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Stochastic star formation and spiral structure

Published online by Cambridge University Press:  04 August 2017

Philip E. Seiden
Philip E. Seiden*
Affiliation:
IBM Thomas J. Watson Research Center Yorktown Heights, New York 10598

Extract

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Most approaches to explaining the long-range order of the spiral arms in galaxies assume that it is induced by the long-range gravitational interaction. However, it is well-known in many fields of physics that long-range order may be induced by short-range interactions. A typical example is magnetism, where the exchange interaction between magnetic spins has a range of only 10 ångströms, yet a bar magnet can be made as large as one likes. Stochastic self-propagating star formation (SSPSF) starts from the point of view of a short-range interaction and examines the spiral structure arising from it (Seiden and Gerola 1982). We assume that the energetic processes of massive stars, stellar winds, ionization-front shocks and supernova shocks, in an OB association or open cluster can induce the creation of a new molecular cloud from cold interstellar atomic hydrogen. In turn this new molecular cloud will begin to form stars that will allow the process to repeat, creating a chain reaction. The differential rotation existing in a spiral galaxy will stretch the aggregation of recently created stars into spiral features.

Type
PART III: Dynamics and Evolution
Information
Symposium - International Astronomical Union , Volume 106: The Milky Way Galaxy , 1985 , pp. 551 - 558
Copyright
Copyright © Reidel 1985 

References

Baker, P.L., and Burton, W.B.: 1975, Astrophys. J. 198, p. 281.Google Scholar
Burton, W.B., and Gordon, M.A.: 1978, Astron. and Astrophys. 63, p. 7.Google Scholar
Chromey, F.R.: 1978, Astron. J. 83, p. 162.Google Scholar
de Vaucouleurs, G., and Pence, W.D.: 1978, Astron. J. 83, p. 1163.CrossRefGoogle Scholar
Freeman, K.C.: 1970, Astrophys. J. 160, p. 811.CrossRefGoogle Scholar
Kulkarni, S.R., Blitz, L., and Heiles, C.: 1982, Astrophys. J. 259, p. L63.Google Scholar
Seiden, P.E.: 1983, Astrophys. J. 266, p. 555.CrossRefGoogle Scholar
Seiden, P.E., and Gerola, H.: 1982, Fund. Cosmic Phys. 7, p. 241.Google Scholar
Seiden, P.E., Schulman, L.S., and Elmegreen, D.B.: 1984, Astrophys. J. (to be published).Google Scholar
Schulman, L.S., and Seiden, P.E.: 1982, J. Stat. Phys. 27, p. 83.Google Scholar
Stark, A.A.: 1983, in “Kinematics, Dynamics and Structure of the Milky Way”, Shuter, W.L.H. (ed.), Reidel, p. 127.CrossRefGoogle Scholar
van der Kruit, P.C., and Searle, L.: 1982, Astron. Astrophys. 95, p. 105.Google Scholar
Young, J.S., and Scoville, N.: 1982, Astrophys. J. 258, p. 467.CrossRefGoogle Scholar