Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999esasp.446..417l&link_type=abstract
8th SOHO Workshop: Plasma Dynamics and Diagnostics in the Solar Transition Region and Corona. Proceedings of the Conference hel
Astronomy and Astrophysics
Astrophysics
Scientific paper
More than two decades after coronal holes (CH) had been recognized to be the source regions of solar wind, we still do not know which structures, within CH, most contribute to the solar wind mass flux. In a recent work, Hassler et al. (1999) obtained velocity maps of a coronal hole region, in the Ne VIII 770 Angstrom line, which suggest that localized areas within the network might be sources of the solar wind. On the opposite, an earlier work of Dupree et al. (1996), from an analysis of the He I 10830 Angstrom line, suggested cell regions as sources of the solar wind. In the present work, we reinvestigate this issue analysing SUMER data taken in an equatorial and in a polar coronal hole, observed respectively on 29 August 1996 and 21 September 1996. We study the behavior of Si II, C IV, O V, N V, Ne VIII, Mg X and Fe XII ions, whose temperatures of formation range from chromospheric (around 2x104 K) to coronal values (around 1.5x105 K). In particular, we analysed intensity and velocity distributions of these lines, and illustrate changes in the plasma velocity pattern as a function of the temperature regime where lines form.
Landi Enrico
Mullan Dermott
Poletto Giannina
Wilhelm Klaus
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