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Simulation of the gravitational collapse and fragmentation of rotating molecular clouds
Репозиторій DSpace/Manakin
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Simulation of the gravitational collapse and fragmentation of rotating molecular clouds
Тема:
MS3: Physics of Stars and Galaxies
Посилання:
Simulation of the gravitational collapse and fragmentation of rotating molecular clouds / P. Berczik, M.I. Petrov // Кинематика и физика небесных тел. — 2005. — Т. 21, № 5-додаток. — С. 216-223. — Бібліогр.: 27 назв. — англ.
Підтримка:
P. B. wish to express his thanks for the support of his work to the German Science Foundation (DFG) under the grant SFB-439 (sub-project B5). P. B.’s work was also supported by the following grants: NNG04GJ48G from NASA, AST-0420920 from NSF and by HST-AR-09519.01-A from STScI. He is very grateful for the hospitality to the Astronomisches Rechen-Institut (Heidelberg, Germany) where a part of this work has been done. The research work of the authors was also supported by the Ukrainian State Fund of Fundamental Investigations within the framework of the project 02.07.00132. The calculation has been performed with the Mitaka Underground Vineyard (MUV) GRAPE6 system of the National Astronomical Observatory of Japan. The authors want to express their special thanks to colleague Naohito Nakasato (Computational Astrophysics Group, RIKEN) for his permanent help and support in handling of the NAOJ GRAPE6 computational facilities. The authors are also very grateful to Dan Batcheldor (Astrophysics Group, RIT) for his constructive comments to the first variant of the paper.
Дата:
2005
Переглядів:
744
Завантажень:
665
Анотація:
In this paper we study the process of the subsequent (runaway) fragmentation of a rotating isothermal Giant Molecular Cloud (GMC) complex. Our own Smoothed Particle Hydrodynamics (SPH) gas-dynamical model successfully reproduces the observed Cloud Mass-distribution Function (CMF) in our Galaxy (even the differences between the inner and outer parts of our Galaxy). The steady state of CMF is established during the collapse within a free-fall timescale of the GMC. We show that one of the key parameters, which defines the observed slope of the present day CMF, is the initial ratio of the rotational (turbulent) and gravitational energy inside the fragmented GMC.
