A generalized method for deriving mass-loss rates - The first order moment of unsaturated P Cygni line profiles

Details A generalized method for deriving mass-loss rates - The first order moment of unsaturated P Cygni line profiles A generalized method for deriving mass-loss rates - The first order moment of unsaturated P Cygni line profiles

Feb 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983ap%26ss..90..299s&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 90, no. 2, Feb. 1983, p. 299-311.

Astronomy and Astrophysics

Astrophysics

9

B Stars, Line Spectra, Stellar Envelopes, Stellar Mass Ejection, Stellar Motions, Stellar Spectra, Numerical Integration, Optical Thickness, Radial Velocity

Scientific paper

For the case of optically thin lines, we show that the relation existing between the first order moment W1 ~ j (E(2)/E~ - 1)(2 - 212) d2 of a P Cygni profile and the quantity ii~in(1eve1), where M is the mass-loss rate of the central star and n(level) the fractional abundance of the ion under study, is in fact independent of any Sobolev-type approximations used for the transfer of line radiation, contrary to what has been assumed in some previous works (Castor eta!., 1981; Surdej, 1982). Consequently, all results established in the context of'very rapidly' expanding atmospheres and mainly referring to the non-dependence of W1 vs various physical (underlying photospheric absorption line, limb darkening, etc.) and geometrical (velocity field v(r), etc.) effects remain unchanged for arbitrary (e.g. non-Sobolev type) outward-accelerating velocity laws. Whenever applied with caution, Equation (50) thus provides a very powerful means of deriving mass-loss rates - with a total uncertainty less than 60 percent - from the measurement W1 of unsaturated P Cygni profiles observed in the spectrum of early - as well as late - type stars, quasars, etc

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