Outwards migration for planets in stellar irradiated 3D discs
(2015) In Monthly Notices of the Royal Astronomical Society 452(2). p.1717-1726- Abstract
- For the very first time we present 3D simulations of planets embedded in stellar irradiated discs. It is well known that thermal effects could reverse the direction of planetary migration from inwards to outwards, potentially saving planets in the inner, optically thick parts of the protoplanetary disc. When considering stellar irradiation in addition to viscous friction as a source of heating, the outer disc changes from a shadowed to a flared structure. Using a suited analytical formula it has been shown that in the flared part of the disc the migration is inwards; planets can migrate outwards only in shadowed regions of the disc, because the radial gradient of entropy is stronger there. In order to confirm this result numerically, we... (More)
- For the very first time we present 3D simulations of planets embedded in stellar irradiated discs. It is well known that thermal effects could reverse the direction of planetary migration from inwards to outwards, potentially saving planets in the inner, optically thick parts of the protoplanetary disc. When considering stellar irradiation in addition to viscous friction as a source of heating, the outer disc changes from a shadowed to a flared structure. Using a suited analytical formula it has been shown that in the flared part of the disc the migration is inwards; planets can migrate outwards only in shadowed regions of the disc, because the radial gradient of entropy is stronger there. In order to confirm this result numerically, we have computed the total torque acting on planets held on fixed orbits embedded in stellar irradiated 3D discs using the hydrodynamical code FARGOCA. We find qualitatively good agreement between the total torque obtained with numerical simulations and the one predicted by the analytical formula. For large masses (>20 M-circle plus) we find quantitative agreement, and we obtain outwards migration regions for planets up to 60 M-circle plus in the early stages of accretional discs. We find nevertheless that the agreement with the analytic formula is quite fortuitous because the formula underestimates the size of the horseshoe region; this error is compensated by imperfect estimates of other terms, most likely the cooling rate and the saturation. (Less)
Please use this url to cite or link to this publication:
https://lup.lub.lu.se/record/8074341
- author
- Lega, E. ; Morbidelli, A. ; Bitsch, Bertram LU ; Crida, A. and Szulagyi, J.
- organization
- publishing date
- 2015
- type
- Contribution to journal
- publication status
- published
- subject
- keywords
- methods: numerical, planet-disc interactions, protoplanetary discs
- in
- Monthly Notices of the Royal Astronomical Society
- volume
- 452
- issue
- 2
- pages
- 1717 - 1726
- publisher
- Oxford University Press
- external identifiers
-
- wos:000360851900052
- scopus:84940112183
- ISSN
- 1365-2966
- DOI
- 10.1093/mnras/stv1385
- language
- English
- LU publication?
- yes
- id
- 7c575a07-3365-48bb-b2de-141d8217993b (old id 8074341)
- date added to LUP
- 2016-04-01 11:12:01
- date last changed
- 2024-01-07 10:12:28
@article{7c575a07-3365-48bb-b2de-141d8217993b,
abstract = {{For the very first time we present 3D simulations of planets embedded in stellar irradiated discs. It is well known that thermal effects could reverse the direction of planetary migration from inwards to outwards, potentially saving planets in the inner, optically thick parts of the protoplanetary disc. When considering stellar irradiation in addition to viscous friction as a source of heating, the outer disc changes from a shadowed to a flared structure. Using a suited analytical formula it has been shown that in the flared part of the disc the migration is inwards; planets can migrate outwards only in shadowed regions of the disc, because the radial gradient of entropy is stronger there. In order to confirm this result numerically, we have computed the total torque acting on planets held on fixed orbits embedded in stellar irradiated 3D discs using the hydrodynamical code FARGOCA. We find qualitatively good agreement between the total torque obtained with numerical simulations and the one predicted by the analytical formula. For large masses (>20 M-circle plus) we find quantitative agreement, and we obtain outwards migration regions for planets up to 60 M-circle plus in the early stages of accretional discs. We find nevertheless that the agreement with the analytic formula is quite fortuitous because the formula underestimates the size of the horseshoe region; this error is compensated by imperfect estimates of other terms, most likely the cooling rate and the saturation.}},
author = {{Lega, E. and Morbidelli, A. and Bitsch, Bertram and Crida, A. and Szulagyi, J.}},
issn = {{1365-2966}},
keywords = {{methods: numerical; planet-disc interactions; protoplanetary discs}},
language = {{eng}},
number = {{2}},
pages = {{1717--1726}},
publisher = {{Oxford University Press}},
series = {{Monthly Notices of the Royal Astronomical Society}},
title = {{Outwards migration for planets in stellar irradiated 3D discs}},
url = {{http://dx.doi.org/10.1093/mnras/stv1385}},
doi = {{10.1093/mnras/stv1385}},
volume = {{452}},
year = {{2015}},
}