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Jackvik (JCK) Ground-based Vector Magnetic Field (L2) 1.0 min Data

Jackvik, Sweden, Ground-based Vector Magnetic Field Level 2 Data, 1.0 min Time Resolution, Station Code: (JCK), Station Location: (GEO Latitude 66.4, Longitude 17.0), TGO Network

Uummannaq (UMQ) Ground-based Vector Magnetic Field (L2) 1.0 min Data

Uummannaq, Greenland, Ground-based Vector Magnetic Field Level 2 Data, 1.0 min Time Resolution, Station Code: (UMQ), Station Location: (GEO Latitude 70.7, Longitude 307.9), DTU Network

Honolulu (HON) Ground-based Vector Magnetic Field (L2) 1.0 s Data

Honolulu (Ewa Beach), HI, Ground-based Vector Magnetic Field Level 2 Data, 1.0 s Time Resolution, Station Code: (HON), Station Location: (GEO Latitude 21.3, Longitude 202.0), USGS Network

Tartu (TAR) Ground-based Vector Magnetic Field (L2) 10.0 s Data

Tartu, Estonia, Ground-based Vector Magnetic Field Level 2 Data, 10.0 s Time Resolution, Station Code: (TAR), Station Location: (GEO Latitude 58.3, Longitude 26.5), IMAGE Network

Clyde River (CRVR/CRV) Ground-based Vector Magnetic Field (L2) 0.5 s Data

Clyde River, NU, Ground-based Vector Magnetic Field Level 2 Data, 0.5 s Time Resolution, Station Code: (CRVR/CRV), Station Location: (GEO Latitude 70.5, Longitude 291.4), MACCS Network

CNOFS VEFI 1-sec Magnetic Field preliminary data

This data set contains magnetic field data from the fluxgate magnetometer associated with the C/NOFS Vector Electric Field Instrument (VEFI). The data include 1-sec resolution magnetic field components (North, West, Up) and spacecraft positions. As of 5/13/2010, the data were preliminary.

Lovozero (LOZ) Ground-based Vector Magnetic Field (L2) 1.0 min Data

Lovozero, Russia, Ground-based Vector Magnetic Field Level 2 Data, 1.0 min Time Resolution, Station Code: (LOZ), Station Location: (GEO Latitude 68.0, Longitude 35.0), AARI Network

Voyager 1 48-s Triaxial Fluxgate Magnetometer (MAG) Magnetic Field Data 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 (degrees) in heliographic (RTN) coordinates, and the magnetic field strength, F2, computed from hour 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 of 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 Science Reviews, 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) was adopted. 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 radial 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 use 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. Magnetic field orientation is defined in relation to the spacecraft. Drawing a line from the Sun's center, the 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 too. 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 and Science Reviews, 39, 255-316. Support data calib_flag_on, calib_flag_MF, and calib_flag_offset are added to file version 2. Variable calib_flag_on consists of points where bit 4 or 5 in variable magStatus equal 1. Variable calib_flag_MF represents observations where magnetometer was in cailbration mode. Variable calib_flag_offset represent delay between data points when the magnetometer was in calibration mode and data points where magStatus variable indicated calibration periods. Due to specific shape of magnetometer data profile variable calibration_flag_

Whitehorse (WHS) Ground-based Vector Magnetic Field (L2) 1.0 s Data

Whitehorse, YT, Ground-based Vector Magnetic Field Level 2 Data, 1.0 s Time Resolution, Station Code: (WHS), Station Location: (GEO Latitude 60.7, Longitude 224.9), STEP Polar Network

Voyager 2 9.6-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.

STEREO-A In-Situ Measurements of Particles and CME Transients (IMPACT) Fluxgate Magnetometer (MAG) Magnetic Field Vectors, in Radial-Tangential-Normal (RTN) Coordinates, Level Beacon (LB), PT0.125S Data

STEREO Ahead reprocessed IMPACT/MAG Beacon magnetic field vector component and vector magnitude data expressed in Heliographic, HG, Radial-Tangential-Normal, RTN, Cartesian coordinates around the 2015 solar conjunction. * Version 1: Used internally at UCB and UCLA ONLY, No corrections applied to raw MAG data * Version 2: Offset correction applied to MAG data * Version 3: Initial algorithm for correcting glitches for the X sensor on STEREO Ahead applied * Version 4: Improvement in glitch correction algorithm applied * Version 5: Further refinement of the glitch correction for the X sensor on STEREO Ahead, Also, two timing issues resolved: - a) applying a 6 ms time shift to account for time lag between IMPACT IDPU and MAG - b) fixing an occasional 1 s 'glitch' * Version 6: Added FILTER_VALUE variable

Tristan Da Cunha (TDC) Ground-based Vector Magnetic Field (L2) 1.0 min Data

Tristan Da Cunha, Ground-based Vector Magnetic Field Level 2 Data, 1.0 min Time Resolution, Station Code: (TDC), Station Location: (GEO Latitude -37.1, Longitude 347.7), DTU Network

Kangerlussuaq (STF) Ground-based Vector Magnetic Field (L2) 1.0 min Data

Kangerlussuaq, Greenland, Ground-based Vector Magnetic Field Level 2 Data, 1.0 min Time Resolution, Station Code: (STF), Station Location: (GEO Latitude 67.0, Longitude 309.3), DTU Network

Wind Magnetic Field Investigation (MFI) Solar Wind Experiment (SWE) 1-min field and plasma data at bow shock nose

Solar wind magnetic field and plasma data at 1-min resolution created from Wind data shifted to the Earth's bow shock nose (BSN).

Wind Magnetic Field Investigation (MFI) Composite Data in RTN Coordinates

Wind MFI composite data in RTN coordinates. The files contain multiple time resolution data: 3-second, 1-minute, and 1-hour. Final Version 5 data are accessible to within about 3 months of current date, newly defined Version 4 data (with final Bz offsets and not-yet-final spacecraft position vectors) between 3 months and about 2 weeks of current date, and newly defined Version 3 data (with the most recently determined Bz offset value, not yet final for the Version 3 interval) from 2 weeks to about 2 days of current.

Daneborg (DNB) Ground-based Vector Magnetic Field (L2) 20.0 s Data

Daneborg, Greenland, Ground-based Vector Magnetic Field Level 2 Data, 20.0 s Time Resolution, Station Code: (DNB), Station Location: (GEO Latitude 74.3, Longitude 339.8), DTU Network

Summit (SUM) Ground-based Vector Magnetic Field (L2) 1.0 min Data

Summit, Greenland, Ground-based Vector Magnetic Field Level 2 Data, 1.0 min Time Resolution, Station Code: (SUM), Station Location: (GEO Latitude 72.3, Longitude 321.7), Norwegian Mag. Network

Nordkapp (NOR) Ground-based Vector Magnetic Field (L2) 1.0 min Data

Nordkapp, Norway, Ground-based Vector Magnetic Field Level 2 Data, 1.0 min Time Resolution, Station Code: (NOR), Station Location: (GEO Latitude 71.1, Longitude 25.8), TGO Network

STEREO-A In-situ Measurements of Particles And CME Transients (IMPACT) Magnetic Field Vectors and Ancillary Data

This data product contains Level 1 0.125-s values of solar wind magnetic field data taken by the IMPACT/Magnetometer on STEREO-A. The interface at UCB provides access to CDF-formatted files of magnetic field data in RTN coordinates. The interface at UCLA allows selection of STEREO A or STEREO B data and of vector quantities in RTN or spacecraft coordinates. It also allows selection of either of two parameter sets: [Bx, By, Bz, B ] or [RBx, RBy, RBz, B , cone and clock angles]. Further, this interface enables easy migration between plot vs. ASCII data presentation options and among the three available resolutions (1, 8, 32 Hz). The parameter level information given below is specific to tyhe CDF version of the data at UCB.

Wallops Island (WLPS) Ground-based Vector Magnetic Field (L2) 0.5 s Data

Wallops Island, VA, Ground-based Vector Magnetic Field Level 2 Data, 0.5 s Time Resolution, Station Code: (WLPS), Station Location: (GEO Latitude 37.9, Longitude 284.6), THEMIS GBO Network