Ionizing Photon Emission Rates from O- and Early B-Type Stars and Clusters

By A. Sternberg, Tadziu Hoffman, A. Pauldrach. 2003

158 citations recorded by the source corpus.

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.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/77dbab5dccb9cf76c855e67bd22bd6a4f165f1bd

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In Astronomy and Astrophysics

1. R. Genzel
2. T. Alexander
3. P. Hopkins
4. Roger Davies
5. F. Eisenhauer
6. L. Hernquist
7. O. Gerhard
8. L. Tacconi

Citations in the corpus

• THE WISE CATALOG OF GALACTIC H ii REGIONS (2013, methodology): “For the calculation of the ionizing flux we used Sternberg et al. (2003) and for the conversion from ionizing flux to 21 cm luminosity we used the relation given in Rubin (1968).”
• The Star-forming Torus and Stellar Dynamical Black Hole Mass in the Seyfert 1 Nucleus of NGC 3227 (2006, methodology): “The data were generated using the population synthesis code STARS (Sternberg 1998; Thornley et al. 2000; Davies et al. 2003; Sternberg et al. 2003; Davies et al. 2005), which calculates the distributions of stars in the Hertzsprung-Russell diagram as a function of age for exponentially decaying…”
• Massive Perturber-driven Interactions between Stars and a Massive Black Hole (2006, methodology): “We assume star formation at a constant rate for 10 Gyr with a Miller-Scalo IMF (Miller & Scalo 1979), and use a stellar population synthesis code (Sternberg et al. 2003) with the Geneva stellar evolution tracks (Schaller etal.”
• [Si II], [Fe II], [C II], and H2 Emission from Massive Star-forming Regions (2006, result): “We have compared our standard cluster spectrum with the atmosphere calculations presented in Sternberg et al. (2003) and find that it is similar in overall shape and strength of breaks to stars with TeA 40;000 K and surface gravity g ¼ 104 cm s 2.”
• A Massive Cluster of Red Supergiants at the Base of the Scutum-Crux Arm (2007, background): “As the far-side distance would imply an extraordinarily massive cluster of 8 O3 stars (e.g., Sternberg et al. 2003), and as no obvious central cluster is seen, the nearside distance seems more likely.”
• AN EXTREMELY TOP-HEAVY INITIAL MASS FUNCTION IN THE GALACTIC CENTER STELLAR DISKS (2009, methodology): “We computed these models using the population synthesis code STARS (Sternberg 1998; Sternberg et al. 2003) assuming solar metallicity Geneva tracks, for a cluster age of 6 Myr, and an exponentially decaying star burst with an 1/e time-scale of 1 Myr.”
• THE GREEN BANK TELESCOPE H ii REGION DISCOVERY SURVEY. II. THE SOURCE CATALOG (2011, methodology): “5 calculated by Sternberg et al. (2003), we convert the Equation 2 Nly values into ionizing star spectral types.”
• A LIBRARY OF THEORETICAL ULTRAVIOLET SPECTRA OF MASSIVE, HOT STARS FOR EVOLUTIONARY SYNTHESIS (2010, methodology): “These values work in favor of an interstellar contribution in Si iv and a stellar contribution in C iv and N v. Smith et al. (2002) and Sternberg et al. (2003) published grids of ionizing fluxes for hot, massive stars using WM-Basic models, however without the inclusion of X-rays.”
• A Close Look at Star Formation around Active Galactic Nuclei (2007, methodology): “We model these observational diagnostics using the stellar population and spectral synthesis code STARS (e.g., Sternberg 1998; Sternberg et al. 2003; Förster Schreiber et al. 2003; Davies et al. 2003, 2005).”