Extreme evaporation of planets in hot thermally unstable protoplanetary discs: the case of FU Ori
File(s)
Published version
Author(s)
Nayakshin, Sergei
Owen, James E
Elbakyan, Vardan
Type
Journal Article
Abstract
Disc accretion rate onto low mass protostar FU Ori suddenly increased hundreds of times 85 yr ago and remains elevated to this day. We show that the sum of historic and recent observations challenges existing FU Ori models. We build a theory of a new process, Extreme Evaporation (EE) of young gas giant planets in discs with midplane temperatures of ≳ 30 000 K. Such temperatures are reached in the inner 0.1 AU during thermal instability bursts. In our 1D time-dependent code the disc and an embedded planet interact through gravity, heat, and mass exchange. We use disc viscosity constrained by simulations and observations of dwarf novae instabilities, and we constrain planet properties with a stellar evolution code. We show that dusty gas giants born in the outer self-gravitating disc reach the innermost disc in a ∼O(104) yr with radius of ∼10RJ. We show that their EE rates are ≳10−5M⊙
yr−1; if this exceeds the background disc accretion activity then the system enters a planet-sourced mode. Like a stellar secondary in mass-transferring binaries, the planet becomes the dominant source of matter for the star, albeit for ∼O(100) yr. We find that a ∼6 Jupiter mass planet evaporating in a disc fed at a time-averaged rate of ∼10−6M⊙
yr−1 appears to explain all that we currently know about FU Ori accretion outburst. More massive planets and/or planets in older less massive discs do not experience EE process. Future FUOR modelling may constrain planet internal structure and evolution of the earliest discs.
yr−1; if this exceeds the background disc accretion activity then the system enters a planet-sourced mode. Like a stellar secondary in mass-transferring binaries, the planet becomes the dominant source of matter for the star, albeit for ∼O(100) yr. We find that a ∼6 Jupiter mass planet evaporating in a disc fed at a time-averaged rate of ∼10−6M⊙
yr−1 appears to explain all that we currently know about FU Ori accretion outburst. More massive planets and/or planets in older less massive discs do not experience EE process. Future FUOR modelling may constrain planet internal structure and evolution of the earliest discs.
Date Issued
2023-07
Date Acceptance
2023-05-03
Citation
Monthly Notices of the Royal Astronomical Society, 2023, 523 (1), pp.385-403
ISSN
0035-8711
Publisher
Oxford University Press
Start Page
385
End Page
403
Journal / Book Title
Monthly Notices of the Royal Astronomical Society
Volume
523
Issue
1
Copyright Statement
© 2023 The Author(s)
Published by Oxford University Press on behalf of Royal Astronomical Society. This is an Open Access article distributed under the terms of the Creative
Commons Attribution License (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium,
provided the original work is properly cited.
Published by Oxford University Press on behalf of Royal Astronomical Society. This is an Open Access article distributed under the terms of the Creative
Commons Attribution License (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium,
provided the original work is properly cited.
License URL
Identifier
https://www.webofscience.com/api/gateway?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000995754400008&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=a2bf6146997ec60c407a63945d4e92bb
Subjects
ACCRETION DISC
Astronomy & Astrophysics
BURST MODE
DWARF NOVAE
EPISODIC ACCRETION
GIANT PLANETS
GRAVITATIONAL-INSTABILITY
INNER REGIONS
LAYERED ACCRETION
ORIONIS OBJECTS
OUTBURSTS
Physical Sciences
planet-disc interactions
planets and satellites: formation
protoplanetary discs
Science & Technology
Publication Status
Published
Date Publish Online
2023-05-12