CA II K2V spectral features and their relation to small-scale photospheric magnetic fields

Details CA II K2V spectral features and their relation to small-scale photospheric magnetic fields CA II K2V spectral features and their relation to small-scale photospheric magnetic fields

Oct 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982soph...80..227s&link_type=abstract

Solar Physics, vol. 80, Oct. 1982, p. 227-231.

Physics

59

K Lines, Photosphere, Solar Magnetic Field, Solar Spectra, Calcium, Magnetic Signatures

Scientific paper

While the Ca II K-232 network is known to be cospatial with magnetic elements, there has been doubt regarding the magnetic origin of the fainter K(2V) points. It is shown that weak magnetic elements also lie at the roots of the K(2V) points and, because the latter are numerous, that they may contribute significantly to the integrated light profile of Ca II K. The observations used were obtained at the vacuum tower telescope of the Kitt Peak National Observatory in May 1980 and March 1981. It is now established that there is a one-to-one correspondence between bright points and the discrete magnetic structures in the interior of the network. When taken together with the observation that a bright point shifts to occupy the new location of its associated magnetic point (perhaps displaced by horizontal flows) and so maintains a one-to-one correlation, this leads to the conclusion that the presence of the magnetic field is probably an essential precondition that decides the location of the bright point within the network. If these bright points represent regions of upward propagation of energy (Liu, 1974) it is thought logical to infer that this energy propagation is guided by the magnetic fields in the magnetic structure associated with the bright point.

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