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24 results for “photosphere”
ELISITY project; Dataset with the photospheric RFLH and various physical parameters for the ARs examined in the project
<p>Dataset with values of the photospheric relative field line helicity (RFLH) in two gauges and of various physical parameters (energies, helicities, quality metrics) for the seven solar active regions examined in the ELISITY project</p>
JWST NIRISS/SOSS analysis of HAT-P-18 b with a photospheric model and TACHELES
<ul> <li><strong>photosphere.csv and TACHELES.csv: </strong>Best-fit parameters for the photospheric (Mandel-Agol) and TACHELES fits of the unbinned light curves.</li> <li><strong>*_results.txt and *_spectrum_retrieved.txt: </strong>POSEIDON output files and best-fit spectra for photospheric and TACHELES models for each of the three stellar heterogeneity setups (no spot, single spot, two heterogeneities)</li> <li><strong>*.pdf: </strong>Corner plots for all POSEIDON fits</li> <li><strong>chromspec.csv: </strong>Chromospheric spectrum</li> </ul>
Animations: The Photospheric Footpoints of Solar Coronal Hole Jets
<p>This repository provides the individual animations of the SDO/AIA and HMI magnetograms of Jets 1, 2, 3, corresponding to jets 14, 32, 35 in Table 1 of the accepted manuscript, "<em>The Photospheric Footpoints of Solar Coronal Hole Jets</em>". </p> <p><strong>jet1-aia193.mp4</strong>: AIA 193A movie of Jet 1<br> <strong>jet1-hmimag.mp4</strong>: HMI magnetograms movie of Jet 1<br> <strong>jet1-aia193-hmi-contour.mp4:</strong> AIA 193A with HMI contours movie of Jet 1<br> <strong>fig1anim.mp4</strong>: Concatenation of Jet 1 movies shown in Figure 1 of the accepted manuscript.</p> <p><strong>jet2-aia193.mp4</strong>: AIA 193A movie of Jet 2<br> <strong>jet2-hmimag.mp4</strong>: HMI magnetograms movie of Jet 2<br> <strong>jet2-aia193-hmi-contour.mp4</strong>: AIA 193A with HMI contours movie of Jet 2<br> <strong>fig4anim.mp4</strong>: Concatenation of Jet 2 movies shown in Figure 4 of the accepted manuscript.</p> <p><strong>jet3-aia193.mp4</strong>: AIA 193A movie of Jet 3<br> <strong>jet3-aia304.mp4</strong>: AIA 304A movie of Jet 3<br> <strong>jet3-hmimag.mp4</strong>: HMI magnetograms movie of Jet 3<br> <strong>jet3-aia193-hmi-contour.mp4</strong>: AIA 193A with HMI contours movie of Jet 3<br> <strong>fig6anim.mp4</strong>: Concatenation of Jet 3 movies shown in Figure 6 of the accepted manuscript.<br> </p> <p> </p> <p> </p>
Flux Emergence Photospheric Data from Simulation with Twist 2
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Stellar chromospheric activity database of solar-like stars based on the Ca II H and K lines of LAMOST Low-Resolution Spectroscopic Survey: the bolometric and photospheric calibration
<p>This database contains the stellar chromospheric activity parameters of solar-like stars based on the Ca II H and K lines from the spectra of the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) Low-Resolution Spectroscopic Survey (LRS). We extract 1,122,495 LRS spectra of solar-like stars from the LAMOST Data Release 8 v2.0 and provide the chromospheric activity parameters $S_{\rm tri}$, $S_{\rm MWO}$, $R_{\rm HK}$ and $R'_{\rm HK}$, as well as their uncertainties in the database. $R_{\rm HK}$ and $R'_{\rm HK}$ are derived from the method in the classic literature (denoted with classic) and the method based on the PHOENIX model (denoted with PHOENIX). These stellar chromospheric activity indexes and their uncertainties, along with the relevant spectroscopic parameters from the LAMOST catalogs, are saved in a CSV-format file (name: CaIIHK_Activity_Indexes_LAMOST_DR8_LRS.csv).</p> <p> </p> <p>Columns in the catalog of the database:</p> <p>obsid - Unique observation identifier of LAMOST LRS spectrum</p> <p>obsdate-Spectral observation date</p> <p>fitsname - FITS file name of LAMOST LRS spectrum</p> <p>snrg - Signal-to-noise ratio in the $g$ band ($\mathrm{S/N}_g$) of LAMOST LRS spectrum</p> <p>snrr - Signal-to-noise ratio in the $r$ band ($\mathrm{S/N}_r$) of LAMOST LRS spectrum</p> <p>teff - Effective temperature ($T_\mathrm{eff}$) derived from the LASP (unit: K)</p> <p>teff_err - Uncertainty of $T_\mathrm{eff}$ derived from the LASP (unit: K)</p> <p>logg - Surface gravity ($\log\,g$) derived from the LASP (unit: dex)</p> <p>logg_err - Uncertainty of $\log\,g$ derived from the LASP (unit: dex)</p> <p>feh - Metallicity ([Fe/H]) derived from the LASP (unit: dex)</p> <p>feh_err - Uncertainty of [Fe/H] derived from the LASP (unit: dex)</p> <p>rv - Radial velocity ($V_r$) derived from the LASP (unit: km/s)</p> <p>rv_err - Uncertainty of $V_r$ derived from the LASP (unit: km/s)</p> <p>ra_obs - Right ascension (RA) of fiber pointing (unit: degree)</p> <p>dec_obs - Declination (DEC) of fiber pointing (unit: degree) </p> <p>gaia_source_id - Source identifier in Gaia DR3 catalog</p> <p>gaia_g_mean_mag - $G$ magnitude in Gaia DR3 catalog</p> <p>S_tri* - $S_{\rm tri}$ index of LAMOST LRS </p> <p>S_tri_err* - Uncertainty of $S_{\rm tri}$ </p> <p>S_MWO* - $S_{\rm MWO}$ </p> <p>S_MWO_err* - Uncertainty of $S_{\rm MWO}$ </p> <p>log_R_HK_classic* - $\log\,R_{\rm HK,classic}$ </p> <p>log_R_HK_classic_err* - Uncertainty of $\log\,R_{\rm HK,classic}$ </p> <p>log_R_p_HK_classic* - $\log\,R'_{\rm HK,classic}$ </p> <p>log_R_p_HK_classic_err* - Uncertainty of $\log\,R'_{\rm HK,classic}$ </p> <p>log_R_HK_PHOENIX* - $\log\,R_{\rm HK,PHOENIX}$ </p> <p>log_R_HK_PHOENIX_err* - Uncertainty of $\log\,R_{\rm HK,PHOENIX}$ </p> <p>log_R_p_HK_PHOENIX* - $\log\,R'_{\rm HK,PHOENIX}$ </p> <p>log_R_p_HK_PHOENIX_err* - Uncertainty of $\log\,R'_{\rm HK,PHOENIX}$ </p> <p>(Note: The columns denoted by an asterisk represent the parameters provided by this database, and the remaining columns are collected from the data release of LAMOST DR8 V2.0. If the values are not available, they will be filled with '-9999' in this database.)</p>
"Nowcasting Solar EUV Irradiance with Photospheric Magnetic Fields and the MgII Index" Figures, Scripts, and Data
<p>These tar files, scripts, and datasets were used in the paper "Nowcasting Solar EUV Irradiance with Photospheric Magnetic Fields and the MgII Index," submitted for publication to the Space Weather Journal. More information on what is included in this archive can be found the the ReadMe file. </p>
Pickled stellar photospheres (MARCS, Castelli & Kurucz) for Oracle
<p>These are just pickled photospheres from Castelli & Kurucz (2004) and MARCS (2011) for use with Oracle.</p>
Flux Emergence Photospheric Data from Simulation with Twist 0
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Flux Emergence Photospheric Data from Simulation with Twist 0.5
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Flux Emergence Photospheric Data from Simulation with Twist 1
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Probing the effect of cadence on the estimates of photospheric energy and helicity injections in eruptive active region NOAA AR 11158 – movies of the data series
<p>This dataset contains movies of all photospheric data series used in the article Lumme et al. (2019) “Probing the effect of cadence on the estimates of photospheric energy and helicity injections in eruptive active region NOAA AR 11158”, submitted. Movies track the evolution of several photospheric quantities in the NOAA active region 11158 from the emergence of the active region well beyond the time of the strongest eruptive activity in the region.</p> <p>The tracked quantities include: magnetic, plasma velocity and electric fields, as well as the vertical component of the Poynting vector and the relative helicity flux density. All quantities are given in several spatial and temporal resolutions: the cadences range from 2.25 minutes to 24 hours, and the spatial resolution is either the maximum resolution of the SDO/HMI instrument (0.03 deg in heliographic coordinates, 364 km on the Sun) or 15 times lower (0.45 deg, 5470 km). Since Lumme et al. (2019) employs three electric field inversion methods, PDFI, raw DAVE4VM and inductive DAVE4VM methods, there are three versions of the electric field maps as well as the derivative quantities Poynting and helicity fluxes for each cadence and spatial resolution.</p> <p>All series, except for the magnetic field and LOS plasma velocity series, are plotted only at the central strong field parts of the active region. The temporal extent of the series used in the paper is Feb 10 14:00 – Feb 17 00:00, 2011. However, some of the movies span only the the most interesting part of the evolution Feb 13 00:00 onward, after which the active region started to exhibit strong flux emergence and energy and helicity fluxes.</p> <p>All movie files in the dataset are given using the following naming convention: “{quantity}_{method}_{cadence}_{res_info}.avi”, where “quantity” specifies the plotted quantity (e.g. horizontal electric field “Eh”), “method” specifies the method used to derive the quantity (e.g., “PDFI” for electric field; if empty, no method is specified), “cadence” specifies the cadence of the data either in minutes or hours (e.g. “2.25_min” or “12_h”), and “res_info” specifies the spatial resolution (if empty then, the data is given in full resolution, otherwise “res_info” is “rebin_15x” corresponding to the 15 lower spatial resolution).</p> <p> Movies of the following data series are included for all cadences and spatial resolutions.:<br> - All three components of the photospheric magnetic field “(Bx,By,Bz)” in a Cartesian basis where the solar surface is approximated flat via Mercator projection, as well as the vertical component of the magnetic field “Bz” and the LOS component of the plasma velocity “Vlos” (i.e. Dopplergram velocity) in the same system (note that the unlike in the usual convention, the LOS plasma velocity is negative for motions away from the observer). These data series are given only for two cadences 2.25- and 12-minutes in full spatial resolution, since rest of the cadences are created by sampling the 2.25-minute data. Data in the 15 times lower spatial resolution are given only at a cadence of 2.025 hours, as it is the highest cadence for which the 15 times lower resolution was used (see Lumme et al., 2019 for details).<br> - Horizontal photospheric plasma velocity "Vh = (Vx,Vy)" estimates derived using two optical flow methods FLCT (Fourier Local Correlation Tracking) and DAVE4VM (Differential Affine Velocity Estimator For Vector Magnetograms) plotted as arrows above the Bz component of the magnetic field.<br> - Horizontal photospheric electric field “Eh = (Ex,Ey)” estimates derived using three methods, PDFI, raw DAVE4VM and the inductive DAVE4VM method, plotted as arrows above the Bz component of the magnetic field.<br> - Vertical component of the Poynting vector “Sz” derived for each electric field estimate.<br> - Photospheric relative helicity flux density (denoted by “dHR/dt”) derived for each electric field estimate.</p> <p>January 16, 2019<br> Erkka Lumme<br> Doctoral student, MSc<br> Department of Physics<br> erkka.lumme@helsinki.fi<br> P.O. Box 68<br> FI-00014 University of Helsinki</p>
MESA input and software files for: 'The imprint of convection on Type I X-ray bursts: Pauses in photospheric radius expansion lightcurves'
<p>Inlists, input models, and other machinery needed to reproduce results in "The imprint of convection on Type I X-ray bursts: Pauses in photospheric radius expansion lightcurves". Includes data files (profiles and histories, and also some movies) for the main "Schwarzschild" run.</p> <p>MESA version: 15140</p> <p>See the README.md for instructions on how to run.</p> <p> </p>
Svalbox 2022 Spring Reconnaissance - Western Spitsbergen photosphere data
<p>360 degree photosphere data for the West Spitsbergen 2022 Svalbox reconnaissance collected in spring 2022.</p>
Longyearbyen - Svea 2021 - 360 degree photospheres
<p>360 degree photosphere acquisition along the Longyearbyen to Svea, Svalbard route recording while driving snowmobiles.</p>
Pickled Stagger-Grid stellar photospheres for Oracle
<p>This dataset contains Python-pickled Stagger-Grid stellar photospheres by Magic et al. (2013).</p>
Flux Emergence Photospheric Data from Simulation with Twist 2 - Just Magnetic Field
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Flux Emergence Photospheric Data from Simulation with Twist 0.5 - Just Magnetic Field
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Flux Emergence Photospheric Data from Simulation with Twist 1 - Just Magnetic Field
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Flux Emergence Photospheric Data from Simulation with Twist 0 - Just Magnetic Field
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Svalbox 2023 GoNorth - 360 degree Photospheres
<p>Photospheres acquired during the Svalbox GoNorth Expedition in spring 2023.</p>
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International Brain Laboratory public data
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OpenNeuro
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