Hostname: page-component-78c5997874-dh8gc Total loading time: 0 Render date: 2024-11-09T14:41:02.089Z Has data issue: false hasContentIssue false
  • English
  • Français

Accretion-Disk-Instability Model for Outbursts of FU Orionis

Published online by Cambridge University Press:  12 April 2016

Hanami Hitoshi
Hanami Hitoshi*
Affiliation:
Department of Physics, Hokkaido University060 Sapporo, 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 FU Orionis objects show us the abrupt brightening by ~5 map. The two best studied examples, FU ori and V1057Cyg, brightened and have remained very luminous for years and began to fade gradually (cf. Herbig 1977). On the other hand, a large number of young stellar objects have been discovered with energetic molecular bipolar outflows (Lada 1985, for a review). On high-resolution radio observations, the disks have been detected around the central infrared sources (cf. Kaifu et al. 1984, Hasegawa et al. 1984). Most of the disks seem to be perpendicular to the bipolar outflows. These observations suggests that the disk is strongly related with the energetics phenomena like bipolar outflow in star forming regions. (cf.Okuda and Ikeuchi 1986, Hanami and Sakashita 1986, Pudritz 1985, Shibata and Uchida 1985)

Type
Part III. Chemical and Dynamical Structures of Exploding Stars
Information
International Astronomical Union Colloquium , Volume 108: Atmospherics Diagnostics of Stellar Evolution: Chemical Peculiarity, Mass Loss, and Explosion , 1988 , pp. 240 - 241
Copyright
Copyright © Springer-Verlag 1988

References

Cannizzo, J.K. and Wheeler, J.C., 1984, Ap. J. Suppl., 55, 367.CrossRefGoogle Scholar
Hanami, H., 1987, “NATO ASI. Galactic and Extragalactic Star Formation”.Google Scholar
Hanami, H. and Sakashita, S., 1986, “IAU Symposium No. 115 on Star Forming Regions”, edited by Peimbert, and Jyugaku, .Google Scholar
Hartman, L. and Kenyon, S.J., 1985, Ap. J., 299, 462.Google Scholar
Hartman, L. and Kenyon, S.J., 1987, Ap. J., 312, 243.CrossRefGoogle Scholar
Hasegawa, T., et al., 1984, Ap. J., 283, 117.Google Scholar
Herbig, G.H., 1977, Ap.J., 214, 747.CrossRefGoogle Scholar
Hoshi, R., 1979, Prog. Theor. Physics, 61, 1307.Google Scholar
Kaifu, N., et al. 1984, A. Ap., 134, 7.Google Scholar
Lada, C.J., 1985, Ann. Rev. Astrophys. 23, 267.Google Scholar
Lin, D.N.C. and Pringle, J.E., 1987, M.N.R.A.S., 225, 607.Google Scholar
Meyer, Y. and Meyer-Hofmeister, E., 1981, A. Ap., 104, L10.Google Scholar
Mineshige, S. and Osaki, Y., 1983, Publ. A, Soc, Japan, 35, 377.Google Scholar
Okuda, T. and Ikeuchi, S., 1986, Publ. A, Soc, Japan,, 38, 199.Google Scholar
Osaki, Y., 1974, Publ. A, Soc, Japan,, 26, 429.Google Scholar
Pudritz, R.E., 1985, Ap. J., 293, 216.Google Scholar
Shibata, K. and Uchida, Y., 1985, Publ. A, Soc, Japan,, 37, 31.Google Scholar
Smak, J., 1982, Acta. Astron., 32, 199.Google Scholar