Astronomy and Astrophysics – Astrophysics
Scientific paper
Mar 1997
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997a%26a...319l..17m&link_type=abstract
Astronomy and Astrophysics, v.319, p.L17-L20
Astronomy and Astrophysics
Astrophysics
71
Sun: Corona, Solar Wind
Scientific paper
Wave effects in a two-fluid model for the solar corona and wind are studied. Heating and acceleration are achieved by high-frequency Alfven waves, which are assumed to be created through small-scale reconnections in the chromospheric network. The wave energy flux F_w_ is given in the model as a lower boundary condition. Waves with a power spectrum of the form P_0_(f/f_0_)^-1^ in the frequency range from 1 to 800Hz and with P_0_=40x10^11^nT^2^/Hz and f_0_=10^-5^Hz, corresponding to an integrated amplitude of 35km/s, can heat the corona to a temperature of 10^6^K at r=1.2Rsun_, and 2.6x10^6^K (the maximum) at r=2Rsun_, starting from 4x10^5^K at r=1Rsun_. Thermal and wave pressure gradients accelerate the wind to speeds of 100km/s at r=1.2Rsun_, and 212km/s at r=2Rsun_, starting from 2km/s at r=1Rsun_ in a rapidly diverging stream tube. Asymptotic wind speeds in the observed range of 700 to 800km/s at 0.3AU are obtained with wave amplitudes of 30 to 37km/s in the frequency range from 1 to 30Hz, corresponding to P_0_=90x10^11^nT^2^/Hz.
Marsch Eckart
Tu Chia-Ying
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