Mass loss from FU Orionis objects

Estimates are presented for the mass loss rates of FU Ori, V1057 Cyg and V1515 Cyg. The approximations are made on the basis of models of the physical conditions required to generate the P Cygni profiles of the observed H-alpha and Na I lines. The spectra were obtained in 1985 using Reticons at the Whipple Observatory and Mt. Hopkins Multiple Mirror Telescope. FU Ori and V1515 Cyg each exhibited an estimate mass loss rate of 1/100,000 solar mass/yr, while that of V1057 Cyg is 10 times smaller. Magnetic wave acceleration is proposed as the driving force for the stellar winds associated with the mass losses, which are at a temperature near 5000 K when leaving the disks proposed around the T Tauri objects.

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