The fine structure of solar granulation and its relationship to large-scale photospheric structures

Details The fine structure of solar granulation and its relationship to large-scale photospheric structures The fine structure of solar granulation and its relationship to large-scale photospheric structures

May 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...272..580a&link_type=abstract

Astronomy and Astrophysics, Vol. 272, p. 580 (1993)

Astronomy and Astrophysics

Astrophysics

6

Sun: Granulation, High Resolution, Mesogranulation

Scientific paper

The structure of brightness and vertical velocities in fine-structure details of the solar photo sphere are studied using the results of two-dimensional photometry of spectrograms (λλ5020-5060 Å) and direct photographs of the granulation (λ4600±200Å) with high spatial resolution, 0".6 and 0".25, respectively.
The vertical velocity (Vrms = 430 m s-1) and its correlation with continuum intensity fluctuations (ΔIrms=4.3%) increase with increasing absolute values of contrast. The statistically non-homogeneous spatial distribution of granules, intergranular lanes and large granular clusters into mesogranular cells (average scale of 6-9") which is accompanied by an enhanced rise of matter is noted. The generation of mesogranules and granules is considered to be a result of overshooting of convective cells into convectively stable levels. A qualitative model of buoyancy of giant convective cells is proposed. These cells reaching the ionization zones (double and single) of He and H are unstable and consecutively split into separate intercorrelating convective cells of granular, mesogranular and supergranular scales.

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