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Astronomy & Astrophysics manuscript no. 0666 February 3, 2004 (DOI: will be inserted by hand later)

Summary: Astronomy & Astrophysics manuscript no. 0666 February 3, 2004
(DOI: will be inserted by hand later)
Signature of oscillations in coronal bright points
I. Ugarte-Urra1, J. G. Doyle1, M. S. Madjarska1,2, and E. O'Shea3
Armagh Observatory, College Hill, Armagh BT61 9DG, N. Ireland
Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey RH5 6NT, UK
Instituto de Astrof┤isica de Canarias, C/ v┤ia L┤actea s/n, 38200 La Laguna, Tenerife, The Canary Islands, Spain
Received / Accepted
Abstract. A detailed study of two consecutive bright points observed simultaneously with the Coronal Diagnostic Spectrometer
(CDS), the Extreme ultraviolet Imaging Telescope (EIT) and the Michelson Doppler Imager (MDI) onboard the Solar and
Heliospheric Observatory (SOHO) is presented. The analysis of the evolution of the photospheric magnetic features and their
coronal counterpart shows that there is a linear dependence between the EIT Fe XII 195 ┼ flux and the total magnetic flux of
the photospheric bipolarity. The appearance of the coronal emission is associated with the emergence of new magnetic flux
and the disappearance of coronal emission is associated with the cancellation of one of the polarities. In one of the cases the
disappearance takes place 3-4 hours before the full cancellation of the weakest polarity.
The spectral data obtained with CDS show that one of the bright points experienced short time variations in the flux on a time
scale of 420-650 seconds, correlated in the transition region lines (O V 629.73 ┼ and O III 599.60 ┼) and also the He I 584.34 ┼


Source: Armagh Observatory


Collections: Physics