We present an open access grid of 3930 calculations of externally evaporating protoplanetary discs. This spans a range of disc sizes (1-400 au), disc masses, UV field strengths (10-104 G0), and stellar masses (0.05-1.9M⊙). The grid is publicly available for download, and offers a means of cheaply including external photoevaporation in disc evolutionary calculations. It can also be queried using an online tool for quick estimates of instantaneous mass-loss rates (e.g for convenient evaluation of real observed systems). The À ÀFRIED" grid itself illustrates that for discs around stars ≤0.3M⊙, external photoevaporation is effective down to small radii ( < 50 au) down to UV fields at least as weak as 10G0. At the other end of the scale, in a 104 G0 environment photoevaporation is effective down to 1 au even for stellar masses at least as high as 1.9M⊙. We also illustrate in which regimes CO survives in the photoevaporative outflow for significant mass-loss rates; marking a system a good candidate to detect external photoevaporation in weak-intermediate UV environments through sub-Keplerian rotation. Finally,wemake illustrative mass-loss rate estimates for discs in Taurus based on theGuilloteau et al. (2011) star-disc parameters, finding that around half are expected to have both significant mass-loss and retain CO in the photoevaporative outflow.

The FRIED grid of mass-loss rates for externally irradiated protoplanetary discs / T.J. Haworth, C.J. Clarke, W. Rahman, A.J. Winter, S. Facchini. - In: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY. - ISSN 0035-8711. - 481:1(2018), pp. 452-466. [10.1093/mnras/sty2323]

The FRIED grid of mass-loss rates for externally irradiated protoplanetary discs

S. Facchini
2018

Abstract

We present an open access grid of 3930 calculations of externally evaporating protoplanetary discs. This spans a range of disc sizes (1-400 au), disc masses, UV field strengths (10-104 G0), and stellar masses (0.05-1.9M⊙). The grid is publicly available for download, and offers a means of cheaply including external photoevaporation in disc evolutionary calculations. It can also be queried using an online tool for quick estimates of instantaneous mass-loss rates (e.g for convenient evaluation of real observed systems). The À ÀFRIED" grid itself illustrates that for discs around stars ≤0.3M⊙, external photoevaporation is effective down to small radii ( < 50 au) down to UV fields at least as weak as 10G0. At the other end of the scale, in a 104 G0 environment photoevaporation is effective down to 1 au even for stellar masses at least as high as 1.9M⊙. We also illustrate in which regimes CO survives in the photoevaporative outflow for significant mass-loss rates; marking a system a good candidate to detect external photoevaporation in weak-intermediate UV environments through sub-Keplerian rotation. Finally,wemake illustrative mass-loss rate estimates for discs in Taurus based on theGuilloteau et al. (2011) star-disc parameters, finding that around half are expected to have both significant mass-loss and retain CO in the photoevaporative outflow.
Accretion; Accretion discs; Circumstellar matter; Hydrodynamics; Photodissociation region (PDR); Planetary systems: formation; Protoplanetary discs
Settore FIS/05 - Astronomia e Astrofisica
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Utilizza questo identificativo per citare o creare un link a questo documento: http://hdl.handle.net/2434/866514
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