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Ionizing Photon Emission Rates from O- and Early B-type Stars and Clusters
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Ionizing Photon Emission Rates from O- and Early B-Type Stars
and Clusters
Amiel Sternberg
School of Physics and Astronomy and the Wise Observatory, The Beverly and Raymond
Sackler Faculty of Exact Sciences, Tel Aviv University, Tel Aviv 69978, Israel
Tadziu L. Hoffmann and A.W.A. Pauldrach
Institute for Astronomy and Astrophysics of the Munich University, Scheinerstra?e 1,
D-81679 Munich, Germany
ABSTRACT
We present new computations of the ionizing spectral energy distributions
(SEDs), and Lyman continuum (Lyc) and He I continuum photon emission rates,
for hot O-type and early B-type stars. We consider solar metallicity stars, with
effective temperatures ranging from 25,000 to 55,000 K, and surface gravities
(cm s?2) log g ranging from 3 to 4, covering the full range of spectral types
and luminosity classes for hot stars. We use our updated (WM-basic) code to
construct radiation-driven wind atmosphere models for hot stars. Our models
include the coupled effects of hydrodynamics and non-LTE radiative transfer in
spherically outflowing winds, including the detailed effects of metal line-blocking
and line-blanketing on the radiative transfer and energy balance. Our grid of
model atmospheres is available on the world-wide-web. We incorporate our hot-
star models into our population synthesis code (STARS), and we compute the
time-dependent SEDs, and resulting Lyc and He I emission rates, for evolving
star clusters. We present results for continuous and impulsive star-formation, for
a range of assumed stellar initial mass functions.
1. Introduction
Massive hot stars inject large amounts of energy and entropy into the interstellar medium
of galaxies, via jets, winds, radiation, and supernova explosions. The production rates of
Lyman continuum photons (Lyc; hν 13.6 eV), and of helium continuum photons (He
I; hν 24.6 eV), are particularly important and fundamental parameters of O-type and
early B-type st
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