VEGA1 DUST PARTICLE IMPACT PLASMA DETECTOR DATA V1.0

공공데이터포털

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.

VEGA1 DUST PARTICLE IMPACT DETECTOR DATA V1.0

공공데이터포털

The SP-2 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.

VEGA1 DUST PARTICLE IMPACT DETECTOR DATA V1.0

공공데이터포털

The SP-2 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.

VEGA2 DUST PARTICLE IMPACT DETECTOR DATA V1.0

공공데이터포털

The SP-2 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.

VEGA2 DUST PARTICLE IMPACT DETECTOR DATA V1.0

공공데이터포털

The SP-2 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.

VEGA1 DUST PARTICLE COUNTER MASS ANALYSER DATA V1.0

공공데이터포털

Encounter Data for Vega-1 included two files: DSFAST17 and Dvega101. These files were submitted by the Univ of Chicago group with hard copy versions of the operating manual and a preprint of results. The following explanation of the contents of the two files is below.

VEGA1 DUST PARTICLE COUNTER MASS ANALYSER DATA V1.0

공공데이터포털

Encounter Data for Vega-1 included two files: DSFAST17 and Dvega101. These files were submitted by the Univ of Chicago group with hard copy versions of the operating manual and a preprint of results. The following explanation of the contents of the two files is below.

VEGA2 DUST PARTICLE IMPACT PLASMA DETECTOR DATA V1.0

공공데이터포털

A number of datasets from the VEGA missions were submitted by Dyachkov at IKI as FITS files (binary data) using the GROUPS form or multidimensioned arrays. In addition, little information was provided except for the date, spacecraft, and experiment. Sometimes in the GROUPS parameters (Pvalues), there were experiment parameters such as 'time' indicated and by inference this could be determined to be exposure time versus a clock time. Since there was at least one extensive set of observations (TVS images), that were provided by IKI in this manner and a separate facility (KFKI) with the proper IHW keywords, it was possible to make estimates as to the meaning of 'time' with proper units (seconds).

VEGA2 DUST PARTICLE IMPACT PLASMA DETECTOR DATA V1.0

공공데이터포털

A number of datasets from the VEGA missions were submitted by Dyachkov at IKI as FITS files (binary data) using the GROUPS form or multidimensioned arrays. In addition, little information was provided except for the date, spacecraft, and experiment. Sometimes in the GROUPS parameters (Pvalues), there were experiment parameters such as 'time' indicated and by inference this could be determined to be exposure time versus a clock time. Since there was at least one extensive set of observations (TVS images), that were provided by IKI in this manner and a separate facility (KFKI) with the proper IHW keywords, it was possible to make estimates as to the meaning of 'time' with proper units (seconds).

VEGA1 HALLEY FLYBY MAGNETOMETER DATA

공공데이터포털

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].