Convection in the solar atmosphere

Details Convection in the solar atmosphere Convection in the solar atmosphere

Nov 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981s%26w....20..405d&link_type=abstract

Sterne und Weltraum, vol. 20, Nov. 1981, p. 405-408. In German.

Physics

Convective Heat Transfer, Photosphere, Solar Atmosphere, Absorption Spectra, Doppler Effect, Solar Granulation, Solar Interior, Solar Spectra

Scientific paper

Convection, in addition to radiation, plays an important role in the processes involved in the transportation of energy from the solar interior to the solar surface. The solar convection zone begins directly below the photosphere and, extending into the solar interior, covers approximately one-third of the solar radius. An investigation of the convection zone is only possible for its upper boundary layer. Of particular interest in this area is the granulation phenomenon. The dynamics of the solar photosphere are discussed. The velocity field can be studied with the aid of the Doppler shift. Attention is given to the extension of the area in which the transport of heat takes place as consequence of motions in the photosphere. Two spectral areas are used in an investigation conducted to obtain values regarding the intensity of large structures. Measurements of the Doppler shift were also carried out. The obtained results show that the brightness and velocity variations of the lowest photospheric layers are of convective origin.

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