Accession Number:

AD0261089

Title:

THE STELLAR WIND REGIONS

Descriptive Note:

Corporate Author:

CHICAGO UNIV ILL ENRICO FERMI INST FOR NUCLEAR STUDIES

Personal Author(s):

Report Date:

1960-11-01

Pagination or Media Count:

1.0

Abstract:

WITH CLASS G main sequence and M-giant stars are given for various interst llar environments. The supersonic wind from a class G star undergoes a shock transition to subsonic flow at a radial distance of 100 - 1,000 a.u. and may extend many times farther as a subsonic flow. Thic storms. Open-ended Terms Stellar Wind. From the observations of the solar wind and of the M-giant alpha-Herculis the gross dynamical features of the stellar wind region associated with class G main sequence and M-giant stars are given for various interst llar environments. The supersonic wind from a class G star undergoes a shock transition to subsonic flow at a radial distance of 100 - 1,000 a.u. and may extend many times farther as a subsonic flow. This subsonic flow will be subject to turbulence and oth r instabilities in many cases. The wind from an Mgiant may extend many parsecs if the M-giant p ase of evolution lasts long enough for its wind to approach equilibrium the resultant in erstellar contamination and heating is important for a distance of many parsecs. A rough calculation of the cavity formed by a stellar wind in a largescale interstellar field is carried out, and it is found that the cavity shape and dimensions for stationary flow depend upon the back pressure at infinity. As the pressure increases, the cavity changes from a circular cylinder of infinite radius, through an increa ingly bulbous shape of finite radius, to a sphere of infinite radius with one finite cyli drical channel from each pole. Author

Subject Categories:

Distribution Statement:

APPROVED FOR PUBLIC RELEASE