The structure of solar granulation. I - Observations of the spatial and temporal behavior of vertical motions. II - Models of vertical motion

Details The structure of solar granulation. I - Observations of the spatial and temporal behavior of vertical motions. II - Models of vertical motion The structure of solar granulation. I - Observations of the spatial and temporal behavior of vertical motions. II - Models of vertical motion

May 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...237.1024k&link_type=abstract

Astrophysical Journal, Part 1, vol. 237, May 1, 1980, p. 1024-1042.

Astronomy and Astrophysics

Astrophysics

25

Atmospheric Circulation, Convective Heat Transfer, Solar Atmosphere, Solar Granulation, Solar Spectra, Atmospheric Models, Flow Velocity, Photosphere, Power Spectra, Spectroheliographs, Stellar Models, Vertical Motion

Scientific paper

The height dependence of the granular contribution to observed photospheric line shifts were deduced using a temporal sequence of spectroscopic measurements each covering a large horizontal distance on the solar disk. The deduced height variations represent the most accurate determination to date because individual granules can be isolated in both time and space simultaneously in several spectral lines. The previous attempts to deduce the height dependence, based on spectrograms having only one spatial resolution which led to conflicting pictures of the granular velocities are discussed; it is shown that a purely spatial separation of oscillatory and granular motions such as used by Mattig and Schlebbe and Durrant et al. (1979) is inadequate for determining granular velocities. Granules are predominant source of line shifts in the photosphere; much of the line-shift fluctuation power at small spatial scales in the stronger lines, which some authors incorrectly attributed to granules, results from high-frequency oscillations.

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