We simulate the collapse of a primordial protostellar cloud by means of a 1D hydrodynamics code accounting for chemical evolution, radiative transfer and radiation pressure. We find that the role of radiation pressure is negligible throughout the whole simulations, i.e. until shortly after the formation of a central hydrostatic core. We also estimate the luminosity and the spectrum of such collapsing clouds. The luminosity is initially due to a number of H-2 lines and is of the order of 10(33-34) erg s(-1). It then grows to values greater than or similar to 10(36) erg s(-1) by the time the core forms, and results from both lines and continuum radiation.

Haardt, F., Ripamonti, E., Colpi, M., & Ferrara, A. (2002). The collapse of primordial stars: Importance of radiation. ASTROPHYSICS AND SPACE SCIENCE, 281(01-feb), 479-482.

The collapse of primordial stars: Importance of radiation

COLPI, MONICA;
2002

Abstract

We simulate the collapse of a primordial protostellar cloud by means of a 1D hydrodynamics code accounting for chemical evolution, radiative transfer and radiation pressure. We find that the role of radiation pressure is negligible throughout the whole simulations, i.e. until shortly after the formation of a central hydrostatic core. We also estimate the luminosity and the spectrum of such collapsing clouds. The luminosity is initially due to a number of H-2 lines and is of the order of 10(33-34) erg s(-1). It then grows to values greater than or similar to 10(36) erg s(-1) by the time the core forms, and results from both lines and continuum radiation.
No
Articolo in rivista - Articolo scientifico
Scientifica
Metal Free Stars
English
479
482
4
Haardt, F., Ripamonti, E., Colpi, M., & Ferrara, A. (2002). The collapse of primordial stars: Importance of radiation. ASTROPHYSICS AND SPACE SCIENCE, 281(01-feb), 479-482.
Haardt, F; Ripamonti, E; Colpi, M; Ferrara, A
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Utilizza questo identificativo per citare o creare un link a questo documento: http://hdl.handle.net/10281/326094
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