The vertical motion of the solar convective elements

Details The vertical motion of the solar convective elements The vertical motion of the solar convective elements

Publishing date

Jun 1990

URL

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...232..231b&link_type=abstract

Journals

Astronomy and Astrophysics (ISSN 0004-6361), vol. 232, no. 1, June 1990, p. 231-233.

Science

Astronomy and Astrophysics

Field

Astrophysics

Additional info 2

4

Additional info 3

Convection Cells, Solar Atmosphere, Solar Granulation, Temperature Gradients, Velocity Distribution, Vertical Motion

Type

Scientific paper

Abstract

The ascent velocity of the solar convective elements (cells) and its variation with depth are deduced by using a temporal evolution of the apparent radius (size) of 13 granules and a simple morphological model for calculations. An attempt is made to 'see' somewhat deeper into the unstable zone and to deduce the acceleration of the convective motion. It is assumed that granules are spherical and practically do not expand as they rise. Thus, the upward convection velocity increases with decreasing depth below tau(5000) = 1; the rms vertical velocity changes from 0.5 km/s to 1.6 km/s between -880 km and -390 km. This is compatible with a verticle mass flux conservation. The acceleration rate is approximately 4 m/s sq. Larger convective elements have higher ascent velocities. The existence of horizontal velocities at tau(5000) = 1 driven by a pressure gradient and the subsequent fall of the material can be understood as a phenomenon related to the late evolution of the cell-granule element.

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