Photoevaporation
Sign in to savePhotoevaporation is the process where energetic radiation ionises gas and causes it to disperse away from the ionising source. The term is typically used in an astrophysical context where ultraviolet radiation from hot stars acts on clouds of material such as molecular clouds, protoplanetary disks, or planetary atmospheres.
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Within Vinony's link graph, Photoevaporation is referenced by 48 other articles, and connects out to heat capacity ratio, water and star.
It is catalogued under the topic Concepts in stellar astronomy.
Its subject is documented across 18 Wikipedia language editions.
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- physical phenomenon
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- purl.obolibrary.org/obo/ENVO_01001146
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Encyclopedic overview
6 sectionsContents
- Molecular clouds
- Evaporating gaseous globules (EGGs)
- Planetary atmospheres
- Protoplanetary disks
- Regions containing protoplanetary disks with clear signs of external photoevaporation
- References
Photoevaporation is the process where energetic radiation ionises gas and causes it to disperse away from the ionising source. The term is typically used in an astrophysical context where ultraviolet radiation from hot stars acts on clouds of material such as molecular clouds, protoplanetary disks, or planetary atmospheres.
==Molecular clouds== thumb|right|upright=1.0|Eagle Nebula pillars being photoevaporated One of the most obvious manifestations of astrophysical photoevaporation is seen in the eroding structures of molecular clouds that luminous stars are born within.
Excerpted from Wikipedia’s “Photoevaporation” article, available under the CC BY-SA 4.0 licence.