Hostname: page-component-55f67697df-4ks9w Total loading time: 0 Render date: 2025-05-10T04:39:00.305Z Has data issue: false hasContentIssue false
  • English
  • Français

A Swept-Up Molecular Bubble in L1551

Published online by Cambridge University Press:  12 April 2016

Saeko S. Hayashi ,
Masahiko Hayashi  and
Norio Kaifu
Saeko S. Hayashi
Affiliation:
Joint Astronomy Centre, 665 Komohana Street Hilo, Hawaii 96720, U.S.A.
Masahiko Hayashi
Affiliation:
Department of Astronomy, University of TokyoBunkyo, Tokyo 181, Japan
Norio Kaifu
Affiliation:
Nobeyama Radio Observatory, Nobeyama, Nagano 384-13, Japan

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The environment of the young stellar object IRS5 in L1551 dark cloud is a representative of the “protostellar disk and outflow” systems found in star forming regions. The bipolar molecular outflow there was discovered as the first of its kind a decade ago (Snell, Loren, and Plambeck 1980). Its location in the sky, that is, its proximity (160 pc), isolation, and its almost edge-on inclination have favored the observation in great detail. IRS5 is thought to have the spectral type G - K (Mundt et al. 1985) similar to the Sun, with its dominant activity in the stellar wind, and not in the UV radiation as in massive protostars. The blueshifted and redshifted outflow lobes are clearly resolved into a pair of shell structures. The successive studies, mostly in CO lines, have led to a model of the outflow in which the molecular material is accelerated at the edge of a cavity evacuated by the protostellar wind (e.g. Uchida et al. 1987, Rainey et al. 1987, Moriarty-Schieven and Snell 1988).

Type
III. Discs, Outflows, Jets and HH Objects
Information
International Astronomical Union Colloquium , Volume 120: Structure and Dynamics of the Interstellar Medium , 1989 , pp. 260 - 263
Copyright
Copyright © Springer-Verlag 1989

References

Bally, J. and Hayashi, M. 1989, in preparation.Google Scholar
Bieging, J.H., Cohen, M., and Schwartz, P.R. 1984, Ap. J.,k 282, 699.CrossRefGoogle Scholar
Cohen, M., Harvey, P.M., and Schwartz, R.D. 1985, Ap. J., 296, 633.Google Scholar
Emerson, J.P. et al. 1984, Ap. J. Lett., 278, L49.Google Scholar
Kaifu, N. et al. 1984, Astr. Ap., 134, 7.Google Scholar
Lada, C.J. 1985, Ann. Rev. Astron. Astrophys., 23, 267.Google Scholar
Menten, K.M., and Walmsley, C.M. 1985, Astr. Ap., 146, 369.Google Scholar
Moriarty-Schieven, G., and Snell, R.L. 1988, Ap. J., 332, 364.Google Scholar
Mundt, R., and Fried, J.W. 1983, Ap. J. Lett., 274, L83.Google Scholar
Mundt, R. et al. 1985, Ap. J. Lett., 297, L41.Google Scholar
Rainey, R. et al. 1987, Astr. Ap., 179, 347.Google Scholar
Snell, R.L., Loren, R.B., and Plambeck, R.L. 1980, Ap. J. Lett, 239, L17.Google Scholar
Uchida, Y. et al. 1987, P.A.S.J., 30, 907.Google Scholar
Weaver, R. et al. 1977, Ap. J., 218, 377.Google Scholar