Metallicity Dependence of Starburst Spectra
| dc.creator | Traat, P. | |
| dc.date | 1999-05-23 | |
| dc.date.accessioned | 2026-07-07T02:31:41Z | |
| dc.date.available | 2026-07-07T02:31:41Z | |
| dc.description | We discuss on the basis of our evolutionary spectral models the impact of chemical composition on the spectrum of stellar population formed in the starburst. Their metallicity range Z=0.0001 - 0.05(0.1) fully covers the observable one; depending on age, wavelength region and IMF the UV-fluxes differ between extreme compositions at least tenfold, usually more. Independently of age, UV-fluxes shortwards of Balmer jump monotonically decline with the growth of metallicity. Optical and especially IR-region are also influenced, with the typical difference 10-50 times in fluxes at wavelengths >1 micron. In IR the situation which composition is the brightest emitter gets reversed with age. | |
| dc.description | 2 pages, LATEX, with 1 encapsulated figure. To appear in: "Wolf-Rayet Phenomena in Massive Stars and Starburst Galaxies", K.A. van der Hucht, G. Koenigsberger & P.R.J. Eenens (eds.),Proc. IAU Symp. No. 193 (San Francisco: ASP) | |
| dc.identifier | https://arxiv.org/abs/astro-ph/9905297 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/9905297 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/14242 | |
| dc.subject | Astrophysics | |
| dc.title | Metallicity Dependence of Starburst Spectra | |
| dc.type | text |