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Circumstellar Disks and Star Formation

Published online by Cambridge University Press:  30 March 2016

L. Hartmann ,
M. Gomez  and
S.J. Kenyon
L. Hartmann
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridg e, MA 02138
M. Gomez
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridg e, MA 02138
S.J. Kenyon
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridg e, MA 02138

Extract

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Results from the IRAS satellite showed that many pre-main sequence stars exhibited unexpectedly large fluxes in the infrared spectral region. Several studies have shown that the simplest and most satisfying explanation of this excess emission is that it arises in optically-thick, dusty, circumstellar disks (Rucinski 1985; Adams, Lada, and Shu 1987, 1988; Kenyon and Hartmann 1987; Bertout, Basri, and Bouvier 1988; Basri and Bertout 1989). The masses of these disks are estimated to range between 10-3M⊙ to 1M⊙ (Beckwith et al. 1990; Adams et al. 1990), large enough that disk accretion may have a significant effect on the evolution of the central star. Indeed, Mercer-Smith, Cameron, and Epstein (1984) suggested that stars are essentially completely accreted from disks, rather than formed from quasi-spherical accretion (Stabler 1983, 1988).

Type
Joint Discussions
Information
Highlights of Astronomy , Volume 9: Highlights of Astronomy. As presented at the XXIst General Assembly of the IAU, 1991 , 1992 , pp. 377 - 380
Copyright
Copyright © Kluwer 1992

References

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