Mass loss from the protoplanetary nebula

Details Mass loss from the protoplanetary nebula Mass loss from the protoplanetary nebula

Jun 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982a%26a...110..209h&link_type=abstract

Astronomy and Astrophysics, vol. 110, no. 2, June 1982, p. 209-214.

Astronomy and Astrophysics

Astrophysics

8

Planetary Nebulae, Protoplanets, Solar Radiation, Stellar Mass Ejection, Extreme Ultraviolet Radiation, Solar Wind, Stellar Winds, T Tauri Stars, Temperature Distribution

Scientific paper

The mass loss from the protoplanetary nebula is examined in terms of energy-balance considerations that take into account loss from the innermost boundary of the nebula. Within the limits of the adopted simple blow-off approximation, the intervals during which the nebula disappears are of the order of one-billion years for heating of the nebula by solar EUV radiation and of the order of one-million years when the nebula interacts with a T-Tauri-like solar wind. An analytical model for the evolution of the inner and outer boundary of the nebula until its complete disappearance is developed, and temperatures occurring in the outer layers of the nebula due to EUV heating are calculated.

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