On Dec 15, 1984, the Vega spacecraft was launched to first flyby Venus at which time landers were released and then continue to a flyby of Halley. The magnetic field experiments MISCHA carried four fluxgate sensors, with three sensors mounted on a boom at the end of the solar panels and the fourth sensor mounted one meter closer. During the cruise phase, the TRASSA-1 mode of the instrument (1 vector/2.5 min) was used. The sensors were switched to the TRASSA-2 mode (1 vector/min) during the flyby which started roughly two days before the encounter. From 3 h before closest approach (CA) until 1 hour after CA, the HS-mode 1 vector/6s) and the DT-mode (1 vector/100ms) was used [DELVAETAL1991].

On MARCH 6, 1986, AT 7:20:06 UT, the Vega spacecraft passed the nucleus of comet Halley at a distance of 8,890 km with a relative velocity of 78 km/s. The magnetic field experiments MISCHA carried four fluxgate sensors, with three sensors mounted on a boom at the end of the solar panels and the fourth sensor mounted one meter closer. During the cruise phase, the TRASSA-1 mode of the instrument (1 vector/2.5 min) was used. The sensors were switched to the TRASSA-2 mode (1 vector/min) during the flyby which started roughly two days before the encounter. From 3 h before closest approach (CA) until 1 hour after CA, the HS-mode (1 vector/6s) and the DT-mode (1 vector/100ms) was used [DELVAETAL1991].

This data set contains the NEAR magnetometer (MAG) data for the CRUISE1 phase. The data set begins on 1996-02-20T00:00:00.000 and ends 1997-06-24T23:59:59.999 . The data are raw telemetry data, provided in engineering units, that have been reformatted into FITS file format (NASA Office of Science and Technology (NOST), 100-1.0). In addition to the raw magnetometer data, a calibration file and algorithm are available. This data set is archived as a set of CDROM images as a part of the NEAR EDR volume set.

This data set contains the NEAR magnetometer (MAG) data for the CRUISE1 phase. The data set begins on 1996-02-20T00:00:00.000 and ends 1997-06-24T23:59:59.999 . The data are raw telemetry data, provided in engineering units, that have been reformatted into FITS file format (NASA Office of Science and Technology (NOST), 100-1.0). In addition to the raw magnetometer data, a calibration file and algorithm are available. This data set is archived as a set of CDROM images as a part of the NEAR EDR volume set.

This data set includes Voyager 1 Jupiter encounter magnetometer data that have been resampled at a 1.92 second sample rate. The data set is composed of 6 columns: 1) ctime - this column contains the data acquisition time. The time is always output in the ISO standard spacecraft event time format (yyyy-mm-dd-Thh:mm:ss.sss) but is stored internally in Cline time which is measured in seconds after 00:00:00.000 Jan 01, 1966, 2) br - this column contains the radial component of the magnetic field, 3) bphi - this column contains the phi component of the magnetic field, 4) btheta - this column contains the theta component of the magnetic field, 5) bmag - this column contains the magnitude of the magnetic field, 6) flag - a flag value that indicates either software error or spacecraft hardware interference reduced confidence in this record (flag value of 1 is bad , 0 is good or unchecked). All magnetic field observations are measured in nanoTeslas. The coordinate system for this dataset is Minus System III. All of the magnetic field data are calibrated (see the instrument calibration description for more details). The Jupiter System III coordinate system is defined in Dessler 1983 and the reference documents for this dataset are: Ness et al, 1979 Lepping et al, 1981 Connerney,Acuna,Ness, 1981 Behannon,Burlaga,Ness, 1981

This data set includes Voyager 1 Jupiter encounter magnetometer data that have been resampled at a 1.92 second sample rate. The data set is composed of 6 columns: 1) ctime - this column contains the data acquisition time. The time is always output in the ISO standard spacecraft event time format (yyyy-mm-dd-Thh:mm:ss.sss) but is stored internally in Cline time which is measured in seconds after 00:00:00.000 Jan 01, 1966, 2) br - this column contains the radial component of the magnetic field, 3) bphi - this column contains the phi component of the magnetic field, 4) btheta - this column contains the theta component of the magnetic field, 5) bmag - this column contains the magnitude of the magnetic field, 6) flag - a flag value that indicates either software error or spacecraft hardware interference reduced confidence in this record (flag value of 1 is bad , 0 is good or unchecked). All magnetic field observations are measured in nanoTeslas. The coordinate system for this dataset is Minus System III. All of the magnetic field data are calibrated (see the instrument calibration description for more details). The Jupiter System III coordinate system is defined in Dessler 1983 and the reference documents for this dataset are: Ness et al, 1979 Lepping et al, 1981 Connerney,Acuna,Ness, 1981 Behannon,Burlaga,Ness, 1981

This data set includes Voyager 1 Jupiter encounter magnetometer data that have been resampled at a 9.6 second sample rate. The data set is composed of 6 columns: 1) ctime - this column contains the data acquisition time. The time is always output in the ISO standard spacecraft event time format (yyyy-mm-dd-Thh:mm:ss.sss) but is stored internally in Cline time which is measured in seconds after 00:00:00.000 Jan 01, 1966, 2) br - this column contains the radial component of the magnetic field, 3) bphi - this column contains the phi component of the magnetic field, 4) btheta - this column contains the theta component of the magnetic field, 5) bmag - this column contains the magnitude of the magnetic field, 6) flag - a flag value that indicates either software error or spacecraft hardware interference reduced confidence in this record (flag value of 1 is bad , 0 is good or unchecked). All magnetic field observations are measured in nanoTeslas. The coordinate system for this dataset is Minus System III. All of the magnetic field data are calibrated (see the instrument calibration description for more details). The Jupiter System III coordinate system is defined in Dessler 1983 and the reference documents for this dataset are: Ness et al, 1979 Lepping et al, 1981 Connerney,Acuna,Ness, 1981 Behannon,Burlaga,Ness, 1981

This data set includes Voyager 1 Jupiter encounter magnetometer data that have been resampled at a 9.6 second sample rate. The data set is composed of 6 columns: 1) ctime - this column contains the data acquisition time. The time is always output in the ISO standard spacecraft event time format (yyyy-mm-dd-Thh:mm:ss.sss) but is stored internally in Cline time which is measured in seconds after 00:00:00.000 Jan 01, 1966, 2) br - this column contains the radial component of the magnetic field, 3) bphi - this column contains the phi component of the magnetic field, 4) btheta - this column contains the theta component of the magnetic field, 5) bmag - this column contains the magnitude of the magnetic field, 6) flag - a flag value that indicates either software error or spacecraft hardware interference reduced confidence in this record (flag value of 1 is bad , 0 is good or unchecked). All magnetic field observations are measured in nanoTeslas. The coordinate system for this dataset is Minus System III. All of the magnetic field data are calibrated (see the instrument calibration description for more details). The Jupiter System III coordinate system is defined in Dessler 1983 and the reference documents for this dataset are: Ness et al, 1979 Lepping et al, 1981 Connerney,Acuna,Ness, 1981 Behannon,Burlaga,Ness, 1981

The SP-1 experiment on Vega spacecraft was intended for studying the spatial and mass distributions of dust particles in the cometary coma over the mass range 1.e-16 to 1.e-6 g. Covering such a broad mass range was made possible by using sensors of two types, namely, impact plasma and acoustic.

The SP-1 experiment on Vega spacecraft was intended for studying the spatial and mass distributions of dust particles in the cometary coma over the mass range 1.e-16 to 1.e-6 g. Covering such a broad mass range was made possible by using sensors of two types, namely, impact plasma and acoustic.