2004/04/20 by Fred C. Adams, David Hollenbach, D. J. Hollenbach +2 · 9 citations
Physics and Astronomy · #Astro and Planetary Science #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Circumstellar disk #Low Mass #Optics #Orion Nebula #Photoevaporation #Physics #RADIUS #Radiation #Star formation #Stars #Stellar, planetary, and galactic studies #Ultraviolet #astro-ph
paper · pdf · doi:10.1086/421989
published as Astrophys.J. 611 (2004) 360-379 · 49 pages including 12 figures; accepted to ApJ
arxiv created 2004/04/20 · openalex publication_date 2004/08/10 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
When stars form within small groups (with N * ≈ 100-500 members), their circumstellar disks are exposed to relatively little extreme-ultraviolet (EUV; h ν > 13.6 eV) radiation but a great deal of far-ultraviolet (FUV; 6 eV < h ν < 13.6 eV) radiation (~10 3 times the local interstellar FUV field) from the most massive stars in the group. This paper calculates the mass-loss rates and evaporation timescales for circumstellar disks exposed to external FUV radiation. Previous work treated large disks and/or intense radiation fields in which the disk radius r d exceeds the critical radius r g where the sound speed in the FUV heated surface layer exceeds the escape speed; it has often been assumed that photoevaporation occurs for r d > r g and is negligible for r d < r g . Since r g ≳ 100 AU for FUV heating, this would imply little mass loss from the planet-forming regions of a disk. In this paper we focus on systems in which photoevaporation is suppressed because r d < r g and show that significant mass loss still takes place as long as r d / r g ≳ 0.1-0.2. Some of the gas extends beyond the disk edge (or above the disk surface) to larger distances where the temperature is higher, the escape speed is lower, and an outflow develops. The resulting evaporation rate is a sensitive function of the central stellar mass and disk radius, which determine the escape speed, and the external FUV flux, which determines the temperature structure of the surface layers and outflowing gas. Disks around red dwarfs, low-mass stars with M * ≲ 0.5 M ☉ , are evaporated and shrink to disk radii r d ≲ 15 AU on short timescales t ≲ 10 Myr when exposed to moderate FUV fields with G 0 = 3000 (where G 0 = 1.7 for the local interstellar FUV field). The disks around solar-type stars are more durable. For intense FUV radiation fields with G 0 = 30,000, however, even these disks shrink to r d ≲ 15 AU on timescales t ~ 10 Myr. Such fields exist within about 0.7 pc of the center of a cluster with N * ≈ 4000 stars. If our solar system formed in the presence of such strong FUV radiation fields, this mechanism could explain why Neptune and Uranus in our solar system are gas-poor, whereas Jupiter and Saturn are relatively gas-rich. This mechanism for photoevaporation can also limit the production of Kuiper Belt objects and can suppress giant planet formation in sufficiently large clusters, such as the Hyades, especially for disks associated with low-mass stars.