Dynamics of the solar granulation. V. The intergranular space.

Details Dynamics of the solar granulation. V. The intergranular space. Dynamics of the solar granulation. V. The intergranular space.

Jun 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996a%26a...310..973n&link_type=abstract

Astronomy and Astrophysics, v.310, p.973-981

Astronomy and Astrophysics

Astrophysics

9

Sun: Photosphere, Sun: Granulation

Scientific paper

This investigation is based on a spectrogram of extraordinary spatial resolution selected from a series of 80 spectrograms taken with the vacuum tower telescope at Izana (Tenerife) in May 1994. The wavelength range was λλ: 491.00-491.40nm and includes both magnetically sensitive and insensitive spectral lines. The spectrograph slit intersected parts of the border and interior of CaII network cells, thus permitting a comparative study of the granular dynamics at varying, but moderate, levels of magnetic activity. As diagnostic tools we use the Doppler shift variation of line cores, which is associated with spatially resolved velocity structures, and the line broadening variation, which is a signature of unresolved velocity fluctuations. We discuss in particular the granular dynamics and the intermittency of the line broadening within the intergranular space as functions of height and position relative to network cells. Our results suggest that the magnetic field in the network is not only located preferentially in the intergranular space, but furthermore coincides with regions of enhanced line broadening. We confirm that the Doppler shift variation is reduced in regions of enhanced magnetic field, but we find that this reduction affects the entire range of granular scales. The slopes of the velocity power spectra are independent of the magnetic activity level. This result is surprising, since on the basis of classical MHD turbulence theory one would have expected shallower power spectra in magnetically active regions. The line broadening variation is much less sensitive to the magnetic field than the line shift variation.

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