Line emission in stellar envelopes

Details Line emission in stellar envelopes Line emission in stellar envelopes

Apr 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997mnras.286..920m&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 286, Issue 4, pp. 920-930.

Astronomy and Astrophysics

Astronomy

3

Radiative Transfer, Stars: Atmospheres, Stars: Emission-Line, Be

Scientific paper

We examine the problem of what could be called a `compact planetary nebula' in studying the radiative equilibrium of a spherical envelope with inner radius comparable or equal to the radius of the illuminating core. The envelope is composed of hydrogen atoms in statistical equilibrium and photoionized by a central radiation of relatively high temperature T*>15 000K. We consistently solve the equations of radiative transfer in spherical geometry for all lines and continua, including the Lyman transitions, together with the equations of statistical equilibrium. Yet we ignore the energy balance equation and consider the electronic temperature as a given parameter. We show that Balmer and other subordinate lines may appear in emission, even at low temperature, provided that (i) the density is low enough for the radiative terms to partly control the populations of the levels and (ii) the geometrical extension of the H II region is significant. Although the present model is only intended to isolate and illustrate a specific physical mechanism, we suggest that the emission features detected in the spectrum of cool giant or supergiant stars could result from purely radiative processes, at least in some cases.

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