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Star formation in CHA T1

Published online by Cambridge University Press:  04 August 2017

P. R. Wesselius ,
R. Assendorp  and
H. Roede
P. R. Wesselius
Affiliation:
Space Research, P.O. Box 800, 9700 AY Groningen, The Netherlands
R. Assendorp
Affiliation:
Space Research, P.O. Box 800, 9700 AY Groningen, The Netherlands
H. Roede
Affiliation:
Space Research, P.O. Box 800, 9700 AY Groningen, The Netherlands

Abstract

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In a region of 0.4 × 0.5 pc around HD 97300 the amount of mass in gas and dust is < 16 M⊙, while the stellar mass is 6–9 M⊙. Thus in this core of a collapsing cloud (Cha T1) several stars have been formed in a very efficient way.

Type
Bipolar Flows, Jets and Protostars
Information
Symposium - International Astronomical Union , Volume 122: Circumstellar Matter , 1987 , pp. 95 - 96
Copyright
Copyright © Reidel 1987 

References

Henize, K.G., Mendoza, E.E. 1973, Astrophys. J. 180, 115.CrossRefGoogle Scholar
Hildebrand, R.H. 1983, Q. Jl. R. astr. Soc. 24, 267.Google Scholar
Hyland, A.R., Jones, T.J., Mitchell, R.M. 1982, MNRAS 201, 1095.CrossRefGoogle Scholar
Jones, T.J. et al. 1985, Astron. J. 90, 1191.CrossRefGoogle Scholar
Thé, P.S., et al. 1986, Astron. Astrophys. 155, 347.Google Scholar
Young, E.T. et al. 1985, PRE-008N, Internal Report IPAC, JPL, USA.Google Scholar
Wesselius, P.R. et al. 1985, Internal Report ROG, Groningen.Google Scholar