Theoretical spectra of circumstellar dust shells around carbon-rich asymptotic giant branch stars

Details Theoretical spectra of circumstellar dust shells around carbon-rich asymptotic giant branch stars Theoretical spectra of circumstellar dust shells around carbon-rich asymptotic giant branch stars

Aug 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...288..255w&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 288, no. 1, p. 255-272

Astronomy and Astrophysics

Astrophysics

60

Asymptotic Giant Branch Stars, Carbon Stars, Stellar Envelopes, Stellar Luminosity, Stellar Mass, Stellar Spectra, Stellar Temperature, Stellar Winds, Abundance, Dust, Hydrodynamics, Mass Flow Rate, Radiative Transfer, Stellar Models, Temperature Distribution

Scientific paper

Realistic modeling of circumstellar dust shells around evolved stars has to include a physical treatment of the interaction among hydrodynamics, thermodynamics, radiative transfer, chemistry and dust formation and -growth. A self-consistent solution of this problem is presented in the case of stationary, spherical symmetric dust-driven winds. The resulting shell structure and the mass-loss rate are completely determined by the three fundamental stellar parameters stellar mass M(stellar), stellar luminosity L(stellar) and effective temperature Teff and by the element abundances epsiloni. A detailed calculation of the transport coefficients of the dust component by means of the particle size distribution function and the solution of the non-grey radiative transfer problem provide realistic synthetic spectra of the dust shell models. We discuss the dependence of the resulting spectra on the stellar parameters in terms of infrared two color diagrams. Application of these model calculations to the prominent infrared object IRC +10216 yields best agreement with the observed spectrum and the visibility data at maximum light for the stellar parameters M(stellar) = 0.7 solar mass, L(stellar) = 2.4 x 104 solar luminosity, T(stellar) = 2010K and a carbon to oxygen ratio of epsilonc/epsilono = 1.40, which corresponds to a mass-loss rate of M-dot = 8 x 10-5 solar mass/yr. In this model only amorphous carbon grains are considered as the main opacity source. From this model a distance to IRC +10216 of d = 170pc is deduced. The total mass contained in the circumstellar dust shell implies and initial main sequence mass of MZAMS greater than or = 1.3 solar mass for IRC +10216.

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