In: Contributions of the Astronomical Observatory Skalnaté Pleso, vol. 37, no. 2
O.g. Badalyan - N.g. Bludova - J. Sýkora
Detaily:
Rok, strany: 2007, 125 - 141
O článku:
Comparisons of the Fe XIV 530.3 nm coronal emission line brightness
strength (extrapolated from the photospheric measurements to the 1.1
R☉ distance in the corona), are discussed. Different
correlations of the coronal green line brightness (CGLB) with the
large-scale coronal magnetic fields and the local fields of
sunspots are found during different solar cycle phases. At the
ascending phase of activity the large-scale coronal magnetic fields
dominate, whereas at the descending phase a somewhat higher
correlation of the CGLB with the local magnetic fields of sunspots
is observed. It is shown that within the ±40° solar
low-latitude zone a portion of the CGLB originating due to the large
scale magnetic field amounts to 25-30% in the period of solar cycle
maximum but it goes up to 85% at the cycle minimum. Impact of the
local sunspot fields on the CGLB level is remarkably lesser, it
provides only 8-10% of the CGLB during cycle maximum and increases
to about 18% at its minimum. Results of this paper could be helpful
when testifying various models of the solar corona heating.
Ako citovať:
ISO 690:
Badalyan, O., Bludova, N., Sýkora, J. 2007. Comparisons of the green-line corona brightness with the magnetic field strength and the summary sunspot area. In Contributions of the Astronomical Observatory Skalnaté Pleso, vol. 37, no.2, pp. 125-141. 1335-1842.
APA:
Badalyan, O., Bludova, N., Sýkora, J. (2007). Comparisons of the green-line corona brightness with the magnetic field strength and the summary sunspot area. Contributions of the Astronomical Observatory Skalnaté Pleso, 37(2), 125-141. 1335-1842.