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Five steps in the evolution from protoplanetary to debris disk

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Abstract

The protoplanetary disks seen around Herbig Ae stars eventually dissipate leaving just a tenuous debris disk, comprised of planetesimals and the dust derived from them, as well as possibly gas and planets. This paper uses the properties of the youngest (10–20 Myr) A star debris disks to consider the transition from protoplanetary to debris disk. It is argued that the physical distinction between these two classes should rest on the presence of primordial gas in sufficient quantities to dominate the motion of small dust grains (rather than on the secondary nature of the dust or its level of stirring). This motivates an observational classification based on the dust emission spectrum which is empirically defined so that A star debris disks require fractional excesses <3 at 12 μm and <2000 at 70 μm. We also propose that a useful hypothesis to test is that the planet and planetesimal systems seen on the main sequence are already in place during the protoplanetary disk phase, but are obscured or overwhelmed by the rest of the disk. This may be only weakly true if the architecture of the planetary system continues to change until frozen at the epoch of disk dispersal, or completely false if planets and planetesimals form during the relatively short dispersal phase. Five steps in the transition are discussed: (i) the well-known carving of an inner hole to form a transition disk; (ii) depletion of mm-sized dust in the outer disk, where it is noted that it is of critical importance to ascertain whether this mass ends up in larger planetesimals or is collisionally depleted; (iii) final clearing of inner regions, where it is noted that multiple debris-like mechanisms exist to replenish moderate levels of hot dust at later phases, and that these likely also operate in protoplanetary disks; (iv) disappearance of the gas, noting the recent discoveries of both primordial and secondary gas in debris disks which highlight our ignorance in this area and its impending enlightenment by ALMA; (v) formation of ring-like structure of planetesimals, noting that these are shaped by interactions with planets, and that the location of the planetesimals in protoplanetary disks may be unrelated to that of dust concentrations therein that are set by gas interactions.

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Notes

  1. In this paper optical depth refers to the fraction of starlight that reaches disk material directly, and so refers to the depth at optical and UV wavelengths along the line-of-sight to the star.

  2. Here optical depth refers to that along the line-of-sight to the observer at the wavelength in question. In the optically thin regime the observer sees all of the emission from the disk at this wavelength, whereas much of that emission remains hidden in the optically thick regime.

  3. The mm-sized dust can also be accreted onto the star through drag induced by the gas, but since this process would also occur throughout the earlier protoplanetary disk phase, relative to which the transition is rapid, this likely only affects a small fraction of the dust.

  4. This is because in a debris disk the same physics applies to all objects in the size range from planetesimals down to mm-sized dust, so as long as collisions do not change significantly the orbits of debris from those of their parent body, then the distribution of mm-sized dust should be the same as that of the planetesimals. This is not the case in a protoplanetary disk due to gas forces which result in the possibility that the distribution of mm-sized dust bears little resemblance to that of the planetesimals, as discussed in Sect. 3.2.

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Acknowledgements

The authors are grateful for support from the European Union through ERC grant number 279973.

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Authors and Affiliations

  1. Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK

    M. C. Wyatt, O. Panić, G. M. Kennedy & L. Matrà

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  1. M. C. Wyatt
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  2. O. Panić
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  3. G. M. Kennedy
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  4. L. Matrà
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Correspondence to M. C. Wyatt.

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This article belongs to the Topical Collection: Herbig Ae/Be stars, Guest Editors: R.D. Oudmaijer, W.-J. de Wit.

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Wyatt, M.C., Panić, O., Kennedy, G.M. et al. Five steps in the evolution from protoplanetary to debris disk. Astrophys Space Sci 357, 103 (2015). https://doi.org/10.1007/s10509-015-2315-6

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