NASA Logo

NTRS

NTRS - NASA Technical Reports Server

Collections About News Help Login
Back to Results
Photoevaporation and the Dispersal of DisksDisk 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.
Document ID
20190001766
Acquisition Source
Ames Research Center
Document Type
Presentation
Authors
Gorti, Uma (Search for Extraterrestrial Intelligence Inst. Moffett Field, CA, United States)
Hollenbach, David (Search for Extraterrestrial Intelligence Inst. Moffett Field, CA, United States)
Dullemond, Kees (Search for Extraterrestrial Intelligence Inst. Moffett Field, CA, United States)
Pascucci, Ilaria (Search for Extraterrestrial Intelligence Inst. Moffett Field, CA, United States)
D'Angelo, Gennaro (Search for Extraterrestrial Intelligence Inst. Moffett Field, CA, United States)
Date Acquired
March 22, 2019
Publication Date
August 27, 2014
Subject Category
Astronomy
Report/Patent Number
ARC-E-DAA-TN17213
Meeting Information
Meeting: The Disk in Relation to The Formation of Planets And Their Protoatmospheres
Location: Beijing
Country: China
Start Date: August 25, 2014
End Date: August 29, 2014
Sponsors: International Space Science Inst.
Funding Number(s)
CONTRACT_GRANT: NNX12AR70A
CONTRACT_GRANT: SAA2401923
Distribution Limits
Public
Copyright
Public Use Permitted.
Keywords
Stellar accretion
Planet forming disks
Planet formation

Related Records

There are no records associated with this record.
No Preview Available