Photoevaporation

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.[1][2][3]

  1. ^ Mellema, G.; Raga, A. C.; Canto, J.; Lundqvist, P.; Balick, B.; Steffen, W.; Noriega-Crespo, A. (1998). "Photo-evaporation of clumps in planetary nebulae". Astronomy and Astrophysics. 331: 335. arXiv:astro-ph/9710205. Bibcode:1998A&A...331..335M.
  2. ^ Owen, James E.; Ercolano, Barbara; Clarke, Cathie J. (2011). "Protoplanetary disc evolution and dispersal: The implications of X-ray photoevaporation". Monthly Notices of the Royal Astronomical Society. 412 (1): 13–25. arXiv:1010.0826. Bibcode:2011MNRAS.412...13O. doi:10.1111/j.1365-2966.2010.17818.x. S2CID 118875248.
  3. ^ Wu, Yanqin; Lithwick, Yoram (2013). "Density and Eccentricity of Kepler Planets". The Astrophysical Journal. 772 (1): 74. arXiv:1210.7810. Bibcode:2013ApJ...772...74W. doi:10.1088/0004-637X/772/1/74. S2CID 118376433.