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97 results for “helium”
Dataset of publication "Speed of Sound Measurements in Helium at Pressures from 15 to 100 MPa and Temperatures from 273 to 373 K"
<p>This is a dataset of the speed of sound in helium, which was measured along five isotherms in a temperature range from 273 to 373 K at pressures from 15 to 100 MPa with a relative expanded uncertainty (k = 2) from 0.02 to 0.04%. A dual-path pulse-echo device was utilized to conduct these measurements.</p>
Measurement of energies and intensities of multiple ionization satellite (MIS) excited in light elements by helium ion beams
<p>TNA project number: <strong>19001708-ST</strong></p> <p><strong>Measurement of energies and intensities of multiple ionization satellite (MIS) excited in light elements by helium ion beams</strong></p> <p><em>Scientific background:</em></p> <p>Over 1600 X-ray spectra have been collected from the alpha particle X-ray spectrometers on Mars rovers including the present Curiosity rover. The spectra are excited by the radionuclide <sup>244</sup>Cm, which emits 5 MeV He ions for PIXE and Pu L X-rays for XRF. These spectra provide elemental analysis of rocks, soils and dust as part of the quest to identify formerly habitable (water-bearing) environments. Applicant is a member of the Curiosity APXS team within NASA’s Mars Science Laboratory. Excitation of K X-rays by 5 MeV He ions produces also energy-shifted satellites due to 1, 2 or 3 L-shell spectator vacancies. These cause significant distortion of the diagram lines and worsen the quality of spectrum fits by the GUPIX(Mars) code. An MIS database is needed to support a correction procedure that is already devised. This work will increase analytical accuracy and will also support more accurate terrestrial PIXE analysis using alpha beams, especially when partnered with RBS; this could lead to increased use of these two IBA methods in a complementary manner.</p> <p> </p> <p><em>Measurements performed within TNA project:</em></p> <p>The wavelength-dispersive in-vacuum x-ray spectrometer of J. Stefan Institute (Ljubljana, Slovenia) [1] have been used to record high energy resolution KaL<sup>N</sup> X-ray spectra of Ca and Cr induced in collisions with MeV alpha particles. The targets used were metallic Cr, Cr<sub>2</sub>O<sub>3</sub>, and CaF<sub>2</sub>. The KaL<sup>N</sup> X-ray spectra of Cr and Cr<sub>2</sub>O<sub>3</sub> were measured using three different energies of He ions, namely 3 MeV, 4 MeV and 5 MeV. For CaF<sub>2</sub> we have collected only spectra induced with 5 MeV He beam. The main purpose of the experiment was to record KaL<sup>N</sup> spectra with good enough statistics to determine precisely energy/intensity of the corresponding satellite lines. The results for the energy shifts and relative intensities of the groups will be incorporated in the MIS database providing an empirical means for inclusion of one peak per satellite group when modelling energy-dispersive spectra (GUPIX(Mars) code).</p> <p>[1] M. Kavčič, M. Budnar, A. Mühleisen, F. Gasser, M. Žitnik, K. Bučar, R. Bohinc, <em>Design and performance of a versatile curved-crystal spectrometer for high-resolution spectroscopy in the tender x-ray range</em>, Rev. Sci. Instr. 83, 033113 (2012). <a href="http://dx.doi.org/10.1063/1.3697862">http://dx.doi.org/10.1063/1.3697862</a></p> <p> </p> <p><em>Data files:</em></p> <p>We are sharing the detector files (a series of single exposure 2D raw images) collected by the Andor DX438-BV CCD camera (770 × 1152 pixels with pixel size 22.5×22.5 <em>μ</em>m<sup>2</sup>) after the diffraction on the crystal analyzer. The horizontal axis of the detector corresponds to the dispersion axis and diffracted photons are detected at different horizontal positions according to their wavelength, the vertical axis of the detector serves mainly to accumulate more statistics. The final emission spectra are obtained from the corresponding detector files using the home-written data processing software.</p> <p> </p> <p> </p>
Data for "Schlieren and BOS velocimetry of a round turbulent helium jet in air"
<p>This is a subset of data used in our publication <a href="https://arxiv.org/abs/2202.04122">Schlieren and BOS velocimetry of a round turbulent helium jet in air</a> </p> <p> </p> <p>In the four helium-jet schlieren-image datasets given below, the nozzle diameter is 1.4 mm, the camera frame rate is 6000 fps and the individual image exposure is 0.0001667 s. 3000 images are provided for each dataset, or 1/2 s in real-time, which we determined to provide statistically-adequate data. Please see the <a href="https://arxiv.org/abs/2202.04122">paper</a> for more detail.</p> <p><strong>20210125-Run1</strong>: traditional mirror-schlieren, $Re_d = 5,890$, $U_j = 436$ m/s, and the scale is 0.29 mm/pixel.</p> <p><strong>20210206-Run1</strong>: traditional mirror-schlieren, $Re_d = 11,300$, $U_j = 682$ m/s, and the scale is 0.29 mm/pixel.</p> <p><strong>20210419-Run1</strong>: background-oriented schlieren (BOS), $Re_d = 5,890$, $U_j = 436$ m/s, and the scale is 0.26 mm/pixel. These are raw BOS images that must be processed with a reference image in order to yield pseudo-schlieren results. The reference (flow-off, tare) image is the first image in the sequence and is so named.</p> <p><strong>20210420-Run1</strong>: background-oriented schlieren (BOS), $Re_d = 11,300$, $U_j = 682$ m/s, and the scale is 0.26 mm/pixel. These are raw BOS images that must be processed with a reference image in order to yield pseudo-schlieren results. The reference (flow-off, tare) image is the first image in the sequence and is so named.</p>
An observed population of intermediate-mass helium stars that have been stripped in binaries - theoretical, computational and observational data
<p>This Zenodo repository contains the observational and computational data presented in the manuscript "An observed population of intermediate-mass helium stars stripped in binaries" by Drout, Götberg, Ludwig, Groh, de Mink, O'Grady and Smith.</p><p>We organize the data as follows:</p><ul><li>The stacked spectra presented in Figures S16-S21 are located in stacked_spectra.tar.gz, which contains a text file for each star. The text files have three columns that correspond to wavelength in Angstrom, normalized counts, and errors, respectively.<br> </li><li>The spectral model grid computed based on binary evolutionary model output and presented in detail in the Supplementary information section S1.2.1, is labeled with names starting S121. The file S121_evol_based_006_absolute_magnitudes.txt contains the absolute AB magnitudes for the models in UV and optical filters. The .tar.gz S121_evol_based_006_spectra.tar.gz contains files with the full spectral energy distribution and normalized spectra of each model. The .tar.gz S121_evol_based_006_complete_models.tar.gz contains the full CMFGEN models.<br> </li><li>For the stellar atmosphere model grid presented in Supplementary material section S1.2.2, we refer to the Zenodo repository 10.5281/zenodo.7976200, which is made available in association with the second paper in our series. We note that we used a subset of that grid in the article associated with this Zenodo repository. We refer to section S1.2.2 for more details.<br> </li><li>The spectral models demonstrating the mass loss rate variations in Supplementary information section S1.2.3 are presented here with names starting with S123. There is one file containing the absolute magnitudes (S123_mdot_variation_absolute_magnitudes.txt), the S123_mdot_variation_spectra.tar.gz contains the spectral energy distributions and normalized spectra for each of the models, and the S123_mdot_variation_complete_models.tar.gz contains the full CMFGEN models.<br> </li><li>The spectral model grid computed based on main-sequence evolutionary model output and presented in detail in the Supplementary information section S1.3.1, is labeled with names starting S131. The file S131_MS_evol_based_006_absolute_magnitudes.tar.gz contains three files with the absolute AB magnitudes for the models in the UV and optical filters, each file corresponding to either 20%, 60%, or 90% through the main-sequence evolution and labeled f20, f60, and f90, respectively. S131_MS_evol_based_006_spectra.tar.gz contains three folders labeled f20, f60 and f90, which each contains the SEDs (in Flambda and ABmag) and normalized spectra for the corresponding models. The files S131_MS_evol_based_006_complete_models_fX0.tar.gz contain the complete CMFGEN models.<br> </li><li>The custom index files we use for astrometry.net in section S3.1.1 are located in the zip file called S311_astrometry_index_files.zip. This information was used to recalculate the astrometry on the Swift UVOT images of the Magellanic Clouds.<br> </li><li>To make Figure 2B, we calculated the equivalent widths for a set of models assuming a signal-to-noise ratio of 35. This procedure is described in Section S3.7.2. In Figure2B_Model_EWs.zip, we provide three files that each contain these modeled equivalent widths for (1) stripped star models, (2) OB star models, and (3) composite models. <br> </li><li>To make Figure S7 (see also Sections S1.2.3 and S2.2), which is similar to Figure 2B, but presents the effects of varying the wind mass loss of stripped stars, we used a similar set of modeled equivalent widths as when we produced Figure 2B. These modeled equivalent widths are provided in FigureS7_Model_EWs.zip. <br> </li><li>To make Figure 3, we calculated equivalent widths for the model grid described in Section S1.2.2 and the TLUSTY OB star grids (see Section S1.3.2) assuming a signal-to-noise ratio of 100. These model equivalent widths are provided in the file called Figure3_Model_EWs.zip. </li></ul>
HPF data for "A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation"
<p>Data from the Habitable Zone Planet Finder (HPF) Spectrograph at McDonald Observatory, in the form of high resolution infrared echelle spectra. The target is HAT-P-67, a planet host star. The spectra were acquired by Queue observations with the Hobby Eberly Telescope in the period 2020-2022. The data were reduced with the "Goldilocks" pipeline. The full dataset is described in detail in the paper "A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation". </p> <p>The abstract for that paper is reproduced below:</p> <div> <div>Atmospheric escape shapes the fate of exoplanets, with statistical evidence for transformative mass loss imprinted across the mass-radius-insolation distribution. Here we present transit spectroscopy of the highly irradiated, low-gravity, inflated hot Saturn HAT-P-67 b. The Habitable Zone Planet Finder (HPF) spectra show a detection of up to 10% absorption depth of the 10833 Angstrom Helium triplet. The 13.8 hours of on-sky integration time over 39 nights sample the entire planet orbit, uncovering excess Helium absorption preceding the transit by up to 130 planetary radii in a large leading tail. This configuration can be understood as the escaping material overflowing its small Roche lobe and advecting most of the gas into the stellar---and not planetary---rest frame, consistent with the Doppler velocity structure seen in the Helium line profiles. The prominent leading tail serves as direct evidence for dayside mass loss with a strong day-/night- side asymmetry. We see some transit-to-transit variability in the line profile, consistent with the interplay of stellar and planetary winds. We employ 1D Parker wind models to estimate the mass loss rate, finding values on the order of 2x10^13 g/s, with large uncertainties owing to the unknown XUV flux of the F host star. The large mass loss in HAT-P-67 b represents a valuable example of an inflated hot Saturn, a class of planets recently identified to be rare as their atmospheres are predicted to evaporate quickly. We contrast two physical mechanisms for runaway evaporation: Ohmic dissipation and XUV irradiation, slightly favoring the latter.</div> </div>
A seven-Earth-radius helium-burning star inside a 20.5-min detached binary
<p><strong>2024-02-19 updated for including the full MESA inlists of evolutionary models.</strong></p> <p><strong>MESA_inlist.zip</strong> -<strong> </strong>the full MESA inlists of evolutionary models (including evolutions of single stars and binaries).</p> <p>_____________________________________________________________________________________________________________________</p> <p>This record contains the data of spectra, photometries and models used for the paper <em><strong>A seven-Earth-radius helium-burning star inside a 20.5-min detached binary</strong>,<a href="https://www.nature.com/articles/s41550-023-02188-2"> click here</a></em></p> <p><strong>J0526_fchart.png</strong> - the finder chart of J0526;</p> <p><strong>J0526_Keck_[0-5].spec </strong> (in Keck_ori_spectra.zip)<strong> </strong>- Keck I/LRIS spectra of J0526;</p> <p><strong>J0526_GTC_[0-6].spec </strong> (in GTC_ori_spectra.zip)<strong> </strong>- GTC/OSIRIS spectra of J0526;</p> <p><strong>J0526_GTC_syn_[0-6].spec </strong> (in GTC_spectra_models.zip)<strong> </strong>- GTC/OSIRIS spectra and their best-fit TLUSTY/Synspec spectra;</p> <p><strong>J0526_RV_bary_corrected.dat</strong> - the barycenter-corrected radial velocities derived from LRIS and OSIRIS spectra;</p> <p><strong>J0526_SED.dat</strong> - the photometric fluxes in the broad-band SED and corresponding synthetic fluxes from the best-fit model spectrum;</p> <p><strong>ZTF_J0526_[r,g].dat </strong>(in light_curves.zip) - ZTF <em>r</em>-/<em>g</em>-band light cuvrs of J0526, the raw data were provided by NASA/IPAC Infrared Science Archive (<a href="https://irsa.ipac.caltech.edu/">https://irsa.ipac.caltech.edu</a> );</p> <p><strong>Lijiang_J0526_[r,g].dat </strong>(in light_curves.zip) - LJT <em>r</em>-/<em>g</em>-band light cuvrs of J0526;</p> <p><strong>TMTS_J0526_L.dat </strong>(in light_curves.zip) - LJT <em>L</em>-band light cuvrs of J0526;</p> <p><strong>CHeB_c[0.32,0.33,0.34]+H1e-6.track</strong> (in MESA_models.zip) - the evolutionary tracks for core helium-burning stars with He-core mass of [0.32,0.33,0.34] M<sub>sun</sub> and H-envelope mass of 1e-6 M<sub>sun</sub>;</p> <p><strong>ZAHeMS_H0_sequence.dat</strong> (in MESA_models.zip) - the zero-age He-star sequence (without H envelope);</p> <p><strong>ZAHeMS_H1e-6_sequence.dat</strong> (in MESA_models.zip) - the zero-age He-star sequence (with H-envelope mass of 1e-6 M_sun );</p> <p><strong>binary_0.33+0.735.dat </strong> (in MESA_models.zip) - the binary evolutionary track for a core helium-burning star (M<sub>core</sub>=0.33 M_sun, M<sub>env</sub>=1e-6 M_sun ) and a CO WD (M=0.735 M_sun);</p> <p><strong>binary_0.36+0.735.dat </strong> (in MESA_models.zip) - the binary evolutionary track for a core helium-burning star (M<sub>core</sub>=0.36 M_sun, M<sub>env</sub>=1e-6 M_sun ) and a CO WD (M=0.735 M_sun);</p> <p><strong>J0526_[SED, RV, lc]_fit_corner.png</strong> - the corner plots for [SED, RV, light curve] MCMC fit.</p>
Apatite and Zircon Helium Data from the Wallowa and Elkhorn Mountains
<p>Apatite and Zircon Helium thermochronometry data from the Wallowa and Bald Mountain Batholiths, Oregon, USA. Dataset accompanies the paper "Multiphase topographic and thermal histories of the Wallowa and Elkhorn Mountains, Blue Mountains Province, Oregon, USA" published in Tectonics.</p>
Synthetic populations and trajectories for sdB stars ejected from the single degenerate helium donor channel for thermonuclear supernovae
<p>This repository is a supplement to a journal paper (Neunteufel+ 2022) and contains the synthetic populations of sdB stars and sdB remnants ejected from the single degenerate helium donor channel for thermonuclear supernovae. See Neunteufel+ 2021 and Neunteufel+ 2022 for simulation parameters. </p> <p>Synthetic populations, including initial and final positions, are contained in the MXX-out.tr (XX=10..15) files where XX is the mass of the WD companion divided by 0.1 solar masses. Each population is a snapshot of stars ejected at the end of a 300 Myr period. (Note that stellar lifetimes are not taken into account here. See Neunteufel+ 2022 on how stellar lifetimes should be truncated in order to produce realistic populations.)</p> <p>Columns:</p> <p>Zeroth column (ID) is the ID of the trajectory. These are assigned consecutively.</p> <p>First column (unnamed) indicates initial (0) and final (1) positions.</p> <p>Third column (time) is the time since ejection in Myrs. Note that stars further down in the list were ejected earlier.</p> <p>Fourth to Ninth columns (vx, y, vy etc..) are velocity (km/s) and position (kpc) in Gal. Carthesian coordinates (velocity first, position second)</p> <p>Tenth to Twelfth column are accelerations in Gal. carthesian coordinates </p> <p>Thirteenth column (v_space) is the total galactocentric space velocity (km/s) </p> <p>Fourteenth column (Phi) is the local Gal. potential according to Model 1 presented by Irrgang+2013</p> <p>Fifteenth column (E_kin/E_pot) is the local kinetic energy of the object divided by its potential energy with respect to the Gal. potential.</p> <p>Sixteenth column (rho) is the local Gal. baryon density according to Model 1 presented by Irrgang+2013</p> <p>Seventeenth column (label_c) is the mass of the ejected sdB star or sdB remnant in solar masses.</p>
QMC Raw Data for Graphene Corrugation Effects during Helium Adsorption
<h2>Graphene Corrugation Data Files</h2> <p> </p> <p>Raw quantum Monte Carlo data and submission scripts for a publication studying the effects of graphene corrugation on helium adsorption. </p> <p>View README.md for more information on repository contents. Updated version (2024-04-28) contains larger system sizes (N_G = 72,108).</p> <p>Fully corrugated lookup tables for isotropic graphene can be found here: https://zenodo.org/records/6574043</p>
Helium Ion Density Ratios Upstream from Mars
<p>This data set contains ratios of singly to doubly ionized helium computed from MAVEN STATIC measurements made upstream from Mars in the magnetosheath and upstream solar wind. </p>
e-MERLIN images in Kool et al. 2023 A radio-detected thermonuclear supernova from a single-degenerate progenitor with a helium star donor
<p>Fits images obtained with e-MERLIN on Nov 19 2021 and April 6-11 2022 on SN2020eyj. Results are published in Kool et al. 2023 "A radio-detected thermonuclear supernova from a single-degenerate progenitor with a helium star donor".</p> <p>Project RR12002<br> Target name: 1111+2923<br> Original observation correlation centre: 11:11:47.180000 +29.23.06.36000<br> Run code: RR12002_C_001_20211119</p> <p>Project RR13005<br> Target name: 1111+2923<br> Original observation correlation centre: 11:11:43.271400 +29.23.37.83200<br> Run codes (combined):<br> RR13005_C_001_20220406<br> RR13005_C_002_20220407<br> RR13005_C_003_20220408<br> RR13005_C_004_20220409<br> RR13005_C_005_20220410<br> RR13005_C_006_20220411</p> <p> </p>
Calculated values of the third dielectric virial coefficient of helium-4, neon-20, and argon-40
<p>Calculated values of the third dielectric virial coefficient of helium-4 (file Ceps_He4.dat), neon-20 (file Ceps_Ne20.dat), and argon-40 (file Ceps_Ar40.dat)</p> <p>ASCII format. Each file has a header whose lines begin with # describing the content.</p> <p>For details on the calculation see <a href="https://doi.org/10.1063/5.0077684">https://doi.org/10.1063/5.0077684</a> or <a href="https://arxiv.org/abs/2111.02691">https://arxiv.org/abs/2111.02691</a></p>
Calculated values of the fourth virial coefficient of helium-3 and helium-4
<p>Calculated values of the fourth virial coefficient of helium-3 (file named D_He3.dat) and helium-4 (file named D_He4.dat)</p> <p>ASCII format. Each file has a header whose lines begin with # describing the content.</p> <p>For details on the calculation see <a href="https://doi.org/10.1063/5.0043446">https://doi.org/10.1063/5.0043446</a> or <a href="https://arxiv.org/abs/2101.02624">https://arxiv.org/abs/2101.02624</a></p>
Supporting Information for "Wave heating during the helium flash and lithium-enhanced clump stars"
<p>"data" contains the data used to generate the plots in this paper.</p> <p>"batches" contains a log of nearly every MESA run performed in this work (including ~all failed experiments). These are stored as Python3 Pickle files. Experiments were run using the RemoteExperiments software package (https://github.com/adamjermyn/remote_experiments). See the documentation there for further information on the data format for these files.</p> <p>"Stokes_Experiments" contains a git repository which includes both the final version of the code used in our canonical run as well as the full history of (nearly) all experiments we performed along the way. Each experiment is a commit (detached from any branch) with the commit message "patch".</p> <p>"Scripts" contains both the scripts we used to run these experiments and those we used to analyze them and make the plots in the paper.</p> <p>Further detail is given in the paper itself.</p>
Data and GenX analysis for "Liquid Helium as a reference may provide clarity for some neutron reflectometry experiments"
<p>Data and GenX analysis for "Liquid Helium as a reference may provide clarity for some neutron reflectometry experiments"</p>
The kinetics of arsenolite inclusion compounds formation with hydrogen and helium - FTIR data
<p>Raw FT-IR spectra of arsenolite and its inclusion compound with hydrogen. The spectra were collected at the Synchrotron SOLEIL during beamtime under proposal no. 20210258</p>
Vapor pressure of helium at different temperatures
<p><strong>Vapor pressure of helium at different temperatures</strong></p> <p>Junjie Chen</p> <p>Department of Energy and Power Engineering, School of Mechanical and Power Engineering, Henan Polytechnic University, 2000 Century Avenue, Jiaozuo, Henan, 454000, P.R. China</p> <p>Contributor: Junjie Chen, ORCID: 0000-0001-5055-4309, E-mail address: komcjj@gmail.com</p> <p> </p> <p>Helium is a chemical element, inert gas of Group 18 of the periodic table. The second lightest element (only hydrogen is lighter), helium is a colourless, odourless, and tasteless gas that becomes liquid at temperature of -268.9 degrees Celsius. The boiling and freezing points of helium are lower than those of any other known substance. Helium is the only element that cannot be solidified by sufficient cooling at normal atmospheric pressure; it is necessary to apply pressure of 25 atmospheres at a temperature of -272 degrees Celsius to convert it to its solid form. Helium gas is isolated from natural gas by liquefying the other components at low temperatures and under high pressures. Adsorption of other gases on cooled, activated charcoal yields 99.995 percent pure helium. Some helium is supplied from liquefaction of air on a large scale; the amount of helium obtainable from 1,000 tons of air is about 3.17 cubic metres, as measured at room temperature and at normal atmospheric pressure. Helium is used as an inert-gas atmosphere for welding metals such as aluminum; in rocket propulsion (to pressurize fuel tanks, especially those for liquid hydrogen, because only helium is still a gas at liquid-hydrogen temperature); in meteorology (as a lifting gas for instrument-carrying balloons); and in cryogenics (as a coolant because liquid helium is the coldest substance). Meteorites and rocks have been analyzed for helium content as a means of dating.</p> <p>Temperature (degrees kelvin), Pressure (kilopascals)</p> <p>2.2 5.332</p> <p>2.3 6.725</p> <p>2.4 8.351</p> <p>2.5 10.23</p> <p>2.6 12.38</p> <p>2.7 14.81</p> <p>2.8 17.56</p> <p>2.9 20.64</p> <p>3 24.06</p> <p>3.1 27.85</p> <p>3.2 32.02</p> <p>3.3 36.6</p> <p>3.4 41.6</p> <p>3.5 47.04</p> <p>3.6 52.94</p> <p>3.7 59.31</p> <p>3.8 66.19</p> <p>3.9 73.58</p> <p>4 81.51</p> <p>4.1 90</p> <p>4.2 99.08</p> <p>4.3 108.8</p> <p>4.4 119.1</p> <p>4.5 130.1</p> <p>4.6 141.7</p> <p>4.7 154.1</p> <p>4.8 167.3</p> <p>4.9 181.3</p> <p>5 196.2</p> <p>5.1 212.1</p> <p>Contributor: Junjie Chen, ORCID: 0000-0001-5055-4309, E-mail address: komcjj@gmail.com, Department of Energy and Power Engineering, School of Mechanical and Power Engineering, Henan Polytechnic University, 2000 Century Avenue, Jiaozuo, Henan, 454000, P.R. China</p>
Supplementary Material for: "Kink-Helium Interactions in Tungsten: Opposing Effects of Assisted Nucleation and Hindered Migration"
<p>This uploaded contains the supporting material and files for the pre-print titled: ”Kink-Helium Interactions in Tungsten: Opposing Effects of Assisted Nucleation and Hindered Migration”.</p> <p> </p> <p>MN is supported by a studentship funded by the UK Engineering and Physical Sciences Research Council–supported Centre for Doctoral Training in Modelling of Heterogeneous Systems, Grant No. EP/S022848/1 and the Atomic Weapons Establishment. JRK acknowledges funding from the Leverhulme Trust under grant RPG-2017-191. APB acknowledges support from the CASTEP-USER project, funded by the Engineering and Physical Sciences Research Council under the grant agreement EP/W030438/1. JRK and APB acknowledge funding from the NOMAD Centre of Excellence funded by the European Commission under grant agreement 951786. We acknowledge the University of Warwick Scientific Computing Research Technology Platform for assisting the research described within this study. Some of the calculations were performed using the Sulis Tier 2 HPC platform hosted by the Scientific Computing Research Technology Platform at the University of Warwick. Sulis is funded by EPSRC Grant EP/T022108/1 and the HPC Midlands+ consortium. We are grateful for computational support from the UK national high performance computing service, ARCHER2, for which access was obtained via the UKCP consortium and funded by EPSRC Grant No. EP/X035891/1.</p>
Evolution models of helium white dwarf-main-sequence star merger remnants: the mass distribution of single low-mass white dwarfs
<p>Inlists and data for "<a href="https://ui.adsabs.harvard.edu/#abs/2018MNRAS.474..427Z/abstract">Evolution models of helium white dwarf-main-sequence star merger remnants: the mass distribution of single low-mass white dwarfs</a>"</p>
Exploring the Helium Core of the δ Scuti Star CoRoT 102749568 with Asteroseismology
<p>MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/#abs/2017ApJ...834..146C/abstract">Chen et al. (2017)</a>. MESA version 7624.</p> <p>Publication DOI: <a href="https://doi.org/10.3847/1538-4357/834/2/146">10.3847/1538-4357/834/2/146</a></p>
ScienceDex guides
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These curated guides explain access requirements, typical timelines, costs, and reuse considerations for widely used research datasets.
Allen Brain Atlas
Allen Brain Atlas is an Allen Institute collection of brain map atlases, datasets, APIs, and analysis tools covering mouse, human, and non-human primate brain resources.
Annotated Behaviour and Observability Dataset (ABODe)
ABODe is a University of Edinburgh DataShare dataset for behavior classification in group-housed mice using home-cage video, identities, bounding boxes, ground-plate positions, and annotator labels.
DANDI Archive for NWB datasets
DANDI is a BRAIN Initiative archive for publishing and sharing neurophysiology data, including electrophysiology, optophysiology, and behavioral data packaged as NWB and related standards.
International Brain Laboratory public data
The International Brain Laboratory public data releases expose standardized mouse decision-making experiments, including Neuropixels recordings, widefield calcium imaging, behavior, and session metadata accessed through the ONE API.
OpenNeuro
OpenNeuro is a free, open platform for sharing neuroimaging datasets, with public search, dataset pages, and download paths for web, S3, DataLad, and the OpenNeuro CLI.