Publication Date:
2019-07-20
Description:
Disk disperse in a few million years, before which they must form planets. Photoevaporation and viscosity are mainly responsible for disk dispersal. EUV, FUV and X-rays have all been suggested as photoevaporation agents, disk evolutionary scenarios and predicted mass loss rates in each case differ. Stellar mass and radiation field, disk properties, magnitude of viscosity, and dust evolution all play significant roles in determining the evolution of the disk and its lifetime. Observational diagnostics of photoevaperative flows include [Nell] and perhaps [OI]. These are at present inconclusive and better diagnostics are needed.
Keywords:
Astronomy
Type:
ARC-E-DAA-TN17213
,
The Disk in Relation to The Formation of Planets And Their Protoatmospheres; Aug 25, 2014 - Aug 29, 2014; Beijing; China
Format:
application/pdf