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zenodo52/100

Supplement to: Electron energy partition across interplanetary shocks

Quick Summary: The three files herein comprise supplemental information and standalone datasets for a three-part study of Electron energy partition across interplanetary shocks that describe the modeling of solar wind electron velocity distribution functions (VDFs) near interplanetary shocks observed by the Wind spacecraft.  Part I of the study (published in the The Astrophysical Journal Supplement Series on July 3, 2019 doi:10.3847/1538-4365/ab22bd) describes the methodology and how the two ASCII files (i.e., those stored here) were created and their contents.  Part I also explains the nuances of the analysis, the limitations of the dataset, and how to use the data within the two ASCII files.  Parts II and III (in preparation) present the statistical results and the detailed analysis of these results in the context of the dependence on relevant interplanetary shock parameters.  Below are the descriptions of each data product starting with the PDF supplemental file to the three-part study and then the associated ASCII files.  First we provide some background/definitions of jargon and terms used in each. Solar Wind Electrons: The solar wind electron VDF below ~1 keV is comprised of cold, dense core (subscript c or ec) population with thermal energies typically in the ~5-15 eV range, a hot, tenuous halo (subscript h or eh) population with thermal energies typically >20-30 eV, and an anti-sunward, field-aligned beam called the strahl or beam/strahl (subscript b or eb) population with thermal energies typically ~few 10s of eV.  Most previous work modeled the core as a bi-Maxwellian and the halo and beam/strahl as bi-kappa VDFs.  The work described in Part I (and the PDF supplement stored here) show that the core is more accurately described by a self-similar model VDF, which reduces to a bi-Maxwellian under appropriate conditions/limits and deviation from Maxwellian quantifies inelasticity in the plasma collisions.  That is, if the plasma were controlled by elastic Coulomb particle-particle collisions (e.g., in the low corona or chromosphere or photosphere), the VDF would relax to a Maxwellian in the absence of other forces.  When the plasma particles undergo inelastic collisions, the VDF profile changes from a Gaussian to something more like a "flattop" or box-like shape. Wind Spacecraft: The Wind spacecraft (<a href="http://wind.nasa.gov">https://wind.nasa.gov</a>) was launched on November 1, 1994 and currently orbits the first Lagrange point between the Earth and sun.  It holds a suite of instruments from gamma ray detectors to quasi-static magnetic field instruments, Bo.  The instruments used in this study and these datasets are the fluxgate magnetometer (MFI), the radio receivers (WAVES), ion Faraday cups (SWE), and the electron and ion electrostatic analyzers (3DP).  The MFI measures 3-vector Bo at ~11 samples per second (sps); the SWE measures reduced VDFs of the thermal proton and alpha-particle populations from which velocity moments are derived and used herein; WAVES observes electromagnetic radiation from ~4 kHz to >12 MHz which provides an observation of the upper hybrid line (also called the plasma line) used to define the total electron density; and 3DP observes full 4π steradian VDFs of electrons and ions from a few eV to ~30 keV which provide both ion velocity moments and the electron VDFs modeled herein. PDF Supplement Description: The PDF document contains descriptions and definitions of relevant interplanetary shock parameters and shock analysis techniques used by the Harvard Smithsonian Center for Astrophysics' Wind shock database at <a href="https://www.cfa.harvard.edu/shocks/wi_data/">https://www.cfa.harvard.edu/shocks/wi_data/</a>.  It describes the details of the symbols/parameters used on the database website and their translation to plasma parameters or shock parameters.  The PDF also defines the shock normal finding techniques listed as two-four character inputs on the database website.  The PDF file lists the shocks analyzed and their relevant parameters in two tables, with the second listing the relevant critical Mach numbers.  Next the PDF provides some extra statistics of the analysis performed in the three-part study on Electron energy partition across interplanetary shocks in the form of histograms comparing differences for different selection criteria (e.g., low versus high Mach number shocks).  Finally, there are detailed descriptions and definitions of the model functions used to fit to the solar wind electron VDFs. Both ASCII files have detailed headers outlining and defining the parameters contained therein.  They also provide column headings where the labels/names of each are defined and/or described in the header.  The headers also provide links to the analysis software used to perform the model fits to the VDFs.  We will first describe the contents of the file labeled Wind_ip_shock_3dp_fit_constraints_electrons.txt (FCONSTS for brevity) and then the file labeled Wind_ip_shock_3dp_fit_results_electrons.txt (FRESULTS for brevity).  Below use the following definitions: <ul> <li>$N_{s}$ = number density of species s [cm-3] (s = ec for core, eh for halo, eb for beam/strahl, p for proton, etc.)</li> <li>$B_{o, j}$= jth component (GSE coordinate basis) of quasi-static magnetic field vector [nT]</li> <li>$V_{Ts, j}$ = jth component (relative to Bo) of thermal speed of species s [km/s] <ul> <li>$V_{Ts,j} = \sqrt{{2 k_{B} T_{s,j} \over m_{s}}}$, where $T_{s, j}$ is the jth component (relative to Bo) of the temperature of species s [eV]</li> </ul> </li> <li>$V_{os, j}$ = jth component (relative to Bo) of drift speed of species s [km/s] in ion rest frame</li> <li>$V_{s, j}$ = jth component (GSE coordinate basis) bulk velocity of species s [km/s] in spacecraft frame</li> <li>$T_{s, tot} = {1 \over 3} (T_{s, \parallel} + 2 \ T_{s, \perp})$, where $\parallel(\perp)$ is the parallel(perpendicular) component relative to Bo</li> <li>$s_{es}$ = exponent for the symmetric self-similar model VDF of species s</li> <li>$\kappa_{es}$ = kappa value for the bi-kappa VDF of species s</li> <li>$p_{es}(q_{es})$ = parallel(perpendicular) exponent for the asymmetric self-similar model VDF of species s</li> <li>$\chi_{s}^{2}$ = least chi-squared of fit to species s</li> <li>$\phi_{sc}$ = spacecraft electric potential [eV]</li> <li>$\delta R = \lvert 1 - Median(f^{data}/f^{model}) \rvert$ = excess median deviation of fit [%]</li> </ul> FCONSTS File Description: The FCONSTS file contains all the pertinent information used during the fit process for all VDFs that were analyzed including the fit results.  The columns are organized by electron component from core to halo to beam/strahl, in that order, sorted by the time stamp (UTC) of the observed VDF (very first column).  The first column in each set of electron component groups is a numerical indicator of the fit status for that component of the ith VDF.  This is followed by 30 columns consisting of 5 sets of 6 numbers.  Each model function has six fit parameters:  $N_{s}$ [0], $V_{Ts, \parallel}$ [1],  $V_{Ts, \perp}$ [2],  $V_{os, \parallel}$ [3],  $V_{os, \perp}$ [4] (or $p_{es}$ for asymmetric self-similar model VDF), and exponent of fit (i.e., $s_{es}$, $\kappa_{es}$, or $q_{es}$).  Thus, there are six columns for each of the following for each of the three components (i.e., 18 columns for each of the following in total):  initial guess values, returned fit values, lower limit constraints, upper limit constraints, and a logical value indicating whether the ith fit value sits on the lower (-1) or upper (+1) limit or neither (0).  These columns are followed by four more containing the number of iterations necessary to find the fit values, the least chi-squared value of the fit, the degrees of freedom in the fit process, and a two-letter designator of the model fit function used (defined in the ASCII file header). FRESULTS File Description: The FRESULTS file contains the fit results used in the three-part study.  Again, the first column starts each row with the time stamp (UTC) of the observed VDF.  In the following, all parameters listed with subscript j will correspond to three columns (one for each component) except the drift velocities which only have two for $\parallel(\perp)$.  That is followed by:  $N_{p}$ (SWE), $N_{\alpha}$ (SWE), $N_{i}$ (3DP), $T_{p, j}$ (SWE), $T_{\alpha, j}$ (SWE), $T_{i, j}$ (3DP), $B_{o, j}$ (MFI), $V_{p, j}$ (SWE), $V_{\alpha, j}$ (SWE), $V_{i, j}$ (3DP), $\phi_{sc}$ (multiple instruments), $\delta R$ (3DP),  $N_{ec}$ (fit), $T_{ec, j}$ (fit), $V_{oec, j}$ (fit), $\kappa_{ec}$ (fit), $s_{es}$ (fit), $p_{es}$ (fit), $q_{es}$ (fit), reduced $\chi_{ec}^{2}$ (fit), core fit status, and repeats for the halo and beam/strahl fits.  The last four columns contain, in the following order, the total reduced chi-squared of the model fit of all components combined and fit flags (0 = worst, 10 = best) for each electron component.  Note that all possible exponents are provided for each component but only the one that is not set as a fill value corresponds to the functional form used to model that electron component (e.g., if $s_{ec}$ is the only non-fill exponent for the core, then the core was modeled as a symmetric self-similar VDF).

opencc-by-4.0May 2019View details →

zenodo44/100

Interplanetary shock data base

This interplanetary shock data base was compiled with Wind, Advanced Composition Explorer (ACE), and Deep Space Climate Observatory (DSCOVR) observations collected at the Lagrangian point L1. The list ranges from January 1995 to December 2024 with 650 events. Many shock parameters are included, such as shock impact angle, shock speed, Mach numbers, compression ratios, and IMF (interplanetary magnetic field) Bz in the upstream and downstream regions. The list also brings geomagnetic activity information such as minimum SMR values in a time interval of 2 hours after shock impact. The author intends to update this list annually. There are three files: (i) full_shock_list_2024.txt, a text file with  650 events; (ii) full_shock_params.cdf, a cdf file with detailed information about each specific shock events; and (iii) read_shock.py, a file that contains a short python routine to read information about a specific shock event. The SpacePy package (<a href="https://spacepy.github.io/spacepy.html#:~:text=SpacePy%3A%20Space%20Science%20Tools%20for,at%20the%20space%20science%20community.">https://spacepy.github.io/spacepy.html#:~:text=SpacePy%3A%20Space%20Science%20Tools%20for,at%20the%20space%20science%20community.</a>) is required to extract shock information from the cdf file. Example (shock number 142, 26 June 2000): from read_shock import read_shock_cdf read_shock_cdf(142) ------------------------------------------------------------------------------------ sn     date     UTS  UTM <a href="tel:142 2000 06 23 1226">142 2000 06 23 1226</a>  1226 Spacecraft is ac Position: X = 239.9 Re; Y =  36.7 Re; Z =  -0.7 Re Time windows Upstream:    5 to 10 minutes before shock Downstream:  5 to 10 minutes after shock Solar wind plasma and IMF                              Bx        By      Bz        Vx              Vy       Vz          N           T Upstream        5.448  -3.946  -4.568   -399.958  18.948 -14.969     6.941    99731.6 Downstream  14.317  -1.766 -16.125  -508.734  37.628 -117.578 17.429  224496.1 Computed parameters  dp1   dp2   Xdp   Xb    Xn     vs_rh    vA      cs 1.864 7.989 4.286 2.661 2.511 604.778  67.317  52.384 Minimum SMR index in the 2-hour window following shock impact:  -9.60 nT         nx      ny     nz    thxn    phiyn    thbn     vs       vfms    Ma     Ms MC    -0.323 -0.944  0.070 108.831  175.779  78.309  127.332   85.704  0.255  0.200 MX1   -0.796  0.191 -0.575 142.729  -71.590  72.348  578.268   86.195  3.681  2.874 MX2   -0.798  0.133 -0.587 142.962  -77.223  74.365  579.175   86.010  3.693  2.890 MX3   -0.798  0.107 -0.592 142.980  -79.739  75.273  578.920   85.933  3.694  2.894 VC    -0.722  0.124 -0.681 136.205  -79.682  80.717  551.670   85.556  3.720  2.927 Type cdf['SHOCK'].attrs for a description of all shock variables and parameters. More details about this list and methods for shock normal calculations can be found in: Oliveira, D. M. (2023). Interplanetary Shock Data Base. Frontiers in    Astronomy and Space Science. (Under review)

opencc-by-4.0Mar 2023View details →

zenodo40/100

Influence of He$^{++}$ and shock geometry on interplanetary shocks in the solar wind: 2D Hybrid simulations

After protons, alpha particles (He$^{++}$) are the most important ion species in the solar wind, constituting typically about 5\% of the total ion number density. Due to their different charge-to-mass ratio protons and He$^{++}$ particles are accelerated differently when they cross the electrostatic potential in a collisionless shock. This behavior can produce changes in the velocity distribution function (VDF) for both species generating anisotropy in the temperature which is considered to be the energy source for various phenomena such as ion cyclotron and mirror mode waves. How these changes in temperature anisotropy and shock structure depend on the percentage of He$^{++}$ particles and the geometry of the shock is not completely understood. In this paper we have performed various 2D local hybrid simulations (particle ions, massless fluid electrons) with similar characteristics (e.g., Mach number) to interplanetary shocks for both quasi-parallel and quasi-perpendicular geometries self-consistently including different percentages of He$^{++}$ particles. We have found changes in the shock transition behavior as well as in the temperature anisotropy as functions of both the shock geometry and He$^{++}$ particle abundance: The change of the initial $\theta_{Bn}$ leads to variations of the efficiency with which particles can escape to the upstream region facilitating or not the formation of compressive structures in the magnetic field  that will produce increments in perpendicular temperature. The regions where both temperature anisotropy and compressive fluctuations appear tend to be more extended and reach higher values as the He$^{++}$ content in the simulations increases.

opencc-by-4.0Mar 2020View details →

zenodo36/100

Supplement to: Electron energy partition across interplanetary shocks: III. Analysis

Quick Summary: The PDF file herein provides additional example superposed epoch analysis (SEA) plots in addition to reference tables of the upstream values used to normalize the SEA data in this file and those in the paper this supplement supports.  This is a supplement to Part 3 of a three-part study of the electron velocity distribution functions (VDFs) observed near interplanetary (IP) shocks by the Wind spacecraft.  Paper I [<a href="https://iopscience.iop.org/article/10.3847/1538-4365/ab22bd">Wilson et al., 2019a</a>] introduced the methodology and data products [<a href="https://doi.org/10.5281/zenodo.2875806">Wilson et al., 2019c</a>] for fitting the electron VDFs to the sum of three model functions.  Paper II [<a href="https://iopscience.iop.org/article/10.3847/1538-4365/ab5445">Wilson et al., 2019b</a>] presents the statistics of the fit parameters produced and provided in the data products from Paper I.  Paper III presents and summarizes the analysis of the fit parameters.  The papers share the title Electron energy partition across interplanetary shocks. Wind Spacecraft: The Wind spacecraft (<a href="http://wind.nasa.gov/">https://wind.nasa.gov</a>) was launched on November 1, 1994 and currently orbits the first Lagrange point between the Earth and sun.  It holds a suite of instruments from gamma ray detectors to quasi-static magnetic field instruments, Bo.  The instruments used in this study and these datasets are the fluxgate magnetometer (<a href="https://doi.org/10.1007/BF00751330">MFI</a>), the radio receivers (<a href="https://doi.org/10.1007/BF00751331">WAVES</a>), ion Faraday cups (<a href="https://doi.org/10.1007/BF00751326">SWE</a>), and the electron and ion electrostatic analyzers (<a href="https://doi.org/10.1007/BF00751328">3DP</a>).  The MFI measures 3-vector Bo at ~11 samples per second (sps); the SWE measures reduced VDFs of the thermal proton and alpha-particle populations from which velocity moments are derived and used herein; WAVES observes electromagnetic radiation from ~4 kHz to >12 MHz which provides an observation of the upper hybrid line (also called the plasma line) used to define the total electron density; and 3DP observes full 4π steradian VDFs of electrons and ions from a few eV to ~30 keV which provide both ion velocity moments and the electron VDFs modeled herein. PDF Supplement Description: Definitions: <ul> <li>VDF = velocity distribution function</li> <li>Electron Components/Populations [taken from <a href="https://iopscience.iop.org/article/10.3847/1538-4365/ab22bd">Wilson et al., 2019a</a>,<a href="https://iopscience.iop.org/article/10.3847/1538-4365/ab5445">b</a>] <ul> <li>Core (s = ec):  cold, dense population with energies $E_{ec} \lesssim \text{15 eV}$</li> <li>Halo (s = eh):  hot, tenuous population with energies $E_{eh} \gtrsim \text{20 eV}$</li> <li>Beam/Strahl (s = eb):  anti-sunward propagating, magnetic field-aligned beam (or strahl) with $E_{eb} \sim \text{a few tens of eV}$</li> <li>Effective (s = eff):  effective total electron population, i.e., used for approximate moments rather than integrating entire VDF</li> </ul> </li> <li>Ion Components/Populations [taken from <a href="https://iopscience.iop.org/article/10.3847/1538-4365/ab22bd">Wilson et al., 2019a</a>,<a href="https://iopscience.iop.org/article/10.3847/1538-4365/ab5445">b</a>] <ul> <li>Proton (s = p):  core solar wind proton beam, i.e., main proton population streaming away from sun</li> <li>Alpha-particles (s = $\alpha$):  alpha-particle magnetic field-aligned beam</li> </ul> </li> <li>$k_{B}$ = the Boltzmann constant [J K-1]</li> <li>$\mu_{o}$ = permeability of free space [T m A-1]</li> <li>$n_{s}$= number density of species s [cm-3] (s = ec for core, eh for halo, eb for beam/strahl, p for proton, etc.)</li> <li>$B_{o, j}$= jth component (GSE coordinate basis) of quasi-static magnetic field vector [nT]</li> <li>$V_{Ts, j}$ = jth component (relative to Bo) of thermal speed of species s [km/s] <ul> <li>$V_{Ts, j} = \sqrt{ \tfrac{ 2 \ k_{B} \ T_{s, j} }{ m_{s} }}$, where $T_{s, j}$ is the jth component (relative to Bo) of the temperature of species s [eV]</li> </ul> </li> <li>$V_{os, j}$ = jth component (relative to Bo) of drift speed of species s [km/s] in ion rest frame</li> <li>$V_{s, j}$ = jth component (GSE coordinate basis) bulk velocity of species s [km/s] in spacecraft frame</li> <li>$T_{s, tot} = {1 \over 3} (T_{s, \parallel} + 2 \ T_{s, \perp})$, where $\parallel(\perp)$ is the parallel(perpendicular) component relative to Bo</li> <li>$P_{s, j} = n_{s} \ k_{B} \ T_{s, j}$ = partial thermal pressure [eV cm-3] of the jth component of species s</li> <li>$P_{t, j} = \sum_{s} \ P_{s, j}$ = total thermal pressure [eV cm-3] of the jth component summed over all species including ions</li> <li>$\mathcal{A}_{s} = \left(\tfrac{ T_{\perp} }{ T_{\parallel} } \right)_{s}$ = temperature anisotropy [N/A] of species s</li> <li>$\xi_{s, j} = \tfrac{1}{2} m_{s} \ n_{s} \ V_{os, j}^{2}$ = ram energy density [eV cm-3] jth component of species s</li> <li>$\epsilon_{j} = \tfrac{ B_{o}^{2} }{ 2 \ \mu_{o} } + \sum_{s} \left[ P_{s, j} + \xi_{s, j} \right]$ = total energy density [eV cm-3] of the jth component of the system in the plasma bulk flow rest frame</li> <li>$\zeta_{s, j} = \tfrac{ \xi_{s, j} }{ \epsilon_{j} }$ = ratio of the ram energy density of the jth component of species s to the total energy density [N/A]</li> <li>$\psi_{s, j} = \tfrac{ P_{s, j} }{ \epsilon_{j} }$ = ratio of the thermal energy density of the jth component of species s to the total energy density [N/A]</li> <li>$\Pi_{s, j} = \tfrac{ P_{s, j} }{ P_{t, j} }$ = ratio of the partial thermal pressure of the jth component of species s to the total thermal pressure [N/A]</li> <li>$s_{es}$ = exponent for the symmetric self-similar model VDF of species s</li> <li>$\kappa_{es}$ = kappa value for the bi-kappa VDF of species s</li> <li>$p_{es}(q_{es})$ = parallel(perpendicular) exponent for the asymmetric self-similar model VDF of species s</li> <li>$n_{eff} = \sum_{s} \ n_{s}$ = effective number density of all electron populations</li> <li>$T_{eff, j} = \tfrac{ \sum_{s} \ n_{s} \ T_{s, j} }{ n_{eff} }$ = effective temperature of the jth component of all electrons populations</li> <li>$\beta_{s, j} = \tfrac{ 2 \ \mu_{o} \ n_{s} \ k_{B} \ T_{s, j} }{ B_{o}^{2} }$ = plasma beta [N/A] of the jth component of species s</li> </ul>   This PDF supplement contains the following SEA plots: <ul> <li>$T_{s, j}$ vs $\Delta$t (for s = ec, eh, and eb and j = $\parallel \text{ or } \perp \text{ or tot}$)</li> <li>$\mathcal{A}_{s}$ vs  $\Delta$t (for s = ec, eh, and eb)</li> <li>$\left( \tfrac{ T_{s} }{ T_{eff} } \right)_{j}$ vs  $\Delta$t (for s = ec, eh, and eb and j = $\parallel \text{ or } \perp \text{ or tot}$)</li> <li> $\psi_{s, j}$ vs  $\Delta$t (for s = ec, eh, eb, p, and $\alpha$ and j = $\parallel \text{ or } \perp \text{ or tot}$) </li> <li> $\Pi_{s, j}$ vs  $\Delta$t (for s = ec, eh, eb, p, and $\alpha$ and j = $\parallel \text{ or } \perp \text{ or tot}$) </li> </ul> The PDF supplement contains tables of upstream median values for each shock used for normalizing the SEA plots, where the parameters listed include: <ul> <li>$T_{s, j}$ (for s = ec, eh, and eb and j = $\parallel \text{ or } \perp \text{ or tot}$)</li> <li>$n_{s}$ (for s = ec, eh, eb, and eff and j = $\parallel \text{ or } \perp \text{ or tot}$)</li> <li>$\tfrac{ n_{s} }{ n_{eff} }$ (for s = ec, eh, and eb and j = $\parallel \text{ or } \perp \text{ or tot}$)</li> <li>$\beta_{s, j}$ (for s = ec, eh, and eb and j = $\parallel \text{ or } \perp \text{ or tot}$)</li> <li>$s_{ec}\text{, }\kappa_{eh}\text{, and }\kappa_{eb}$</li> <li>$\mathcal{A}_{s}$ (for s = ec, eh, eb, and eff)</li> <li>$\left( \tfrac{ T_{s} }{ T_{eff} } \right)_{j}$ (for s = ec, eh, and eb and j = $\parallel \text{ or } \perp \text{ or tot}$)</li> </ul>

opencc-by-4.0Jan 2020View details →

zenodo36/100

Multi-Spacecraft Cycle 25 Interplanetary Shock List

This dataset contains a list of interplenatary shocks observed by multiple spacecraft in conjunction with multi-spacecraft SEP events reported by WP2 during the SERPENTINE project. Please find documentation below <a href="https://data.serpentine-h2020.eu/static/doc/Shock_Cycle25_Documentation.pdf">https://data.serpentine-h2020.eu/static/doc/Shock_Cycle25_Documentation.pdf</a> Please refer to the SERPENTINE data centre for the latest (and best) version of the catalog. <a href="https://data.serpentine-h2020.eu/catalogs/shock-sc25/">https://data.serpentine-h2020.eu/catalogs/shock-sc25/</a>

opencc-by-4.0Jun 2024View details →

zenodo36/100

Solar Orbiter Cycle 25 Interplanetary Shock List

This dataset contains a list of interplenatary shocks observed by Solar Orbiter during solar cycle 25. The catalog has been built as follows in the SERPENTINE project. <a href="https://data.serpentine-h2020.eu/static/doc/Shock_Cycle25_Documentation.pdf">https://data.serpentine-h2020.eu/static/doc/Shock_Cycle25_Documentation.pdf</a> Please refer to the SERPENTINE data centre for the latest (and best) version of the catalog. <a href="https://data.serpentine-h2020.eu/catalogs/shock-sc25/">https://data.serpentine-h2020.eu/catalogs/shock-sc25/</a>

opencc-by-4.0Jun 2024View details →

zenodo36/100

Effects of Energetic Electron and Proton Precipitations on Thermospheric Nitric Oxide Cooling during shock-led Interplanetary Coronal Mass Ejections

Satellite measurements have revealed significant enhancement of 5.3-µm nitric oxide (NO) emission during shock-led interplanetary coronal mass ejections (ICMEs). Great discrepancies in modeled neutral density occur during these events, and may be attributed to the abnormally high NO cooling. Meanwhile, the relative significance of protons, soft electrons, and keV-electrons to NO emission is yet to be well determined. The goal of this study is to identify the contribution of electron and proton precipitations to the thermospheric NO cooling by using the Defense Meteorological Satellite Program (DMSP) data. The observed energetic electrons and protons (0.1–30.2 keV) during 36 shock-led ICME events in 2002–2010 are binned into geomagnetic grids to provide statistical distributions of the particle precipitation for polar regions. The distributions are incorporated into the Global Ionosphere-Thermosphere Model. The results show that electrons play a dominant role to NO cooling, but protons are also important and contribute to up to a quarter of NO cooling by electrons and ions combined. NO cooling enhancement during the events is proportional to the level of energy flux and is dominated by the electrons in the energy band of 1.4–3.1 keV. Both total electron content (TEC) and NO cooling enhance at the source regions, but they have different lifetime and correlation with the particle precipitations. Generally, NO cooling and TEC enhancements have a positive correlation with the precipitating energy. Cross correlation shows that particle precipitations have more direct and instantaneous impact on TEC while it takes longer for the atmosphere to heat up for cooling to proceed.

opencc-by-4.0Sep 2019View details →

nasa20/100

OMNI, Combined Solar Wind Plasma Moments and Interplanetary Magnetic Field (IMF) Time-Shifted to the Nose of the Earth's Bow Shock, plus Geomagnetic Indices, 5 min Data

Near-Earth Heliospheric Data, OMNI, Definitive Multispacecraft Interplanetary Parameters Data, 5 min averagedAdditional information for all parameters are available from OMNI Data Documentation: https://omniweb..sci.gsfc.nasa.gov/html/HROdocum.htmlNew data may be accesible via the Space Physics Data Facility, SPDF, OMNIWeb Service: https://omniweb.gsfc.nasa.gov/ow_min.htmlThe Modified (Level-3) High Resolution OMNI data files are made in the same format as the OMNI files based on SWE Key Parameter data. There are a few differences between old and new high resolution OMNI data sets:* 1) In the newly modified Level-3 OMNI data files, we used the Wind SWE plasma definitive data rather than the Wind SWE plasma KP-despiked data. Using the definitive data give us possibility to include the Alpha/Proton Density Ratio and to use more accurate plasma parameters. However, the time coverage in the new OMNI data was decreased by from 2% to 10%. See the data description at https://spdf.gsfc.nasa.gov/pub/data/omni/high_res_omni/modified/. For detail comparison 1 min SWE definitive and cross-normalized SWE Key Parameter data sets, see https://omniweb.gsfc.nasa.gov/ftpbrowser/wind_pla_def_kp_norm.html.* 2) To keep the number of words and the record lengths the same as in the old OMNI high resolution data set, we replaced the PCN Index (word #45) in the ASCII records with the new Alpha/Proton Density Ratio parameter.* 3) The latest date for these new data is usually behind of the OMNI based on SWE_KP data.Modifications:* 1) Conversion to ISTP/IACG CDFs via SKTEditor, February 2000* 2) Time tags in CDAWeb version were modified to use the CDAWeb convention of having mid-average time tags rather than OMNI original convention of start-of-average time tags, March 2005

restrictednotspecifiedApr 2025View details →

nasa20/100

OMNI, Combined Solar Wind Plasma Moments and Interplanetary Magnetic Field (IMF) Time-Shifted to the Nose of the Earth's Bow Shock, plus Geomagnetic Indices, 1 min Data

Near-Earth Heliospheric Data, OMNI, Definitive Multispacecraft Interplanetary Parameters Data, 1 min averagedAdditional information for all parameters are available from OMNI Data Documentation: https://omniweb..sci.gsfc.nasa.gov/html/HROdocum.htmlNew data may be accesible via the Space Physics Data Facility, SPDF, OMNIWeb Service: https://omniweb.gsfc.nasa.gov/ow_min.htmlThe Modified (Level-3) High Resolution OMNI data files are made in the same format as the OMNI files based on SWE Key Parameter data. There are a few differences between old and new high resolution OMNI data sets:* 1) In the newly modified Level-3 OMNI data files, we used the Wind SWE plasma definitive data rather than the Wind SWE plasma KP-despiked data. Using the definitive data give us possibility to include the Alpha/Proton Density Ratio and to use more accurate plasma parameters. However, the time coverage in the new OMNI data was decreased by from 2% to 10%. See the data description at https://spdf.gsfc.nasa.gov/pub/data/omni/high_res_omni/modified/. For detail comparison 1 min SWE definitive and cross-normalized SWE Key Parameter data sets, see https://omniweb.gsfc.nasa.gov/ftpbrowser/wind_pla_def_kp_norm.html.* 2) To keep the number of words and the record lengths the same as in the old OMNI high resolution data set, we replaced the PCN Index (word #45) in the ASCII records with the new Alpha/Proton Density Ratio parameter.* 3) The latest date for these new data is usually behind of the OMNI based on SWE_KP data.Modifications:* 1) Conversion to ISTP/IACG CDFs via SKTEditor, February 2000* 2) Time tags in CDAWeb version were modified to use the CDAWeb convention of having mid-average time tags rather than OMNI original convention of start-of-average time tags, March 2005

restrictednotspecifiedApr 2025View details →

zenodo12/100

Interplanetary shock data base

This interplanetary shock data base was compiled with Wind and Advanced Composition Explorer (ACE) observations collected at the Lagrangian point L1. The list ranges from January 1995 to December 2022. Many shock parameters are included, such as shock impact angle, shock speed, Mach numbers, compression ratios, and IMF (interplanetary magnetic field) Bz in the upstream and downstream regions. More details about this list and methods for shock normal calculations can be found in:   Oliveira, D. M. (2023a). A database of interplanetary shocks observed by Wind and ACE at the Lagrangian point L1. Frontiers in    Astronomy and Space Science. (Under review)

restrictedMar 2023View details →

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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.

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neuroscienceopenDocumentation, web resources, and API references are available online.

Last verified 2026-04-30Open record

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.

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behavioral-neuroscienceopenThe DataShare record exposes download links for annotations, documentation, license text, and the zipped per-snippet data directory.

Last verified 2026-04-30Open record

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.

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electrophysiologyopenPublished Dandiset metadata and archive endpoints are available through the production DANDI API.

Last verified 2026-04-30Open record

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.

ibl

behavioral-neuroscienceopenPublic sessions can be searched and loaded from the IBL public data server through ONE.

Last verified 2026-04-29Open record

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.

openneuro

neuroscienceopenPublished datasets are available on demand over the internet.

Last verified 2026-04-29Open record