Other
Scientific paper
Dec 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...181.1907m&link_type=abstract
American Astronomical Society, 181st AAS Meeting, #19.07; Bulletin of the American Astronomical Society, Vol. 24, p.1151
Other
Scientific paper
Recently the continuous energy distribution from the infrared to the radio region has been obtained for six Be stars, three of which are Be stars and three of which are shell stars. Analysis of these continuous energy distributions by Waters et al. (1991) in terms of a disk model has yielded the density distribution and the radial component of velocity in the circumstellar material. In this paper we determine the additional force, F_x(r), exclusive of those arising from gravity, rotation, and the gas pressure gradient, which is required in this disk model to produce the radial component of velocity for each of the stars studied. We find that F_x(r) for the three Be stars and the three shell stars has the same behavior. Between the surface of the star and the turning point F_x(r) decreases with increasing r but a little less rapidly than does gravity. Beyond the turning point F_x(r) increases dramatically with r. We show that the normalized F_x(r) has several characteristic properties: a) between 2-3 stellar radii and the turning point the normalized F_x(r) is essentially identical for the six stars, b) beyond the turning point F_x(r) increases with increasing distance, but the rate of increase depends on the star considered, and c) Be stars as a group may have the turning point closer to the surface of the star than do shell stars. The first property suggests the same mechanism is responsible for driving the wind inside the turning point for Be stars and shell stars. The second property suggests that either a second driving mechanism takes over from the first or a change in physical conditions leading to an increase in F_x(r) takes place which is different from one star to another. The third characteristic, if real, suggests that the increase in F_x(r) occurs at smaller r for Be stars than for shell stars. This latter result, if real, suggests that some shell stars have envelopes which are more extended than those of Be stars.
Chen Haiqi
Marlborough J. M.
Waters Laurens B. F. M.
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