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1. IMPLICATIONS OF PRELIMINARY VEGA BALLOON RESULTS FOR THE VENUS ATMOSPHERE DYNAMICS

Author

Blamont, Je, Sagdeev, Rz, Linkin, Vm, Kerzhanovich, Vv, David Crisp, Ingersoll, Ap, Elson, Ls, Preston, Ra, Golitsyn, Gs, Ivanov, Vn, Ragent, B., Seiff, A., and Young, Re

Abstract

The typical 1-2 m/sec vertical winds encountered by the Vega balloons probably result from thermal convection. The consistent 6.5-kelvin differential between the Vega 1 and Vega 2 temperatures is attributable to disturbances of synoptic or planetary scale. According to the Doppler tracking the winds were stronger than on earlier missions, perhaps because of solar thermal tides. The motions of Vega 2 may have been affected by waves from mountainous terrain.

3. Implications of the VEGA Balloon Results for Venus Atmospheric Dynamics.

Author

Blamont JE, Young RE, Seiff A, Ragent B, Sagdeev R, Linkin VM, Kerzhanovich VV, Ingersoll AP, Crisp D, Elson LS, Preston RA, Golitsyn GS, and Ivanov VN

Abstract

Both VEGA balloons encountered vertical winds with typical velocities of 1 to 2 meters per second. These values are consistent with those estimated from mixing length theory of thermal convection. However, small-scale temperature fluctuations for each balloon were sometimes larger than predicted. The approximate 6.5-kelvin difference in temperature consistently seen between VEGA-1 and VEGA-2 is probably due to synoptic or planetary-scale nonaxisymmetric disturbances that propagate westward with respect to the planet. There is also evidence from Doppler data for the existence of solar-fixed nonaxisymmetric motions that may be thermal tides. Surface topography may influence atmospheric motions experienced by the VEGA-2 balloon.

Published
1986
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