The scale of solar granulation

Details The scale of solar granulation The scale of solar granulation

Jun 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...222l..69n&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor, vol. 222, June 1, 1978, p. L69-L72.

Astronomy and Astrophysics

Astrophysics

27

Solar Atmosphere, Solar Granulation, Convective Flow, Photosphere, Radiative Heat Transfer, Solar Temperature, Stellar Models, Temperature Distribution

Scientific paper

The observed scale of granulation is derived as a consequence of a physical model. At scales smaller than granulation, horizontal radiative transport reduces temperature fluctuations and the resultant buoyancy forces in the surface layers. At scales only slightly larger than granulation, the dynamical pressure required to drive horizontal motions changes the opacity sufficiently to reduce the apparent contrast. This raises the possibility that the dark center of an exploding granule may actually be hot below the surface. The maximum possible horizontal extent of a surface-driven convective flow is estimated as 4.5 times granular scale.

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