CRITICAL METALLICITY FOR POPULATION II STARS

Автор(и)

  • E. O. Vasiliev Institute of Physics, Southern Federal University, Rostov-on-Don 344090 Russia, ; Institute of Astronomy, Russian Academy of Sciences, Moscow 119017 Russia, Russian Federation
  • Yu. A. Shchekinov Department of Physics, Southern Federal University, Rostov-on-Don 344090 Russia; Special Astrophysical Observatory, Nizhnij Arkhyz, Karachai-Cherkess Republic 369167 Russia, Russian Federation

DOI:

https://doi.org/10.18524/1810-4215.2008.21.86882

Ключові слова:

early universe, shock waves, mixing, heavy elements, supernovae, stars (Population III, Population II).

Анотація

We present simple arguments about metallicity of transition from first stellar generation (population III) to the second one. We consider the efficiency of fragmentation in gas induced by thermal instability in cold gas layers and filaments (T < 104 K), and in the shells formed by supernovae explosions from first stars. We estimate the metallicity at which the gas behind shock waves becomes unstable against thermal instability. We argue that this metallicity is inherited by population II stars and can be thus treated as the critical metallicity.

Посилання

Bromm V., Ferrara A., Coppi P .S., Larson R.B.: 2001, MNRAS, 328, 969.

Glover S.C.O.: 2008, AIP Conf. Proc., 990, 25.

Field G.B.: 1965, ApJ, 142, 531.

Omukai K., Tsuribe T., Schneider R., Ferrara A.: 2005, ApJ, 626, 627.

Vasiliev E., Dedikov S., Shchekinov Yu.: in press.

Smith B., Sigurdsson S., Abel T.: 2008, MNRAS, 385, 1443.

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Опубліковано

2008-12-20

Номер

Том 21 (2008)

Розділ

Статті

Ліцензія

Авторське право (c) 2016 Odessa Astronomical Publications

Creative Commons License

Ця робота ліцензується відповідно до Creative Commons Attribution-NonCommercial 4.0 International License.

Відповідно Закону України про авторське право і суміжні права N 3792-XII від 23 грудня 1993 року