Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998a%26a...340..203t&link_type=abstract
Astronomy and Astrophysics, v.340, p.203-215 (1998)
Astronomy and Astrophysics
Astrophysics
1
Hydrodynamics, Methods: Numerical, Stars: Coronae, Stars: Mass Loss
Scientific paper
A grid of 74 coronal models with parameterized heating distribution, representing a wide range of physical parameters, has been calculated. We find that three of these models reproduce the recent observations made by Hara et al. (\cite{hara:tsun}) with the soft X-ray telescope aboard the Japanese satellite Yohkoh, which indicate a temperature of 1.8 ~ 2.4 x es 10(6) { K with an emission measure of 10(25.5) to 10(26.2) cm^{-5}, while other solutions reproduce the more standard Yohkoh and Skylab observations, which have a temperature of about 1.4 x es 10(6) { K The best fit for the coronal temperature and emission measure gives a velocity at the Earth's orbit of only 10 {km s^{-1}. A model including acceleration by Alfven waves gives a final velocity of 630 km s^{-1} which is in agreement with the observations. The mechanical heating flux at the transition region is 2.1 x es 10(5) ergcms with a weighted average dissipation scale length of 0.1 R_{\odot}. The flux of Alfven waves is 1 x es 10(5) ergcms . In our models the velocity of the solar wind from coronal holes is completely determined by the Alfven wave acceleration, in contrast to previous models in which the Alfven wave acceleration increased the velocity of the purely thermal model only by a factor 2. Observations of the non thermal broadening of the coronal red and green lines are consistent with this model.
Hearn A. G.
Martens Petrus C. H.
Tziotziou Kostas
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