BNN results before and after the calibration. The black dashed line indicates that the uncertainties are well calibrated with the statistical principle perfectly followed.
Paper: On the Influence of the Solar Wind on the Propagation of Earth-impacting Coronal Mass Ejections
Authors: Sandeep Kumar, Nandita Srivastava, Nat Gopalswamy, Ashutosh Dash
Figure caption: Radial magnetic field (top) and solar wind velocity (bottom) environment of the 2017 May 23 CME (Event 12).
Paper: On the Influence of the Solar Wind on the Propagation of Earth-impacting Coronal Mass Ejections
Authors: Sandeep Kumar, Nandita Srivastava, Nat Gopalswamy, Ashutosh Dash
Figure caption: Magnetic field environment of the events showing the latitudinal deflection inferred from PFSS extrapolation of respective Carrington magnetic field maps. The top panel shows the 2010 May 23 CME (Event 2), and the bottom panel shows the 2012 September 28 (Event 6) CME. The color bar shows the magnetic field in Gauss. θ CR and ϕ CR represent Carrington latitude and longitude, respectively.
Paper: Accurately Estimating Redshifts from CSST Slitless Spectroscopic Survey Using Deep Learning
Authors: Xingchen Zhou, Yan Gong, Xin Zhang, Nan Li, Xian-Min Meng, Xuelei Chen, Run Wen, Yunkun Han, Hu Zou, Xian Zhong Zheng, Xiaohu Yang, Hong Guo, Pengjie Zhang
Figure caption: The accuracy σ NMAD and outlier percentage η with respect to true redshifts are displayed in the upper and lower panels, respectively. The two metrics over the whole redshift range are also shown in black dashed lines.
Paper: On the Influence of the Solar Wind on the Propagation of Earth-impacting Coronal Mass Ejections
Authors: Sandeep Kumar, Nandita Srivastava, Nat Gopalswamy, Ashutosh Dash
Figure caption: The 2011 September 7 CME (Event 3) with velocity ≈850 km s−1 on the left showing a disturbed, noncoherent structure at the heliocentric distance of ≈37 R ⊙ estimated from GCS reconstruction. The 2017 May 23 CME (Event 12) on the right with velocity ≈400 km s−1 showing a coherent circular structure at ≈48 R ⊙ in the HI1 FOV. The top panel shows the CME structure without the GCS mesh, and the bottom panel shows the CME with the GCS mesh overplotted on it (one can clearly notice the differences in the quality of fit between the two cases).
Paper: On the Influence of the Solar Wind on the Propagation of Earth-impacting Coronal Mass Ejections
Authors: Sandeep Kumar, Nandita Srivastava, Nat Gopalswamy, Ashutosh Dash
Figure caption: Fitting of the toroidal model with solar wind parameters in the MC (red line) and observed solar wind parameters from ACE plotted with respect to time (YY/MM/DD), i.e., B, B  x , B  y , and B  z , of IMF and bulk solar wind velocity in km s−1 from top to bottom (black curve).
Paper: Universal Nonthermal Power-law Distribution Functions from the Self-consistent Evolution of Collisionless Electrostatic Plasmas
Authors: Uddipan Banik, Amitava Bhattacharjee, Wrick Sengupta
Figure caption: The quasi-linear diffusion coefficient, D(v), normalized by ﹩{D}_{0}=32{\pi }^{5}{e}^{2}{k}^{2}{{ \mathcal E }}_{0}/{m}^{2}V﹩, as a function of v/σ for a white noise forcing (with a single wavenumber k such that the power spectrum is ﹩{ \mathcal E }(k^{\prime} )={{ \mathcal E }}_{0}\delta \left(k^{\prime} -k\right)﹩) of a collisionless plasma characterized by f 0 that follows a κ distribution with κ = 1 and velocity dispersion, σ. Different lines indicate different values of k λ D, where λ D = σ/ω P is the Debye length. Note that D(v) ∼ v 4 for σ ≲ v ≲ ω P/k = σ/k λ D. This range widens as k λ D decreases, i.e., for larger-scale forcing. For smaller values of k λ D, D(v) spikes at v = ω P/k since these particles are resonant with the plasma waves (electron Langmuir waves or ion acoustic waves) and extract the maximum energy from the electric field.
Paper: Magnetic Diagnostics of Prominence Eruptions through the Hanle Effect of the He I 1083 nm Line
Authors: Momchil E. Molnar, Roberto Casini
Figure caption: Left panel: magnetic flux-rope geometry in the solar frame  S  ≡ (O; x, y, z) and in the local frame  S  † ≡ (A; x †, y †, z †). The origin O of  S  corresponds to the Sun’s center and the z-axis to its rotation axis. The point P is an arbitrary location in the flux-rope domain, lying on the ACO ≡ 〈z †, x †〉 plane. The axis of the flux rope is represented by the open blue circle, tangent to the y †-axis in A. Right panel: example of the magnetic field line of a helical flux rope with RH chirality, for a fixed distance AP from the flux-rope axis (colored in blue).
Paper: Universal Nonthermal Power-law Distribution Functions from the Self-consistent Evolution of Collisionless Electrostatic Plasmas
Authors: Uddipan Banik, Amitava Bhattacharjee, Wrick Sengupta
Figure caption: Same as Figure 1 but for a red noise driver (of the model given by Equation (17)) with different correlation times, τ c, as indicated. Note how D(v) scales the same way as in the white noise case, i.e., ∼v 4 for σ ≲ v ≲ ω P/k, when ω P τ c ≲ 1. For larger correlation times such that ω P τ c ≳ 1 ≳ k σ τ c, the high-velocity end between v ∼ 1/k τ c and ω P/k develops a v 2 scaling, while for σ ≲ v ≲ 1/k τ c D(v) still scales as v 4. The very high-velocity end (v ≳ ω P/k) develops a v −1 scaling.
Paper: Universal Nonthermal Power-law Distribution Functions from the Self-consistent Evolution of Collisionless Electrostatic Plasmas
Authors: Uddipan Banik, Amitava Bhattacharjee, Wrick Sengupta
Figure caption: Quasi-linear evolution of the mean coarse-grained DF, f 0(v), as a function of v, obtained by solving Equation (23) in 3D (see Section 4 for details), starting from an initial Maxwellian. The system is driven by a white noise field of a single wavenumber k = 10−2/λ D. Different colors denote different times in units of ﹩{\sigma }^{2}/{ \mathcal D }﹩ with ﹩{ \mathcal D }={\left(k{\lambda }_{{\rm{D}}}\right)}^{4}{D}_{0}﹩ and ﹩{D}_{0}=32{\pi }^{5}{e}^{2}{k}^{2}{{ \mathcal E }}_{0}/{m}^{2}V﹩. Note how a v −5 power-law tail develops for σ ≲ v ≲ ω P/k = 100σ with σ the velocity dispersion of the initial DF. The high-velocity end (v ≳ ω P/k) forms a plateau. The Maxwellian core (v ≲ σ) heats up over a much longer timescale ﹩\sim {\left(k{\lambda }_{{\rm{D}}}\right)}^{-4}{\sigma }^{2}/2{D}_{0}﹩ than that over which the power-law tail forms.
Paper: Magnetic Diagnostics of Prominence Eruptions through the Hanle Effect of the He I 1083 nm Line
Authors: Momchil E. Molnar, Roberto Casini
Figure caption: He I 1083 wavelength-integrated Stokes U/I (left column) and V/I (right column) produced by a global dipolar magnetic field. The top row corresponds to a dipole field with positive polarity at the north solar pole. The middle row shows the same dipole field with inverted polarity. The magenta arrows in those plots trace the magnetic field lines in the POS for the two models. The bottom row shows the polarization difference between the two models. While in the pure Zeeman case, this difference would be exactly zero, in the case of the Hanle effect, there are subtle differences due to the symmetry breaking of non-isotropic scattering. As expected, the amplitudes of the Hanle-induced Stokes U polarization are significantly larger than those of the Zeeman-dominated Stokes V polarization.
Paper: Universal Nonthermal Power-law Distribution Functions from the Self-consistent Evolution of Collisionless Electrostatic Plasmas
Authors: Uddipan Banik, Amitava Bhattacharjee, Wrick Sengupta
Figure caption: Same as Figure 6 but for a red noise driver of the form given in Equation (17) with a correlation time τ c = 10/ω P. Note that a v −5 power-law tail still forms but for σ ≲ v ≲ 1/k τ c = 10σ, while a shallower ∼v −3 tail forms for 10σ = 1/k τ c ≲ v ≲ ω P/k = 100σ. To compensate for the formation of this harder spectrum, the high-velocity (v ≳ ω P/k) plateau forms slower than in the white noise case.
Paper: Universal Nonthermal Power-law Distribution Functions from the Self-consistent Evolution of Collisionless Electrostatic Plasmas
Authors: Uddipan Banik, Amitava Bhattacharjee, Wrick Sengupta
Figure caption: Same as Figure 1 but for ﹩{ \mathcal E }(k)﹩, a Schechter function, given by Equation (22), with k c λ D = 10−2 and different values of α 0 as indicated. D(v) develops a more pronounced and more extended v 4 scaling (for σ ≲ v ≲ ω P/k * with k * a characteristic wavenumber) as α 0 increases, i.e., larger scales dominate.
Paper: Universal Nonthermal Power-law Distribution Functions from the Self-consistent Evolution of Collisionless Electrostatic Plasmas
Authors: Uddipan Banik, Amitava Bhattacharjee, Wrick Sengupta
Figure caption: Same as Figure 1 but for different values of κ as indicated and k λ D = 10−3. Note that D(v) is largely insensitive to κ and scales as v 4 for σ ≲ v ≲ ω P/k = σ/k λ D = 103 σ regardless of κ.
Paper: Universal Nonthermal Power-law Distribution Functions from the Self-consistent Evolution of Collisionless Electrostatic Plasmas
Authors: Uddipan Banik, Amitava Bhattacharjee, Wrick Sengupta
Figure caption: Same as Figure 1 but for ﹩{ \mathcal E }(k),﹩ a Schechter function, given by Equation (22), with α 0 = 1 and different values of the cutoff wavenumber k c as indicated. D(v) develops a more pronounced v 4 scaling (for σ ≲ v ≲ ω P/k c) as k c λ D decreases, i.e., larger scales dominate.
Paper: Magnetic Diagnostics of Prominence Eruptions through the Hanle Effect of the He I 1083 nm Line
Authors: Momchil E. Molnar, Roberto Casini
Figure caption: Magnetic flux rope perpendicular to the ecliptic plane observed at 60° of heliocentric longitude. The flux rope is anchored to the Sun as in Figure 3 and intersects the ecliptic at X = 0.75 R ⊙, Y = 1.3 R ⊙. Panels (a), (d), (e), and (h) show slices of the magnetic field in the ecliptic plane; the observer is to the right, at 1 au (X = 214 R ⊙); panels (b), (c), (f), and (g) show the Stokes U/I maps for the different magnetic configurations, distinguished by their chirality (RH, LH), and orientation of the axial field (northward, +B  T ; southward, −B  T ). Note that the global pattern of Stokes U is determined by the poloidal component of the field, rather than by the axial component as in the case of the edge-on flux rope. The differences between the pairs resembling Stokes U/I maps are on the order of a few tenths of a percent, as shown in panels (i) and (j). The dashed line outlines the core of the flux rope.
Paper: Magnetic Diagnostics of Prominence Eruptions through the Hanle Effect of the He I 1083 nm Line
Authors: Momchil E. Molnar, Roberto Casini
Figure caption: Model of a helical flux rope laying in the ecliptic plane, and intersecting the YZ plane at X = 0 R ⊙ and Y = 1.5 R ⊙. The flux rope has a radius R = 0.5 R ⊙ and it is anchored to the Sun. Panels (a) and (b) illustrate the observing geometry (in this case, a “quadrature” configuration), where the telescope symbol represents the observer. The spectrally integrated Stokes signals (Q, U, V) are shown in panels (c) through (h) for the longitudinal field of the flux rope pointing either toward (− B ) or away from (+ B ) the observer (see Figure 1). Panels (i) through (k) show the corresponding differences between the two cases. We adopt the same convention for the local reference direction of linear polarization as described in Figure 2.
Paper: Magnetic Diagnostics of Prominence Eruptions through the Hanle Effect of the He I 1083 nm Line
Authors: Momchil E. Molnar, Roberto Casini
Figure caption: Similar magnetic flux-rope setup to the one described in Figure 5, but with the flux rope tilted at 45° to the ecliptic plane. Again, the poloidal magnetic field direction determines the global Stokes U pattern, as shown in panels (a), (b), (c), and (d). The differences between the models, shown in panel (c) for models (a)–(b) and panel (f) for models (d)–(e) illustrate that there are detectable Stokes U differences on the order of 1%. The lime green dotted line follows the core of the flux rope.
Paper: Magnetic Diagnostics of Prominence Eruptions through the Hanle Effect of the He I 1083 nm Line
Authors: Momchil E. Molnar, Roberto Casini
Figure caption: He I 1083 Stokes U/I synthetic observables from a halo CME-like flux rope oriented toward the observer. Panels (a)–(f) follow the notation of Figure 6. Panels (g) and (h) show the orientation of the flux rope with respect to the observer, who is marked as the telescope. The large-scale degeneracy of the opposite chirality and axial-field combinations, previously noted in Figure 5, persists in this case, as shown in panels (a)–(b) and (d)–(e). The green dashed line indicates the POS projection of the flux-rope core.
Paper: Magnetic Diagnostics of Prominence Eruptions through the Hanle Effect of the He I 1083 nm Line
Authors: Momchil E. Molnar, Roberto Casini
Figure caption: Impact of noise on the Stokes U/I synthetic observations of a flux rope on the Sun–Earth line observed from L4/L5. This figure shows the effect of decreasing noise levels for the model in Figure 5 panel (b) in the top row and in the second row for the model in Figure 5 panel (c). The SNR listed in the panel titles. For the instrument proposed in the text, we expect the scenario of SNR ∼ 1000 along the core of the flux rope, corresponding to column (e). The green dashed line shows the core of the flux rope.
Paper: Magnetic Diagnostics of Prominence Eruptions through the Hanle Effect of the He I 1083 nm Line
Authors: Momchil E. Molnar, Roberto Casini
Figure caption: Top row: He I 1083 Stokes U/I maps for the flux-rope model of Figure 5 panel (c), with different central density ρ 0 of the flux rope. The values of ρ 0 in units per cubic centimeter are annotated at the top of the panels. The lime green dashed line shows the core of the flux rope. Bottom row: cross section on the Z = 0 (ecliptic) plane of the number density of scattering atoms in the solar corona for the corresponding models in the top row.
Paper: Magnetic Diagnostics of Prominence Eruptions through the Hanle Effect of the He I 1083 nm Line
Authors: Momchil E. Molnar, Roberto Casini
Figure caption: Changing the magnetic field strength creates different polarization Stokes U signals, but the overall polarization sign remains the same in the unsaturated Hanle regime. We present the same geometrical setting as in Figure 3 with a positive toroidal field component but for varying axial-field strengths. For panels (a)–(e) the field strength is changing from 0.01 of the Hanle saturation strength (for the He I 1083 B crit ≈ 0.7 G) to 1000 times the saturation strength.
Paper: Stellar Pulsation and Evolution: A Combined Theoretical Renewal and Updated Models (SPECTRUM). I. Updating Radiative Opacities for Pulsation Models of Classical Cepheid and RR-Lyrae
Authors: Giulia De Somma, Marcella Marconi, Santi Cassisi, Roberto Molinaro
Figure caption: The trend of the logarithmic opacity (top panels), the derivatives of opacity with respect to temperature (middle panels), and with respect to volume (bottom panels) derived from linear and radiative models of a 4M ⊙ CC with a luminosity of ﹩\mathrm{log}(L/{L}_{\odot })=2.94﹩, Z = 0.02, and Y = 0.28, as obtained using various opacity sets. The dashed lines represent results from the models presented in DS22, while the solid lines represent results from the present computations. The left panels show the results corresponding to a pulsation model near the blue edge of the instability strip (IS) in the H-R diagram, the central panels correspond to a model at the midpoint of the IS temperature range, and the right panels show the behavior near the red edge of the IS (see the labels).
Paper: Stellar Pulsation and Evolution: A Combined Theoretical Renewal and Updated Models (SPECTRUM). I. Updating Radiative Opacities for Pulsation Models of Classical Cepheid and RR-Lyrae
Authors: Giulia De Somma, Marcella Marconi, Santi Cassisi, Roberto Molinaro
Figure caption: Upper panels: the CC F and FO instability strips for Z = 0.004, Y = 0.25 (left panel) and Z = 0.02, Y = 0.28 (right panel). Solid and long-dashed lines represent the results of the present work for F and FO pulsators, respectively, while short-dashed and dotted lines represent the IS results for F and FO pulsators, respectively, from DS20 and DS22. Bottom panels: same as the upper panels but for RRL pulsators with Z = 0.001, Y = 0.245 (left panel) and Z = 0.02, Y = 0.28 (right panel). Solid and long-dashed lines represent the results of the present work for F and FO pulsators, respectively; while short-dashed and dotted lines represent results for F and FO pulsators, respectively, from (M15). Please note that different scales are used in the upper and lower panels due to the substantial difference in the temperature ranges covered by CCs and RR Lyrae stars.
Paper: Stellar Pulsation and Evolution: A Combined Theoretical Renewal and Updated Models (SPECTRUM). I. Updating Radiative Opacities for Pulsation Models of Classical Cepheid and RR-Lyrae
Authors: Giulia De Somma, Marcella Marconi, Santi Cassisi, Roberto Molinaro
Figure caption: Bolometric light curves for FO (upper panels) and F (lower panels) CC pulsators with Z = 0.004 and Y = 0.25, plotted as a function of the pulsation phase. These light curves correspond to selected pulsation models (see the labels for the chosen mass and luminosity level) located close to the blue edge (left column), red edge (right column), and central temperature (central column) of the IS. Dashed lines represent results obtained with the older opacity tables, while solid lines show results with the updated opacity tables. Nonlinear periods (in days) and static effective temperatures (in kelvin) are labeled for each individual model.
Paper: Stellar Pulsation and Evolution: A Combined Theoretical Renewal and Updated Models (SPECTRUM). I. Updating Radiative Opacities for Pulsation Models of Classical Cepheid and RR-Lyrae
Authors: Giulia De Somma, Marcella Marconi, Santi Cassisi, Roberto Molinaro
Figure caption: Theoretical CC F-mode bolometric light curves, as derived by M24 (dashed lines) and in the present work (solid lines), along the HP, for Z = 0.004 (upper panels) and Z = 0.02 (lower panels). The adopted stellar mass (in solar units), effective temperature (in kelvin), and inferred pulsation period (in days) are labeled in each panel.
Paper: Stellar Pulsation and Evolution: A Combined Theoretical Renewal and Updated Models (SPECTRUM). I. Updating Radiative Opacities for Pulsation Models of Classical Cepheid and RR-Lyrae
Authors: Giulia De Somma, Marcella Marconi, Santi Cassisi, Roberto Molinaro
Figure caption: Upper panels: relative variations of the pulsation periods obtained from the present models compared to those from DS22 for CCs with Z = 0.004 and DS20 for CCs with Z = 0.02. The dashed horizontal line represents the equation y = 0. Lower panels: same as the upper panels but for RR Lyrae pulsators; in this case, the comparison is performed with the estimates provided by M15.
Paper: Stellar Pulsation and Evolution: A Combined Theoretical Renewal and Updated Models (SPECTRUM). I. Updating Radiative Opacities for Pulsation Models of Classical Cepheid and RR-Lyrae
Authors: Giulia De Somma, Marcella Marconi, Santi Cassisi, Roberto Molinaro
Figure caption: As in Figure 1, but for CC pulsation models for the chemical composition: Z = 0.004, Y = 0.25.
Paper: Stellar Pulsation and Evolution: A Combined Theoretical Renewal and Updated Models (SPECTRUM). I. Updating Radiative Opacities for Pulsation Models of Classical Cepheid and RR-Lyrae
Authors: Giulia De Somma, Marcella Marconi, Santi Cassisi, Roberto Molinaro
Figure caption: As in Figure 5 but for RRL pulsators with Z = 0.001 and Y = 0.245.
Paper: Stellar Pulsation and Evolution: A Combined Theoretical Renewal and Updated Models (SPECTRUM). I. Updating Radiative Opacities for Pulsation Models of Classical Cepheid and RR-Lyrae
Authors: Giulia De Somma, Marcella Marconi, Santi Cassisi, Roberto Molinaro
Figure caption: As in Figure 1, but for RR Lyrae pulsation models for the chemical composition: Z = 0.001, Y = 0.245.
Paper: Radial Evolution of Non-Maxwellian Electron Populations Derived from Quasi-thermal Noise Spectroscopy: Parker Solar Probe Observations
Authors: Xianming Zheng, Mihailo M. Martinović, Viviane Pierrard, Kristopher G. Klein, Mingzhe Liu, Joel B. Abraham, Yong Liu, Jingting Luo, Xiaodong Lin, Guoqing Liu, Jingchun Li
Figure caption: The variation of the solar wind energy flux w and its constituent components with heliocentric distance. The energy values are represented by distinct dots with the squares representing median values surrounded by their standard deviations The red line represents the fitted profile, which aligns with the model and measurement results proposed in the study by M. Liu et al. (2021), ﹩w=\left(52.1\pm 1.4\right){\left(\tfrac{r}{{R}_{s}}\right)}^{-1.92\pm 0.007}﹩, (a) is the energy flux as an function of the heliocentric distance, and the dots represent the QTN results and the step line represent the SPAN-E and SPAN-I (wave energy flux) data fitting results, (b) is the fractional energy flux for the w  g , w enthalpy, and w kinetic.
Paper: Evolution of Cataclysmic Variables with Binary-driven Mass Loss during Nova Eruptions
Authors: Wen-Shi Tang, Xiang-Dong Li, Zhe Cui
Figure caption: Evolution of CVs with a WD of initial mass M WD,i = 0.6 M ☉ and f dt = 0.5. The left, middle, and right panels show the evolution of the mass transfer rate, the WD mass, and the companion mass as a function of the orbital period, respectively. The initial parameters are labeled in the middle panels. The blue and orange lines represent the evolutionary tracks with and without BDML considered, respectively. The dashed lines in the left panels denote the lower and upper boundaries of the mass transfer rates for stable hydrogen burning and in the right panels the lower (2.15 hr) and upper boundaries (3.18 hr) of the period gap (C. Knigge et al. 2011).
Paper: Radial Evolution of Non-Maxwellian Electron Populations Derived from Quasi-thermal Noise Spectroscopy: Parker Solar Probe Observations
Authors: Xianming Zheng, Mihailo M. Martinović, Viviane Pierrard, Kristopher G. Klein, Mingzhe Liu, Joel B. Abraham, Yong Liu, Jingting Luo, Xiaodong Lin, Guoqing Liu, Jingchun Li
Figure caption: The radial variation of the kappa index in the selected QTN data is shown in gray. The black dots represent the statistical results from each 5 Rs. The blue line shows the results of direct fitting from SPAN-E data, compared to kappa-fitting results from previous studies represented by the red, green, and pink lines. Note that the orange dashed line represents the turbulent dissipation range index as a function of solar radial distance (S. Lotz et al. 2023). During the fitting process, we constrain the kappa index within the range of [2, 15]. Between 30 Rs and 60 Rs, the kappa index experiences an increase, and its trend is essentially consistent with that of the turbulent dissipation range index, indicating a decrease in superthermal electrons within this range. Conversely, beyond 60Rs, the kappa index decreases, signifying an increase in superthermal electrons within that specific range.