Pre-main-sequence disk accretion in Z Canis Majoris
Lee HartmannHarvard Smithsonian Center for Astrophysics, Cambridge, MA, United StatesScott J. KenyonR. HewettSuzan EdwardsK. M. StromS. E. StromMassachusetts, University Amherst, United StatesJ. R. StaufferNASA Ames Research Center Moffett Field, CA, United States
1989en
ABI
Abstract
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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