Hydrogen line and continuum emission in young stellar objects. I - Excitation model

Details Hydrogen line and continuum emission in young stellar objects. I - Excitation model Hydrogen line and continuum emission in young stellar objects. I - Excitation model

Jul 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...330..870k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 330, July 15, 1988, p. 870-896. NASA-supported research.

Astronomy and Astrophysics

Astrophysics

14

Early Stars, Pre-Main Sequence Stars, Stellar Radiation, Balmer Series, Continuous Radiation, Cooling, Heating, Hydrogen, Lyman Spectra, Photoionization, Radiative Transfer, Spectral Energy Distribution, Stellar Models

Scientific paper

Two mechanisms that populate the n = 2 level of hydrogen after the Lyman continuum is depleted are identified. They are ionization of N I from its excited states, followed by charge-exchange between N II and H I, and Ly-beta line wing absorption. Both processes involve absorption of the sub-Lyman continuum between 11 and 13.6 eV. With population in level n = 2 thus maintained, the strong Brackett line fluxes observed are then produced as a result of Balmer photoionization. The magnitude of the sub-Lyman continuum dictates the fraction of Balmer continuum that will be absorbed. Numerical calculations for four young stellar objects with luminosity ranging from 10 to 10,000 solar are performed, and it is concluded that this two-step process of sub-Lyman continuum absorption followed by Balmer photoionization can account for the great majority of observed Brackett line fluxes. The location and mass of the emitting as as determined from the Brackett line fluxes are reported. The Br-alpha luminosity is calculated as a function of the mass loss rate.

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