Solution to the debris disc mass problem: planetesimals are born small?
TLDR
In this paper, the authors estimate the total mass of the disc by extrapolating up the mass of emitting dust with the help of collisional cascade models, and argue that the easiest solution would be to assume that planetesimals in systems with bright debris discs were "born small", with sizes in the kilometre range, especially at large distances from the stars.Abstract:
Debris belts on the periphery of planetary systems, encompassing the region occupied by planetary orbits, are massive analogues of the Solar system's Kuiper belt. They are detected by thermal emission of dust released in collisions amongst directly unobservable larger bodies that carry most of the debris disc mass. We estimate the total mass of the discs by extrapolating up the mass of emitting dust with the help of collisional cascade models. The resulting mass of bright debris discs appears to be unrealistically large, exceeding the mass of solids available in the systems at the preceding protoplanetary stage. We discuss this "mass problem" in detail and investigate possible solutions to it. These include uncertainties in the dust opacity and planetesimal strength, variation of the bulk density with size, steepening of the size distribution by damping processes, the role of the unknown "collisional age" of the discs, and dust production in recent giant impacts. While we cannot rule out the possibility that a combination of these might help, we argue that the easiest solution would be to assume that planetesimals in systems with bright debris discs were "born small", with sizes in the kilometre range, especially at large distances from the stars. This conclusion would necessitate revisions to the existing planetesimal formation models, and may have a range of implications for planet formation. We also discuss potential tests to constrain the largest planetesimal sizes and debris disc masses.read more
Citations
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On the Submillimeter Opacity of Protoplanetary Disks
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The effects of a stellar encounter on a planetesimal disk
Hiroshi Kobayashi,Shigeru Ida +1 more
TL;DR: In this paper, the effects of a passing stellar encounter on a planetesimal disk through analytical calculations and numerical simulations were investigated, and the boundary radius outside which planet formation is inhibited by disruptive collisions with high relative velocities was derived.
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The Ophiuchus DIsc Survey Employing ALMA (ODISEA) - III. The evolution of substructures in massive discs at 3-5 au resolution
Lucas A. Cieza,Camilo González-Ruilova,Antonio Hales,P. Pinilla,Dary Ruíz-Rodríguez,Alice Zurlo,Simon Casassus,Sebastián Pérez,Hector Canovas,Carla Arce-Tord,Mario Flock,Nicolás T. Kurtovic,Sebastian Marino,Pedro H Nogueira,Laura M. Pérez,Daniel J. Price,David A. Principe,Jonathan Williams +17 more
TL;DR: In this article, 1.3 mm continuum ALMA long-baseline observations at 3-5 au resolution of 10 of the brightest discs from the Ophiuchus DIsc Survey Employing ALMA (ODISEA) project were used to identify a total of 26 narrow rings and gaps distributed in 8 sources and 3 discs with small dust cavities.
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On the origin & thermal stability of Arrokoth's and Pluto's ices
Carey M. Lisse,Leslie A. Young,Dale P. Cruikshank,Scott A. Sandford,Bernard Schmitt,S. A. Stern,Harold A. Weaver,Orkan M. Umurhan,Y. J. Pendleton,J. T. Keane,G. R. Gladstone,G. R. Gladstone,J. M. Parker,R. P. Binzel,Alissa M. Earle,Mihaly Horanyi,Mohamed Ramy El-Maarry,Mohamed Ramy El-Maarry,Andrew F. Cheng,J. M. Moore,William B. McKinnon,William M. Grundy,Jj Kavelaars,Ivan Linscott,Wladimir Lyra,B. L. Lewis,B. L. Lewis,Daniel T. Britt,John R. Spencer,Catherine B. Olkin,Ralph L. McNutt,H. A. Elliott,H. A. Elliott,N. Dello-Russo,Jordan K. Steckloff,Jordan K. Steckloff,Marc Neveu,Marc Neveu,Olivier Mousis +38 more
TL;DR: In this article, the long-term nature of the stable majority ices that could be present in Kuiper Belt object (KBO) 2014 MU69 (also called Arrokoth; hereafter “MU69”) after its 4.6 Gyr residence in the Edgeworth-Kuiper belt (EKB) as a cold classical object was discussed in a thermodynamic, geologically empirical way.
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Planetesimal formation by the streaming instability in a photoevaporating disk
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References
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