adsabs/AstroCLIMB huggingface dataset:
Paper: Stellar Neutrino Emission across the Mass–Metallicity Plane
Authors: Ebraheem Farag, F. X. Timmes, Morgan T. Chidester, Samalka Anandagoda, Dieter H. Hartmann
Figure caption: Neutrino targets for the nitrogen flash in 1 M ⊙ models for all six metallicities. The x-axis is the time since the first, and strongest, nitrogen flash. The y-axis is a luminosity relative to L ⊙ = 3.828 × 1033 erg s−1 (Prša et al. 2016). Colored curves show the ν, γ, and He-burning luminosity. The red circle marks the maximum L  ν , and the red label gives the value of ﹩{L}_{\nu ,\max }﹩ and the average neutrino energy. Labeled are the maximum flux at a distance d in parsecs, and the duration for the L  ν  to be larger than 1/2 and 1/3 ﹩{L}_{\nu ,\max }﹩. Metal-rich models have larger ﹩{L}_{\nu ,\max }﹩ and longer periods between flashes.
Paper: Stellar Neutrino Emission across the Mass–Metallicity Plane
Authors: Ebraheem Farag, F. X. Timmes, Morgan T. Chidester, Samalka Anandagoda, Dieter H. Hartmann
Figure caption: Components of L  ν  from nuclear reactions over the lifetime of an M ZAMS = 1 M ⊙ model for all six metallicities. The x-axis is the sequential model number, a proxy for time, beginning at core H depletion (left) and ending as a cool WD (right). Curves are smoothed with a 50 model moving-average filter. Evolutionary phases are shown by the colored regions and labeled. Reactions emitting neutrinos in the pp-chain and CNO cycles are listed in Section 3.1.
Paper: Stellar Neutrino Emission across the Mass–Metallicity Plane
Authors: Ebraheem Farag, F. X. Timmes, Morgan T. Chidester, Samalka Anandagoda, Dieter H. Hartmann
Figure caption: Tracks in a γHRD (left panels) and a νHRD (right panels) for Z = 1 Z ⊙ over M ZAMS = 8–150 M ⊙. Tracks are colored by evolutionary phase and labeled. Black circles mark convective core C burning, and red circles mark radiative core C burning. Luminosities are normalized to L ⊙ = 3.828 × 1033 erg s−1 (Prša et al. 2016).
Paper: Stellar Neutrino Emission across the Mass–Metallicity Plane
Authors: Ebraheem Farag, F. X. Timmes, Morgan T. Chidester, Samalka Anandagoda, Dieter H. Hartmann
Figure caption: Average electron neutrino energy for beta decays (top), and average electron antineutrino energy for inverse-beta decays (bottom) for the 1 Z ⊙ models across a range of M ZAMS. Curves are smoothed with a 50 time step moving-average filter. The average pair-neutrino energy is shown by the black curve, with the gray band giving the lower 10% and upper 90% of pair-neutrino energies. Phases of evolution are shown by the colored panels and labeled. The horizontal dashed line shows a representative ≃1.8 MeV detection threshold to inverse-beta decay of current neutrino detectors (e.g., Simpson et al. 2019; Harada et al. 2023). The average electron neutrino and antineutrino energies are approximately independent of M ZAMS.
Paper: Stellar Neutrino Emission across the Mass–Metallicity Plane
Authors: Ebraheem Farag, F. X. Timmes, Morgan T. Chidester, Samalka Anandagoda, Dieter H. Hartmann
Figure caption: Components of L  ν  for each phase of evolution of an M ZAMS = 20 M ⊙, 1 Z ⊙ model. The x-axis is the time to the onset of CC. Curves show the contributions from nuclear and thermal neutrinos, and are smoothed with a 50 time step moving-average filter. Phases of evolution are shown by the colored regions and labeled above the plot. Boundaries between phases are defined by the ignition of the next fuel source, when the central mass fraction of the next fuel source decreases by 10−3.
Paper: Stellar Neutrino Emission across the Mass–Metallicity Plane
Authors: Ebraheem Farag, F. X. Timmes, Morgan T. Chidester, Samalka Anandagoda, Dieter H. Hartmann
Figure caption: Fraction of E  ν  emitted at different phases of evolution for all six metallicities (colored circles). From top to bottom, the panels show ﹩{[E/{E}_{\mathrm{tot}}]}_{\nu }﹩ for core H burning, shell H burning, core He burning prior to any TP-AGB phase, He burning through the TP-AGB phase, and during the WD cooling phase.
Paper: Stellar Neutrino Emission across the Mass–Metallicity Plane
Authors: Ebraheem Farag, F. X. Timmes, Morgan T. Chidester, Samalka Anandagoda, Dieter H. Hartmann
Figure caption: Same format as Figure 10 but for the TP-AGB phase of evolution.
Paper: Stellar Neutrino Emission across the Mass–Metallicity Plane
Authors: Ebraheem Farag, F. X. Timmes, Morgan T. Chidester, Samalka Anandagoda, Dieter H. Hartmann
Figure caption: Same as Figure 8 but for 3 M ⊙ models.
Paper: Stellar Neutrino Emission across the Mass–Metallicity Plane
Authors: Ebraheem Farag, F. X. Timmes, Morgan T. Chidester, Samalka Anandagoda, Dieter H. Hartmann
Figure caption: Same format as Figure 11 but for 3 M ⊙ models across all six metallicities.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-104 (Kepler-94). Left: the best-fit model includes a nontransiting planet, Kepler-94 c (orbital parameters inset in phase-folded panel). Right: the periodogram of the RVs after removing the signals from the transiting planet (top) and both planets (bottom).
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-116 (Kepler-106). The best-fit model includes a nontransiting planet, although the period of that planet is uncertain owing to aliasing (right).
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-142. Left: RVs are from HIRES (black circles) and SOPHIE (yellow circles). The best-fit model has two nontransiting giant planets (details inset in RV panels, left).
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-148 (Kepler-48). The longest-period companion presented here was not detected by the KGPS algorithm but was identified in the residuals by eye.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-108 (Kepler-103). No nontransiting companions are detected.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-103 (Kepler-1710). No nontransiting companions are detected.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-123 (Kepler-109). No nontransiting companions are detected.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-122 (Kepler-95). No nontransiting companions are detected.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-137 (Kepler-18). No nontransiting companions are detected.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-246. Left: the best-fit model includes two nontransiting planets, Kepler-68 d at 633 days and Kepler-68 e at 5000 days (see insets in phase-folded panels). Right: the top panel is a periodogram of the HIRES RVs after removing the transiting planets only, the middle panel is the periodogram after removing one nontransiting planet at 636 days (note the strong yearly alias at 362 days), and the bottom panel is after removing nontransiting planets at 634 and 5000 days.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-245 (Kepler-37). Left: the RVs were taken at Keck-HIRES (black circles) and TNG-HARPS-N (maroon triangles). The best-fit model includes a Keplerian signal at either 460 days (pictured left) or 2000 days. Right: the periodogram of the Kepler-37 RVs after removing the signals associated with the transiting planets yields multiple peaks that are challenging to distinguish from stellar activity.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-153 (Kepler-113). No nontransiting companions are detected.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-265 (Kepler-507). Left: the best-fit model includes a nontransiting planet, Kepler-507 c (orbital parameters inset in phase-folded panel). Right: periodograms of the RVs after subtracting the models from the transiting planets only (top) and the best-fit model that includes the nontransiting planet (bottom).
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-157 (Kepler-11). No nontransiting companions are detected.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-244 (Kepler-25). The best-fit model includes a nontransiting planet, Kepler-25 d (orbital parameters inset in phase-folded panel).
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-262 (Kepler-50). No nontransiting companions are detected.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-260 (Kepler-126). No nontransiting companions are detected.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-261 (Kepler-96). No nontransiting companions are detected.
Paper: The MeerKAT Absorption Line Survey (MALS) Data Release. I. Stokes I Image Catalogs at 1–1.4 GHz
Authors: P. P. Deka, N. Gupta, P. Jagannathan, S. Sekhar, E. Momjian, S. Bhatnagar, J. Wagenveld, H.-R. Klöckner, J. Jose, S. A. Balashev, F. Combes, M. Hilton, D. Borgaonkar, A. Chatterjee, K. L. Emig, A. N. Gaunekar, G. I. G. Józsa, D. Y. Klutse, K. Knowles, J.-K. Krogager, A. Mohapatra, K. Moodley, Sébastien Muller, P. Noterdaeme, P. Petitjean, P. Salas, S. Sikhosana
Figure caption: Spectral indices of 122,077 sources detected in both the SPWs vs. the distance from the pointing center. The red (black) points mark the median spectral indices derived from katbeam (plumber) corrected flux densities in bins of 5′. The horizontal dotted lines indicate median spectral indices for the full sample corrected using katbeam (﹩-{0.732}_{-0.003}^{+0.003}﹩) and plumber (﹩-{0.680}_{-0.003}^{+0.003}﹩) beam models. The points are color coded according to their space density. The error bars defining the 90% confidence level estimated by bootstrapping are enlarged by a factor of 10 for clarity.
Paper: The MeerKAT Absorption Line Survey (MALS) Data Release. I. Stokes I Image Catalogs at 1–1.4 GHz
Authors: P. P. Deka, N. Gupta, P. Jagannathan, S. Sekhar, E. Momjian, S. Bhatnagar, J. Wagenveld, H.-R. Klöckner, J. Jose, S. A. Balashev, F. Combes, M. Hilton, D. Borgaonkar, A. Chatterjee, K. L. Emig, A. N. Gaunekar, G. I. G. Józsa, D. Y. Klutse, K. Knowles, J.-K. Krogager, A. Mohapatra, K. Moodley, Sébastien Muller, P. Noterdaeme, P. Petitjean, P. Salas, S. Sikhosana
Figure caption: Spectral indices (﹩{\alpha }_{{spw}9}^{{spw}2}﹩) as a function of flux density in SPW2 (left panels) and SPW9 (right panels). In the top row, the points are color coded according to their space density. The second row shows the fraction of upper (left) and lower (right) limits on spectral indices in each flux density bin. The third row shows the median S/N of sources in each bin. Note that the sources with S/N < 15 were excluded from the analysis. The median spectral indices calculated using survival analysis methods in bins of 0.2 dex in flux density are shown for both katbeam and plumber beam-corrected flux densities (bottom panels). The median spectral indices considering only compact sources for the case of katbeam model are also shown. For reference, 1.4 GHz measurements from Prandoni et al. (2006) (P06) are plotted in the bottom-right panel.
Paper: The MeerKAT Absorption Line Survey (MALS) Data Release. I. Stokes I Image Catalogs at 1–1.4 GHz
Authors: P. P. Deka, N. Gupta, P. Jagannathan, S. Sekhar, E. Momjian, S. Bhatnagar, J. Wagenveld, H.-R. Klöckner, J. Jose, S. A. Balashev, F. Combes, M. Hilton, D. Borgaonkar, A. Chatterjee, K. L. Emig, A. N. Gaunekar, G. I. G. Józsa, D. Y. Klutse, K. Knowles, J.-K. Krogager, A. Mohapatra, K. Moodley, Sébastien Muller, P. Noterdaeme, P. Petitjean, P. Salas, S. Sikhosana
Figure caption: Spectral index (﹩{\alpha }_{{spw}9}^{{spw}2}﹩) distribution of sources detected at S/N > 8 (median ﹩\alpha \,=\,-{0.736}_{-0.003}^{+0.003}﹩) and at S/N > 15 (median ﹩\alpha \,=\,-{0.757}_{-0.003}^{+0.003}﹩). The vertical lines mark the median spectral indices.
Paper: Simulating the Photospheric to Coronal Plasma Using Magnetohydrodynamic Characteristics. I. Data-driven Boundary Conditions
Authors: Lucas A. Tarr, N. Dylan Kee, Mark G. Linton, Peter W. Schuck, James E. Leake
Figure caption: Weighted mean-squared-difference (wMSD) as a function of time using different driving cadences, with Δt = 1, 5, 20, 50, and 100δt for the blue, green, brown, violet, and yellow lines, respectively. (a) wMSD calculated in the driving boundary layer, i.e., cell k = 100 (k = 0) in the GT (Data-Driven) simulation. (b) Zoom-in near the middle of the simulation. (c) Same as (a) but 15 cells higher into the simulation (i.e., in the plane shown in Figure 7). (d) Zoom-in shortly after the spheromak edge reaches the k = 15 layer in the Data-Driven simulation.
Paper: Simulating the Photospheric to Coronal Plasma Using Magnetohydrodynamic Characteristics. I. Data-driven Boundary Conditions
Authors: Lucas A. Tarr, N. Dylan Kee, Mark G. Linton, Peter W. Schuck, James E. Leake
Figure caption: Comparison of wMSD for our data-driving algorithm vs. linear baseline interpolation algorithms. For each line type, the red (blue) line shows driving at Δt = 20 (50)δt. The solid curves reproduce the SVD-based CHAR-DDBC results from Figure 8, for reference; the dashed curves show the difference metric for SVD CHAR-DDBC when no information is known about either the density ρ or internal energy density ϵ, and the dotted curves show the metric when  B  and  v  are linearly interpolated while ρ and ϵ are held fixed to their initial values. Panel (a) gives wMSD calculated in the driving boundary layer, i.e., the k = 100 (k = 0) cell in the GT (Data-Driven) simulation. (b) Same as (a) but 15 cells higher into the simulation, i.e., the layer from Figure 7.
Paper: Simulating the Photospheric to Coronal Plasma Using Magnetohydrodynamic Characteristics. I. Data-driven Boundary Conditions
Authors: Lucas A. Tarr, N. Dylan Kee, Mark G. Linton, Peter W. Schuck, James E. Leake
Figure caption: Comparison of all primitive variables in the interior of the Data-Driven simulation at a horizontal slice at k = 15 cells above the driven boundary (z ≈ 1.59), between the GT simulation (columns 1, 5) and simulations driven every 20 δt (columns 2, 6), 50 δt (columns 3, 7), and 100 δt (columns 4, 8). The horizontal axis is x, the vertical axis is y, and data corresponds to Courant step 320, or t = 1.18. The color scale for each primitive variable is common for all simulations. The top row compares the density in the left four columns and internal energy density in the right four columns. The next three rows compare components of the velocity field (left) in a red–blue color map and magnetic field (right) in a gray-scale color map.
Paper: Simulating the Photospheric to Coronal Plasma Using Magnetohydrodynamic Characteristics. I. Data-driven Boundary Conditions
Authors: Lucas A. Tarr, N. Dylan Kee, Mark G. Linton, Peter W. Schuck, James E. Leake
Figure caption: Time–distance plot showing the horizontal expansion of the spheromak along the x-direction along the line (y = 0, z  b  = 1.11) for four primitive variables: (a) ρ, (b) B  z , (c) v  x , and (d) v  y . The approximate average expansion rate of ﹩{dx}/{dt}\approx 2/1.4\left[{L}_{N}/{T}_{N}\right]﹩ is indicated by the white dashed line.