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Physical Conditions and Heating/Cooling Processes in High Mass Star Formation Regions

  • Chapter
The Physics of Star Formation and Early Stellar Evolution

Part of the book series: NATO ASI Series ((ASIC,volume 342))

Abstract

Massive stars have a profound impact on their environment. At a distance of a few pc from a massive O-star (> 106 L⨀) the flux of UV photons is about 1000 times larger than in the average radiation field of the solar neighborhood. Massive stars also have supersonic winds with velocities up to several thousand km s−1 carrying between 0.1 and 1% of the star’s luminosity in form of kinetic energy. Massive stars affect their environment very soon after a stellar core has formed as their thermal (Kelvin-Helmholtz) time scale is very short compared to all other time scales (τKH ≤ 104y for an O-star). At the end of its lifetime (several 106 to 107 y) an O star explodes as a supernova, ejecting 1051 erg of energy into its surroundings.

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  1. Max-Planck-Institut für extraterrestrische Physik, Garching, Germany

    Reinhard Genzel

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  1. Smithsonian Astrophysical Observatory, Cambridge, MA, USA

    Charles J. Lada

  2. Department of Physics, University of Crete, Heraklion, Crete, Greece

    Nikolaos D. Kylafis

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Genzel, R. (1991). Physical Conditions and Heating/Cooling Processes in High Mass Star Formation Regions. In: Lada, C.J., Kylafis, N.D. (eds) The Physics of Star Formation and Early Stellar Evolution. NATO ASI Series, vol 342. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-3642-6_5

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