Pre-main-sequence disk accretion in Z Canis Majoris

Details Pre-main-sequence disk accretion in Z Canis Majoris Pre-main-sequence disk accretion in Z Canis Majoris

Mar 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...338.1001h&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 338, March 15, 1989, p. 1001-1010. Research supported by the Smithsonian In

Astronomy and Astrophysics

Astronomy

102

Accretion Disks, Pre-Main Sequence Stars, Stellar Evolution, Stellar Mass Accretion, Stellar Models, Infrared Astronomy, Stellar Luminosity, Stellar Spectra, Stellar Winds

Scientific paper

It is suggested that the pre-main-sequence object Z CMa is a luminous accretion disk, similar in many respects to the FU Orionis variables. Z CMa shows the broad, doubled optical absorption lines expected from a rapidly rotating accretion disk. The first overtone CO absorption detected in Z CMa is blue-shifted, suggesting line formation in a disk wind. Accretion at rates about 0.001 solar mass/yr over 100 yr is required to explain the luminosity of Z CMa. The large amount of material accreted (0.1 solar mass/yr) indicates that Z CMa is in a very early stage of stellar evolution, possibly in an initial phase of massive disk accretion.

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