adsabs/AstroCLIMB huggingface dataset:
Paper: Material Properties of Saturn’s Interior from Ab Initio Simulations
Authors: Martin Preising, Martin French, Christopher Mankovich, François Soubiran, Ronald Redmer
Figure caption: Mass fraction over radius coordinate. Solid lines represent the MF20 model’s mass fractions, open circles those of our simulations. The colors denote the elements (hydrogen in black, helium in orange, and oxygen in red).
Paper: Material Properties of Saturn’s Interior from Ab Initio Simulations
Authors: Martin Preising, Martin French, Christopher Mankovich, François Soubiran, Ronald Redmer
Figure caption: Thermal expansion coefficient α (solid lines) and isothermal compressibility κ  T  (dashed lines), with results for Saturn in black and Jupiter (French et al. 2012) in orange. The inset displays values of α in the vicinity of the dissociation of hydrogen.
Paper: Material Properties of Saturn’s Interior from Ab Initio Simulations
Authors: Martin Preising, Martin French, Christopher Mankovich, François Soubiran, Ronald Redmer
Figure caption: DOS (upper panel) over energy and radial distribution function of hydrogen g H−H(r) over the interatomic distance r (lower panel) at color-coded radius coordinates.
Paper: Material Properties of Saturn’s Interior from Ab Initio Simulations
Authors: Martin Preising, Martin French, Christopher Mankovich, François Soubiran, Ronald Redmer
Figure caption: Specific heat capacities at constant volume c  V  (dashed lines) and constant pressure c  P  (solid lines) in Saturn (black) and Jupiter (French et al. 2012) (orange).
Paper: Material Properties of Saturn’s Interior from Ab Initio Simulations
Authors: Martin Preising, Martin French, Christopher Mankovich, François Soubiran, Ronald Redmer
Figure caption: Grüneisen parameter γ in Saturn (black) and Jupiter (French et al. 2012) (orange). Blue-dashed lines denote values of an ideal Fermi gas (γ = 2/3) and a classical ideal gas in the vibrational ground state with the H–He concentration predicted by the Saturn model (γ = 0.575). The red-dashed line (γ = 0.487) indicates values for a H–He ideal gas with Jovian composition.
Paper: Material Properties of Saturn’s Interior from Ab Initio Simulations
Authors: Martin Preising, Martin French, Christopher Mankovich, François Soubiran, Ronald Redmer
Figure caption: Dynamic shear viscosity η from DFT–MD for Saturn in black and Jupiter (French et al. 2012) in orange, compared to viscosity data for pure hydrogen from fitting to experimental data in blue (Stiel & Thodos 1963), and interpolated data from DFT–MD results for a similar mixture with a higher content of heavy elements (Soubiran et al. 2017) as light blue diamond.
Paper: Material Properties of Saturn’s Interior from Ab Initio Simulations
Authors: Martin Preising, Martin French, Christopher Mankovich, François Soubiran, Ronald Redmer
Figure caption: Lorenz number L for Saturn (black) and Jupiter (French et al. 2012) (orange) from DFT–MD compared to the Wiedemann–Franz law (gray-dashed line). The inset shows the results for the outer layer.
Paper: Material Properties of Saturn’s Interior from Ab Initio Simulations
Authors: Martin Preising, Martin French, Christopher Mankovich, François Soubiran, Ronald Redmer
Figure caption: Upper panel: results for the thermal conductivity λ in Saturn (black) and Jupiter (French et al. 2012) (orange). Saturn: blue diamonds connected by dashed–dotted lines represent electronic contributions to λ and light blue circles connected by dashed lines represent ionic contributions to λ. Lower panel: thermal diffusivity κ in Saturn and Jupiter.
Paper: Material Properties of Saturn’s Interior from Ab Initio Simulations
Authors: Martin Preising, Martin French, Christopher Mankovich, François Soubiran, Ronald Redmer
Figure caption: DFT–MD results for the DC conductivity σ for Saturn (black) and Jupiter (French et al. 2012) (orange). Data shown in blue and light blue represent the results of earlier studies, obtained from calculations in the chemical picture, by Liu et al. (2008, 2014).
Paper: Material Properties of Saturn’s Interior from Ab Initio Simulations
Authors: Martin Preising, Martin French, Christopher Mankovich, François Soubiran, Ronald Redmer
Figure caption: Sound velocity c s in Saturn (black) and Jupiter (French et al. 2012) (orange).
Paper: Material Properties of Saturn’s Interior from Ab Initio Simulations
Authors: Martin Preising, Martin French, Christopher Mankovich, François Soubiran, Ronald Redmer
Figure caption: Kinematic shear viscosity ν from DFT–MD for Saturn in black and Jupiter (French et al. 2012) in orange.
Paper: Application of the Tianwen-1 DOR Signals Observed by Very Long Baseline Interferometry Radio Telescopes in the Study of Solar Wind Plasma and a Coronal Mass Ejection
Authors: Zhichao Wang, Maoli Ma, Qinghui Liu, Qingbao He, Xin Zheng, Lijia Liu, Guifré Molera Calvés
Figure caption: The projected radial and tangential distance of the baselines between the station pairs onto the ecliptic plane in heliographic coordinates are marked at SH 05:12:22. The CME first occurred in the SOHO/LASCO C2 images at 21:36 on 2021 November 1, and was observed by VLBI radio telescopes at 30.6 Rs at 03:02 on November 2.
Paper: Application of the Tianwen-1 DOR Signals Observed by Very Long Baseline Interferometry Radio Telescopes in the Study of Solar Wind Plasma and a Coronal Mass Ejection
Authors: Zhichao Wang, Maoli Ma, Qinghui Liu, Qingbao He, Xin Zheng, Lijia Liu, Guifré Molera Calvés
Figure caption: (a) Frequency and (c) phase spikes at SH 03:02:35. (b) Frequency and (d) phase spikes at SH 05:12:22.
Paper: Erratum: “The Statistical Properties of Solar Wind Temperature Parameters Near 1 au” (2018, ApJS, 236, 41)
Authors: Lynn B. Wilson, Michael L. Stevens, Justin C. Kasper, Kristopher G. Klein, Bennett A. Maruca, Stuart D. Bale, Trevor A. Bowen, Marc P. Pulupa, Chadi S. Salem
Figure caption: Temperature ratios [unitless] for different particle species in each column and for the different constraints (i.e., rows) listed in Table 2. In each panel, there are three color-coded histograms for the different components defined as follows: total (magenta), parallel (blue), and perpendicular (green). The color-coded vertical lines are the median values (values found in Table 2) of the distributions for the corresponding color-coded histograms.
Paper: Erratum: “The Statistical Properties of Solar Wind Temperature Parameters Near 1 au” (2018, ApJS, 236, 41)
Authors: Lynn B. Wilson, Michael L. Stevens, Justin C. Kasper, Kristopher G. Klein, Bennett A. Maruca, Stuart D. Bale, Trevor A. Bowen, Marc P. Pulupa, Chadi S. Salem
Figure caption: Plasma betas [unitless] for different particle species in each column and for the different constraints (i.e., rows) listed in Table 3. In each panel, there are three color-coded histograms for the different components defined as follows: total (magenta), parallel (blue), and perpendicular (green). The color-coded vertical lines are the median values (values found in Table 3) of the distributions for the corresponding color-coded histograms.
Paper: Erratum: “The Statistical Properties of Solar Wind Temperature Parameters Near 1 au” (2018, ApJS, 236, 41)
Authors: Lynn B. Wilson, Michael L. Stevens, Justin C. Kasper, Kristopher G. Klein, Bennett A. Maruca, Stuart D. Bale, Trevor A. Bowen, Marc P. Pulupa, Chadi S. Salem
Figure caption: Temperatures [eV] for different particle species in each column and for the different constraints (i.e., rows) listed in Table 1. In each panel, there are three color-coded histograms for the different components defined as follows: total (magenta), parallel (blue), and perpendicular (green). The color-coded vertical lines are the median values (values found in Table 1) of the distributions for the corresponding color-coded histograms.
Paper: Erratum: “The Statistical Properties of Solar Wind Temperature Parameters Near 1 au” (2018, ApJS, 236, 41)
Authors: Lynn B. Wilson, Michael L. Stevens, Justin C. Kasper, Kristopher G. Klein, Bennett A. Maruca, Stuart D. Bale, Trevor A. Bowen, Marc P. Pulupa, Chadi S. Salem
Figure caption: Temperature ratios for different particle species in each column and for the different constraints (i.e., rows) listed in Table 4. In each panel, there are three color-coded histograms for the different components defined as follows: total (magenta), parallel (blue), and perpendicular (green). The color-coded vertical lines are the median values (values found in Table 4) of the distributions for the corresponding color-coded histograms.
Paper: Application of the Tianwen-1 DOR Signals Observed by Very Long Baseline Interferometry Radio Telescopes in the Study of Solar Wind Plasma and a Coronal Mass Ejection
Authors: Zhichao Wang, Maoli Ma, Qinghui Liu, Qingbao He, Xin Zheng, Lijia Liu, Guifré Molera Calvés
Figure caption: Projection of VLBI baselines in the heliocentric coordinate system. (a) Radial projection, (b) tangential projection.
Paper: Application of the Tianwen-1 DOR Signals Observed by Very Long Baseline Interferometry Radio Telescopes in the Study of Solar Wind Plasma and a Coronal Mass Ejection
Authors: Zhichao Wang, Maoli Ma, Qinghui Liu, Qingbao He, Xin Zheng, Lijia Liu, Guifré Molera Calvés
Figure caption: Differential phase delays and their corresponding TEC changes (right axis) on 2021 October 23.
Paper: Material Properties of Saturn’s Interior from Ab Initio Simulations
Authors: Martin Preising, Martin French, Christopher Mankovich, François Soubiran, Ronald Redmer
Figure caption: Self-diffusion coefficients D from DFT–MD for Saturn (solid lines) and Jupiter (French et al. 2012) (orange-dashed lines). Upper panel: D of hydrogen (black), helium (orange), and oxygen (red). The two lower panels show D H and D He, respectively. Blue diamonds denote interpolated data from DFT–MD results for a similar mixture with a higher content of heavy elements (Soubiran et al. 2017).
Paper: Material Properties of Saturn’s Interior from Ab Initio Simulations
Authors: Martin Preising, Martin French, Christopher Mankovich, François Soubiran, Ronald Redmer
Figure caption: Temperature T over pressure P of the MF20 Saturn model (alternating red and yellow lines), our simulations (black circles), calculations of the DC conductivity by Knudson et al. (2018) performed with DFT–MD and the vdW-DF1 functional (orange circles), dissociation of hydrogen from DFT–MD simulations with the vdW-DF1 functional by Knudson et al. (2015) (orange line) and from quantum Monte Carlo (QMC) calculations by Mazzola et al. (2018) (blue line). Different colors and line styles of the MF20 model denote (from lowest to highest pressures): layer with molecular, dissociating, and fully dissociated H2, He-rich layer, and isothermal core, respectively.
Paper: Erratum: “The Statistical Properties of Solar Wind Temperature Parameters Near 1 au” (2018, ApJS, 236, 41)
Authors: Lynn B. Wilson, Michael L. Stevens, Justin C. Kasper, Kristopher G. Klein, Bennett A. Maruca, Stuart D. Bale, Trevor A. Bowen, Marc P. Pulupa, Chadi S. Salem
Figure caption: Plasma betas for different particle species in each column and for the different constraints (i.e., rows) listed in Table 6. In each panel, there are three color-coded histograms for the different components defined as follows: total (magenta), parallel (blue), and perpendicular (green). The color-coded vertical lines are the median values (values found in Table 6) of the distributions for the corresponding color-coded histograms.
Paper: Erratum: “The Statistical Properties of Solar Wind Temperature Parameters Near 1 au” (2018, ApJS, 236, 41)
Authors: Lynn B. Wilson, Michael L. Stevens, Justin C. Kasper, Kristopher G. Klein, Bennett A. Maruca, Stuart D. Bale, Trevor A. Bowen, Marc P. Pulupa, Chadi S. Salem
Figure caption: Temperature ratios for different particle species in each column and for the different constraints (i.e., rows) listed in Table 5. In each panel, there are three color-coded histograms for the different components defined as follows: total (magenta), parallel (blue), and perpendicular (green). The color-coded vertical lines are the median values (values found in Table 5) of the distributions for the corresponding color-coded histograms.
Paper: Application of the Tianwen-1 DOR Signals Observed by Very Long Baseline Interferometry Radio Telescopes in the Study of Solar Wind Plasma and a Coronal Mass Ejection
Authors: Zhichao Wang, Maoli Ma, Qinghui Liu, Qingbao He, Xin Zheng, Lijia Liu, Guifré Molera Calvés
Figure caption: STDs of fluctuations of TW1 signals at different heliocentric distances (ingress: 129.4 Rs (2021 June 18) − 33.5 Rs (2021 September 11); egress: 13.5 Rs (2021 October 19) − 102.1 Rs (2022 January 4)). (a) ΔDOR group delay, (b) delay rate, (c) frequency, (d) phase.
Paper: Application of the Tianwen-1 DOR Signals Observed by Very Long Baseline Interferometry Radio Telescopes in the Study of Solar Wind Plasma and a Coronal Mass Ejection
Authors: Zhichao Wang, Maoli Ma, Qinghui Liu, Qingbao He, Xin Zheng, Lijia Liu, Guifré Molera Calvés
Figure caption: The fluctuations of the (a) frequency, (b) phase, and (c) TEC variations. The STDs of the fluctuations of the (d) frequency, (e) phase, and (f) TEC variations on 2021 November 2.
Paper: Application of the Tianwen-1 DOR Signals Observed by Very Long Baseline Interferometry Radio Telescopes in the Study of Solar Wind Plasma and a Coronal Mass Ejection
Authors: Zhichao Wang, Maoli Ma, Qinghui Liu, Qingbao He, Xin Zheng, Lijia Liu, Guifré Molera Calvés
Figure caption: STDs of TEC variations at different heliocentric distances (ingress: 129.4 Rs (2021 June 18) − 33.5 Rs (2021 September 11); egress: 13.5 Rs (2021 October 19) − 102.1 Rs (2022 January 4)).
Paper: Application of the Tianwen-1 DOR Signals Observed by Very Long Baseline Interferometry Radio Telescopes in the Study of Solar Wind Plasma and a Coronal Mass Ejection
Authors: Zhichao Wang, Maoli Ma, Qinghui Liu, Qingbao He, Xin Zheng, Lijia Liu, Guifré Molera Calvés
Figure caption: SOHO/LASCO C3 image. (a) 2021 October 26, 07:54. Mars’s position is marked by a black arrow. (b) 2021 November 2, 02:42. The black arrow marks a CME. (c) 2021 November 2. The diagram of Mars’s position in the LASCO C3 field of view. The red dot is the position of Mars.
Paper: Application of the Tianwen-1 DOR Signals Observed by Very Long Baseline Interferometry Radio Telescopes in the Study of Solar Wind Plasma and a Coronal Mass Ejection
Authors: Zhichao Wang, Maoli Ma, Qinghui Liu, Qingbao He, Xin Zheng, Lijia Liu, Guifré Molera Calvés
Figure caption: Power density spectra of Tianwen-1 (TW1) at BJ station at 02:15 on 2021 November 12. Fc is the carrier frequency at 8431 MHz. (a) −DOR2 = Fc − 19.2 MHz, (b) −DOR1 = Fc − 3.8 MHz, (c) Fc = 8431 MHz, (d) +DOR1 = Fc + 3.8 MHz, (e) +DOR2 = Fc + 19.2 MHz.
Paper: Application of the Tianwen-1 DOR Signals Observed by Very Long Baseline Interferometry Radio Telescopes in the Study of Solar Wind Plasma and a Coronal Mass Ejection
Authors: Zhichao Wang, Maoli Ma, Qinghui Liu, Qingbao He, Xin Zheng, Lijia Liu, Guifré Molera Calvés
Figure caption: Connected DPDs and their corresponding TEC changes (right axes). (a) 2021 October 26, (b) 2021 November 2, (c) 2021 November 9.
Paper: Application of the Tianwen-1 DOR Signals Observed by Very Long Baseline Interferometry Radio Telescopes in the Study of Solar Wind Plasma and a Coronal Mass Ejection
Authors: Zhichao Wang, Maoli Ma, Qinghui Liu, Qingbao He, Xin Zheng, Lijia Liu, Guifré Molera Calvés
Figure caption: Flow chart of the data processing.
Paper: The Statistical Uncertainties on X-Ray Flux and Spectral Parameters from Chandra ACIS-I Observations of Faint Sources: Application to the Cygnus OB2 Association
Authors: J. F. Albacete-Colombo, E. Flaccomio, J. J. Drake, N. J. Wright, M. Guarcello, V. Kashyap
Figure caption: Top: the ratios of individual fit errors from noninteractive spectral fitting to the Q uncertainty computed from MC simulations (i.e., Fit_err/Q), for each of the sources that were included in the comparison analysis (see Section 5.1). Error ratios were computed for the three main parameters, NH, kT, and unabsorbed flux. Gray crosses are the individual source Fit_err/Q ratios for combined positive and negative uncertainties, with errors representing 1σ uncertainties. Small green and blue circles correspond to the forward-moving averages (see text for description) as a function of the increasing background fraction for positive and negative 1σ quantiles, respectively. Small red circles were computed in the same way but assuming both positive and negative quantile distributions as a single one. Bottom: simply histograms taken on the y-axis (mean Fit_err/Q) of the corresponding set of colored points in the top panels.
Paper: The Statistical Uncertainties on X-Ray Flux and Spectral Parameters from Chandra ACIS-I Observations of Faint Sources: Application to the Cygnus OB2 Association
Authors: J. F. Albacete-Colombo, E. Flaccomio, J. J. Drake, N. J. Wright, M. Guarcello, V. Kashyap
Figure caption: Left: N H–kT space of solutions from ∼ 500,000 MC simulations for different models, net counts, and background fractions. The different colors refer to the simulated thermal spectra at the 14 different N H–kT input values (large colored circles). Small colored circles are those that correspond to MC simulations for 20 and 30 net counts in the spectra. Light-gray and darker-gray circles show the MC simulations for net counts of 100 and 300 photons in the spectra, respectively. The clustering of points giving rise to a small degree of horizontal striping along the direction of the kT axis corresponds to slightly biased spectral fit solutions that mostly occur for MC simulations with 20 and 30 net counts (see text). Right: a similar illustration of a total of ∼192,000 nonthermal MC simulations for different N H–Γ models and background fractions.
Paper: The Statistical Uncertainties on X-Ray Flux and Spectral Parameters from Chandra ACIS-I Observations of Faint Sources: Application to the Cygnus OB2 Association
Authors: J. F. Albacete-Colombo, E. Flaccomio, J. J. Drake, N. J. Wright, M. Guarcello, V. Kashyap
Figure caption: Flux Q uncertainty as a function of N H and kT. The top left panel shows a set of eight different kT curves interpolated using a cubic spline function for MC-simulated spectra in the range of 35–40 photons. The Q flux uncertainty is shown in the left column as 2D bidimensional maps, which was computed from the kT (y-axis) curves followed by a linear interpolation along the orthogonal (N H) direction (x-axis). The top right panel shows the median Q flux uncertainties (boxes) for the six different N H curves also interpolated by a cubic spline function and for the same range of photon counts. The rest of the panels in the right column show the Q flux uncertainty as a bidimensional map computed in an inverse interpolation order, i.e., along the kT direction. Note that for the 2D maps both columns are essentially the same, with only very small differences, which suggests that no interpolation artifacts were created in our numerical treatment of Q uncertainties.
Paper: The Statistical Uncertainties on X-Ray Flux and Spectral Parameters from Chandra ACIS-I Observations of Faint Sources: Application to the Cygnus OB2 Association
Authors: J. F. Albacete-Colombo, E. Flaccomio, J. J. Drake, N. J. Wright, M. Guarcello, V. Kashyap
Figure caption: The relative errors in N H, kT, and flux as a function of the input net counts imposed on the spectral simulations. The top panels correspond to a spectral model grid point log(N H) = 22.0 and kT = 3.0 keV, and the bottom panels correspond to a model with log(N H) = 21.0 and kT = 1.2 keV. The red and blue boxes refer to the Q uncertainty computed for the relative error distributions (gray circles) for each incremental range in photon counts in which we simulate the spectra. The numbers next to these points indicate the number of simulations included in each respective bin. We point out that relative errors for N H in the bottom middle panel artificially bottom out at an N H value a factor of 100 lower than the input value for cases of less than about 100 net source counts. This numerical conditioning is imposed in order to avoid unconstrained lower limit values of N H for low column density cases (see also Section 3).
Paper: The Statistical Uncertainties on X-Ray Flux and Spectral Parameters from Chandra ACIS-I Observations of Faint Sources: Application to the Cygnus OB2 Association
Authors: J. F. Albacete-Colombo, E. Flaccomio, J. J. Drake, N. J. Wright, M. Guarcello, V. Kashyap
Figure caption: The left panel illustrates curves fitted to the relative flux error as a function of the background fraction for the thermal model 1 (N H = 1.0 × 1022, kT = 3.0) according to MC simulations containing 20 (red), 30 (orange), 100 (blue), and 300 (black) net photons in the spectra, respectively (see text). Large colored circles in the panel are the quantile uncertainties for flux. The relationship between the flux uncertainty and background fraction is clearly quite linear. The right panel illustrates the synthesis of the fits to the data of the left panel. The whole set of interpolated curves for the rest of the model parameters investigated and for each of 14 models was computed but not shown here. The same numerical treatment was performed for nonthermal models and for all spectral parameters.
Paper: The Statistical Uncertainties on X-Ray Flux and Spectral Parameters from Chandra ACIS-I Observations of Faint Sources: Application to the Cygnus OB2 Association
Authors: J. F. Albacete-Colombo, E. Flaccomio, J. J. Drake, N. J. Wright, M. Guarcello, V. Kashyap
Figure caption: The relative 1σ quantile flux errors, ∣Q flux∣ (see text for the formal definition), as a function of either the minimum number of counts per bin (red points, upper x-axis) or the minimum S/N per bin (black points, lower x-axis) in X-ray spectral fitting simulations. The errors were computed from a set of 1000 simulations for each binning strategy. The minimum relative error occurs whenever simulated X-ray spectra are fitted with an S/N/bin > 1. The same result is derived from the analysis of relative errors of other spectral model parameters.
Paper: The Statistical Uncertainties on X-Ray Flux and Spectral Parameters from Chandra ACIS-I Observations of Faint Sources: Application to the Cygnus OB2 Association
Authors: J. F. Albacete-Colombo, E. Flaccomio, J. J. Drake, N. J. Wright, M. Guarcello, V. Kashyap
Figure caption: The kT–N H plane for parameter values obtained from X-ray spectral fits to Cyg OB2 in sources having a signal strength in the range of 20–350 net photons. The nine colored models are those used to compute the influence of the different background fractions in the determination of uncertainty for a range of spectral parameters.
Paper: Classification of Chandra X-Ray Sources in Cygnus OB2
Authors: Vinay L. Kashyap, Mario G. Guarcello, Nicholas J. Wright, Jeremy J. Drake, Ettore Flaccomio, Tom L. Aldcroft, Juan F. Albacete Colombo, Kevin Briggs, Francesco Damiani, Janet E. Drew, Eduardo L. Martin, Giusi Micela, Tim Naylor, Salvatore Sciortino
Figure caption:  r − i vs. i − z diagrams of all the sources with good OSIRIS or SDSS photometry. The solid line is the 2.5 Myr isochrone from Siess et al. (2000) after applying the F96 transformation between the UBVRI and the u  I  g  I  r  I  i  I  z  I  photometric systems, and the dashed line is from the MIST database. The extinction vector is obtained from O’Donnell (1994). The corresponding masses are indicated with a horizontal displacement from the isochrone. The classifications are according to the automated NBC method (left) and after manual reclassification (right) and show foreground objects (red diamonds), members (green circles), and background objects (blue crosses).