Photoevaporation of protoplanetary discs – I. Hydrodynamic models
In this paper, we consider the effect of the direct ionizing stellar radiation field on the evolution of protoplanetary discs subject to photoevaporative winds. We suggest that models which combine viscous evolution with photoevaporation of the disc incorrectly neglect the direct field after the inn...
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| Veröffentlicht in: | Monthly notices of the Royal Astronomical Society 2006-06, Vol.369 (1), p.216-228 |
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| creator | Alexander, R. D. Clarke, C. J. Pringle, J. E. |
| description | In this paper, we consider the effect of the direct ionizing stellar radiation field on the evolution of protoplanetary discs subject to photoevaporative winds. We suggest that models which combine viscous evolution with photoevaporation of the disc incorrectly neglect the direct field after the inner disc has drained, at late times in the evolution. We construct models of the photoevaporative wind produced by the direct field, first using simple analytic arguments and later using detailed numerical hydrodynamics. We find that the wind produced by the direct field at late times is much larger than has previously been assumed, and we show that the mass-loss rate scales as R1/2in (where Rin is the radius of the instantaneous inner disc edge). We suggest that this result has important consequences for theories of disc evolution, and go on to consider the effects of this result on disc evolution in detail in a companion paper. |
| doi_str_mv | 10.1111/j.1365-2966.2006.10293.x |
| format | Article |
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D.</creatorcontrib><creatorcontrib>Clarke, C. J.</creatorcontrib><creatorcontrib>Pringle, J. E.</creatorcontrib><title>Photoevaporation of protoplanetary discs – I. Hydrodynamic models</title><title>Monthly notices of the Royal Astronomical Society</title><addtitle>Monthly Notices of the Royal Astronomical Society</addtitle><addtitle>Monthly Notices of the Royal Astronomical Society</addtitle><description>In this paper, we consider the effect of the direct ionizing stellar radiation field on the evolution of protoplanetary discs subject to photoevaporative winds. We suggest that models which combine viscous evolution with photoevaporation of the disc incorrectly neglect the direct field after the inner disc has drained, at late times in the evolution. We construct models of the photoevaporative wind produced by the direct field, first using simple analytic arguments and later using detailed numerical hydrodynamics. We find that the wind produced by the direct field at late times is much larger than has previously been assumed, and we show that the mass-loss rate scales as R1/2in (where Rin is the radius of the instantaneous inner disc edge). 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Hydrodynamic models</atitle><jtitle>Monthly notices of the Royal Astronomical Society</jtitle><stitle>Monthly Notices of the Royal Astronomical Society</stitle><addtitle>Monthly Notices of the Royal Astronomical Society</addtitle><date>2006-06-11</date><risdate>2006</risdate><volume>369</volume><issue>1</issue><spage>216</spage><epage>228</epage><pages>216-228</pages><issn>0035-8711</issn><eissn>1365-2966</eissn><coden>MNRAA4</coden><abstract>In this paper, we consider the effect of the direct ionizing stellar radiation field on the evolution of protoplanetary discs subject to photoevaporative winds. We suggest that models which combine viscous evolution with photoevaporation of the disc incorrectly neglect the direct field after the inner disc has drained, at late times in the evolution. We construct models of the photoevaporative wind produced by the direct field, first using simple analytic arguments and later using detailed numerical hydrodynamics. 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| source | Oxford Journals Open Access Collection; Wiley Online Library Journals Frontfile Complete |
| subjects | accretion accretion discs accretion, accretion discs Astronomy circumstellar matter Earth, ocean, space Evaporation Exact sciences and technology hydrodynamics planetary systems: protoplanetary discs Planets Radiation stars: pre-main-sequence |
| title | Photoevaporation of protoplanetary discs – I. Hydrodynamic models |
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