Possibility of spectroscopic detection of oxygen in lower Venusian atmosphere

Details Possibility of spectroscopic detection of oxygen in lower Venusian atmosphere Possibility of spectroscopic detection of oxygen in lower Venusian atmosphere

Sep 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985rpspr...5...67k&link_type=abstract

In its USSR Rept.: Space (JPRS-USP-85-005) p 67-68 (SEE N86-14111 04-88) Transl. into ENGLISH from Kosmich. Issled. (Moscow),

Computer Science

Magnetic Dipoles, Magnetic Field Configurations, Mars (Planet), Planetary Magnetic Fields, Planetary Magnetospheres, Interplanetary Magnetic Fields, Mars 2 Spacecraft, Mars 3 Spacecraft, Solar Wind

Scientific paper

The parameters of the Martian magnetic dipole on the basis of measurements from the Mars-2 satellite on 23 to 24 February 1972 were discussed. Although the experimental data have deficiencies (the satellite was without triaxial orientation and the interrogation of the vehicle was infrequent) the magnetograms contain important information. This is because during the 35 hours of measurements the satellite twice reached pericenter on the daytime side and twice reached the region of the magnetic tail on the nighttime side. Simultaneously with the measurements from the Mars-2 the magnetic field was measured from the high-apogee satellite Mars-3 (with triaxial orientation) in the free solar wind. Changes in the dynamic pressure of the solar wind during the time of the measurements were simple. The combined data made it possible to determine field topology, which is compared with the field topology near Venus and a model of a draped magnetosphere corresponding to the observed interplanetary magnetic field. Proof is given that Mars has its own magnetic field with a magnetic moment MM1.5 x 10 to the 22 gauss. cubic cm, this constituting an effective obstacle to the solar wind. The strike of the magnetic tail was traced to 8 RM. The problems involved in determining orientation of the dipole on the basis of observations in the tail at distances 6 to 8 RM are discussed. On the assumption that a width of the Martian polar cap is approx. 45 deg it is estimated that the magnetic tail of the Martian magnetosphere can extend to 90 RM. The real obstacle to the solar wind near Mars is its magnetosphere, not its ionosphere. Near Mars there is an Earth-type, not a Venusian type of interaction with the solar wind.

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