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691 results for “magnetic field”
Yellowknife (YKC) Ground-based Vector Magnetic Field (L2) 1.0 s Data
Yellowknife, NT, Ground-based Vector Magnetic Field Level 2 Data, 1.0 s Time Resolution, Station Code: (YKC), Station Location: (GEO Latitude 62.5, Longitude 245.5), GSCan Network
Val-d'Or (VLDR) Ground-based Vector Magnetic Field (L2) 0.5 s Data
Val-d'Or, QC, Ground-based Vector Magnetic Field Level 2 Data, 0.5 s Time Resolution, Station Code: (VLDR), Station Location: (GEO Latitude 48.2, Longitude 282.2), Athabasca University Network
Stellar models used in the paper "An efficient tidal dissipation mechanism via stellar magnetic fields"
<p>Data for stellar models used in the paper "An efficient tidal dissipation mechanism via stellar magnetic fields" (2024). </p> <p> </p> <p>We used MESA version r22.11.1 for these calculations.</p>
Transcriptome profiles of differentiated mouse embryonic stem cells cultured in normal condition and static magnetic field condition by RNA-seq analysisanalysis
GEO Series GSE206413. Mus musculus. 6 samples. Type: Expression profiling by high throughput sequencing.
Effects of magnetite nanoparticles and static magnetic field on neural differentiation of pluripotent stem cells
GEO Series GSE190686. Homo sapiens. 6 samples. Type: Expression profiling by high throughput sequencing.
ULY JUP MAGNETIC FIELD JOVIGRAPHIC SYS III LH COORDS 60 AVGS
The data set covers the period Jan 25 through Feb 18, 1992 (days 25 to 48 inclusive).
RENU2 Science Magnetometer (FGM) Magnetic Field, High Time Resolution (H0), 1 ms Data
Rocket Experiment for Neutral Upwelling 2, RENU2, Science Magnetometer, Magnetic Field Measurements
Transcriptome sequencing of hippocampal tissue of APP/PS1 mice treated with rotating magnetic field for 12 months
GEO Series GSE269222. Mus musculus. 11 samples. Type: Expression profiling by high throughput sequencing.
Static Magnetic Fields Regulate T-Type Calcium Ion Channels and Mediate Mesenchymal Stem Cells Proliferation
GEO Series GSE210518. Mus musculus. 2 samples. Type: Expression profiling by high throughput sequencing.
Non-invasive electric magnetic fields: Effects on keratinocyte migration and proliferation
GEO Series GSE11181. Homo sapiens. 2 samples. Type: Expression profiling by array.
PENGUIn-2 (PG2) Ground-based Vector Magnetic Field (L2) 1.0 s Data
PENGUIn-2, Antarctica, Ground-based Vector Magnetic Field Level 2 Data, 1.0 s Time Resolution, Station Code: (PG2), Station Location: (GEO Latitude -84.4, Longitude 58.0), Antarctic Network
Yellowknife (YKNF) Ground-based Vector Magnetic Field (L2) 0.5 s Data
Yellowknife, NT, Ground-based Vector Magnetic Field Level 2 Data, 0.5 s Time Resolution, Station Code: (YKNF), Station Location: (GEO Latitude 62.5, Longitude 245.7), THEMIS GBO/UCLA Network
MMS 1 Digital Signal Processor (DSP) Search Coil Magnetometer (SCM), Magnetic Field Power Spectral Density, Level 2 (L2), Fast Mode, 2 s Data
The MMS magnetic field power spectral density (BPSD) is computed onboard by the Digital Signal Processor (DSP). The fast Fourier transform (FFT) calculation is performed on a digitized version of analog signals from the Search Coil Magnetometer (SCM) in the SCM123 coordinate system, see SCM data product guide for details, https://lasp.colorado.edu/mms/sdc/public/datasets/fields/. This data product is computed in space from individual components that are not synchronized to the 1 second pulse. Therefore, the timing between channels can be inaccurate by a fraction of a second. The samples times are interval start times taken from the x component. The spectra are calculated via a 1024-point FFT algorithm on piecewise continuous sets of waveform data. Nine signals can be processed simultaneously. Six of the twelve DC-coupled E, DC-coupled V, or SCM signals (16384 samples/s) are selected for spectral processing at 100% duty cycle. In addition, the three AC-coupled signals (262,144 kS/s) each can be processed at 6.25% duty cycle. Each of the nine signals has 16, 1024-point FFT operations every second; the field-programmable gate array (FPGA) performs 144 FFTs per second. The FFT is performed by an arithmetic logic unit (ALU), which is controlled by a state machine. Both are hard-coded into the FPGA. The operation starts by applying a 1024-point Hanning window onto a waveform. Next, an FFT is implemented. The FFT is broken into a series of "butterfly" operations performed by the ALU. The result has real and imaginary data. Power spectra are calculated by taking the sum of squares of real and imaginary values (the ALU includes a multiplier), which produces a power spectrum with 512 frequency bins. The frequency bins are then combined to give pseudo-logarithmic frequency spacing (del f)/f. The spectra are reduced to 88 frequency bins with (del f)/f between 6% and 12% when possible. Narrow-band emissions can be fit to an accuracy of (del f)/f ~3%, allowing for an accurate determination of plasma density. The spectra can be averaged in time. The fastest reporting rate of any signal is 16 spectra per second. Reporting rates can be as slow a one spectra every 16 s (averaging 256 spectra). The DSP and SCM instrument papers can be found at https://link.springer.com/article/10.1007/s11214-014-0115-x and https://link.springer.com/article/10.1007/s11214-014-0096-9, respectively. The DSP and SCM data product guides can be found at https://lasp.colorado.edu/mms/sdc/public/datasets/fields/.
Dikson (DIK) Ground-based Vector Magnetic Field (L2) 1.0 min Data
Dikson, Russia, Ground-based Vector Magnetic Field Level 2 Data, 1.0 min Time Resolution, Station Code: (DIK), Station Location: (GEO Latitude 73.5, Longitude 80.7), AARI Network
Longyearbyen (LYR) Ground-based Vector Magnetic Field (L2) 1.0 min Data
Longyearbyen, Norway, Ground-based Vector Magnetic Field Level 2 Data, 1.0 min Time Resolution, Station Code: (LYR), Station Location: (GEO Latitude 78.2, Longitude 15.8), TGO Network
Dead Horse (DED) Ground-based Vector Magnetic Field (L2) 1.0 s Data
Dead Horse, AK, Ground-based Vector Magnetic Field Level 2 Data, 1.0 s Time Resolution, Station Code: (DED), Station Location: (GEO Latitude 70.4, Longitude 211.2), USGS Network
Voyager 2 1.92-s Averaged Triaxial Fluxgate Magnetometer (MAG) Interplanetary Magnetic Field in CDF Format
This data set includes the Voyager spacecraft number (1 or 2), the date-time in decimal year (90.00000 is day 1 of 1990), the magnetic field strength, F1, computed from high-resolution magnitudes, the elevation and azimuth angles in heliographic (RTN) coordinates, and the magnetic field strength, F2, computed from 1-hr averages of the components. The vector components of B can be computed from F2 and the two angles. The elevation angle is the latitude angle above or below the solar equatorial plane, and the azimuth angle is in the direction orbital motion around the Sun from the projection of the Sun-to-spacecraft axis into the solar equatorial plane. The Voyager MAG experiment and coordinates are further described in the following publication: Behannon, K.W., M.H. Acuna, L.F. Burlaga, R.P. Lepping, N.F. Ness, and F.M. Neubauer, Magnetic-Field Experiment for Voyager-1 and Voyager-2, Space Sci. Rev., 21 (3), 235-257, 1977. At the time of experiment proposal, it was expected that the required accuracy of the measurements would be 0.1 nT, determined by the combined noise of the sensors and the spacecraft field. The spacecraft magnetic field at the outboard magnetic field sensor, referred to as the primary unit, was expected to be 0.2 nT and highly variable, consistent with current estimates. Hence, the dual magnetometer design (Ness et al., 1971, 1973; Behannon et al., 1977). At distances > 40 AU, the heliospheric magnetic fields are generally much weaker than 0.4 nT; the average magnetic field strength near 40 AU and 85 AU is about 0.15 nT and 0.05 nT, respectively. The use of roll calibrations lasting about 6 hours permits determination of the effective zero levels for the two independent magnetic axes that are perpendicular to the roll axis, which is nearly parallel to the radius vector to the Sun, at intervals of about 3 months. There is no roll calibration for the third magnetic axis. Comparison of the two derived magnetic vectors from the two magnetometers permits validation of the primary magnetometer data with an accuracy of 0.02 to 0.05 nT. A discussion of the uncertainties that must be considered when using these data is given in the Appendix of Burlaga et al. (1994) and in Appendix A of Burlaga et al. (2002). References: Behannon, K.W., M.H. Acuna, L.F. Burlaga, R.P. Lepping, N.F. Ness, and F.M. Neubauer, Magnetic-Field Experiment for Voyager-1 and Voyager-2, Space Science Reviews, 21 (3), 235-257, 1977. Burlaga, L.F., Merged interaction regions and large-scale magnetic field fluctuations during 1991 - Voyager-2 observations, J. Geophys. Res., 99 (A10), 19341-19350, 1994. Burlaga, L.F., N.F. Ness, Y.-M. Wang, and N.R. Sheeley, Jr., Heliospheric magnetic field strength and polarity from 1 to 81 AU during the ascending phase of solar cycle 23, J. Geophys. Res., 107 (A11), 1410, 2002. Ness, N., K.W. Behannon, R. Lepping, and K.H. Schatten, J. Geophys. Res., 76, 3564, 1971. Ness et al., 1973. Coordinate Systems: Interplanetary magnetic field studies make use of two important coordinate systems, the Heliographic Inertial (HGI) coordinate system and the Heliographic (HG) coordinate system. The HGI coordinate system is used to define the spacecraft's position. The HGI system is defined with its origin at the Sun. There are three orthogonal axes, X(HGI), Y(HGI), and Z(HGI). The Z(HGI) axis points northward along the Sun's spin axis. The X(HGI)-Y(HGI) plane lays in the solar equatorial plane. The intersection of the solar equatorial plane with the ecliptic plane defines a line, the longitude of the ascending node, which is taken to be the X(HGI) axis. The X(HGI) axis drifts slowly with time, approximately one degree per 72 years. The magnetic field orientation is defined in relation to the spacecraft. Drawing a line from the Sun's center (HGI origin) to the spacecraft defines the X axis of the HG coordinate system. The HG coordinate system is defined with its origin centered at the spacecraft. Three orthogonal axes are defined, X(HG), Y(HG), and Z(HG). The X(HG) axis points radially away from the Sun and the Y(HG) axis is parallel to the solar equatorial plane and therefore parallel to the X(HGI)-Y(HGI) plane as well. The Z(HG) axis is chosen to complete the orthonormal triad. An excellent reference guide with diagrams explaining the HGI and HG systems may be found in L.F. Burlaga, MHD Processes in the Outer Heliosphere, Space Sci. Rev., 39, 255-316, 1984.
DE 1 Plasma Wave Instrument (PWI) Low Frequency Correlator Electric and Magnetic Field Spectral Density
Two Dynamics Explorer (DE) spacecraft were launched August 3, 1981, and placed into coplanar polar orbits with DE-1 in a highly elliptical orbit and DE-2 in a lower more circular orbit. The primary objective of the DE program was to investigate magnetosphere-ionosphere-atmosphere coupling processes. The DE mission provided a wealth of new information on a wide variety of magnetospheric plasma wave phenomena including auroral kilometric radiation, auroral hiss, Z mode radiation, narrow-band electromagnetic emissions associated with equatorial upper hybrid waves, whistler mode emissions, wave-particle interactions stimulated by ground VLF transmitters, equatorial ion cyclotron emissions, ion Bernstein mode emissions, and electric field turbulence along the auroral field lines. These files contain calibrated, full resolution, data from the DE-1 Plasma Wave Instrument (PWI). This instrument was designed and built by the plasma wave group at The University of Iowa, Department of Physics and Astronomy, in collaboration with investigators at Stanford University's STAR Laboratory. It measured plasma wave phenomena and quasi-static electric fields using paired combinations of five PWI sensors: a 200m tip-to-tip long wire electric antenna deployed in the spacecraft spin plane, a 9m tip-to-tip tubular electric antenna deployed along the spacecraft spin axis, a short 0.6m electric antenna, mounted on the boom and oriented parallel to the long wire antenna, a magnetic loop antenna mounted on the boom and oriented to measure the component of the magnetic field parallel to the long wire antenna, and a magnetic search coil antenna, also mounted on a boom and oriented to measure the magnetic field parallel to the spacecraft spin axis. The PWI main electronics unit consisted of a Step Frequency Correlator (SFC), a Low Frequency Correlator (LFC), a Wideband Analog Receiver (WBR) and a Linear Wave Receiver (LWR). Only the LFC data are included in these files. The SFC data were provided in a companion fileset. A dataset containing available high rate WBR LWR data may be provided in future archive products. The LFC consisted of two receivers (LFR-A and LFR-B) with 8 analog channels each. The analog channels were centered at 1.78, 3.12, 5.62, 10.0, 17.8, 31.2, 56.2 and 100 Hz. Each channel's band-edge was at +/-15% of the center value. Each LFR in the LFC could be connected to either the Ex, Es, Ez, or H antenna during an 8 second major frame. In addition, the Low Frequency Correlator provided in-phase and quadrature-phase correlations of signals from any selected antenna pair. Phase data are not provided in this file set.
Baranov (BRN) Ground-based Vector Magnetic Field (L2) 1.0 min Data
Baranov, Russia, Ground-based Vector Magnetic Field Level 2 Data, 1.0 min Time Resolution, Station Code: (BRN), Station Location: (GEO Latitude 47.8, Longitude 132.4), AARI Network
IMP 8 MAG 15.36s Magnetic Field Measurements
IMP 8 magnetic field measurements from tri-axis magnetometer. Time resolution is 15.36 second. Data are based on a 2010 data reprocessing by the PI team. Parameter details below are based on the version of the data in CDAWeb.
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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.
Annotated Behaviour and Observability Dataset (ABODe)
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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.