The structure of protoplanetary discs around evolving young stars
(2015) In Astronomy & Astrophysics 575.- Abstract
- The formation of planets with gaseous envelopes takes place in protoplanetary accretion discs on time scales of several million years. Small dust particles stick to each other to form pebbles, pebbles concentrate in the turbulent flow to form planetesimals and planetary embryos and grow to planets, which undergo substantial radial migration. All these processes are influenced by the underlying structure of the protoplanetary disc, specifically the profiles of temperature, gas scale height, and density. The commonly used disc structure of the minimum mass solar nebula (MMSN) is a simple power law in all these quantities. However, protoplanetary disc models with both viscous and stellar heating show several bumps and dips in temperature,... (More)
- The formation of planets with gaseous envelopes takes place in protoplanetary accretion discs on time scales of several million years. Small dust particles stick to each other to form pebbles, pebbles concentrate in the turbulent flow to form planetesimals and planetary embryos and grow to planets, which undergo substantial radial migration. All these processes are influenced by the underlying structure of the protoplanetary disc, specifically the profiles of temperature, gas scale height, and density. The commonly used disc structure of the minimum mass solar nebula (MMSN) is a simple power law in all these quantities. However, protoplanetary disc models with both viscous and stellar heating show several bumps and dips in temperature, scale height, and density caused by transitions in opacity, which are missing in the MMSN model. These play an important role in the formation of planets, since they can act as sweet spots for forming planetesimals via the streaming instability and affect the direction and magnitude of type-I migration. We present 2D simulations of accretion discs that feature radiative cooling and viscous and stellar heating, and they are linked to the observed evolutionary stages of protoplanetary discs and their host stars. These models allow us to identify preferred planetesimal and planet formation regions in the protoplanetary disc as a function of the disc's metallicity, accretion rate, and lifetime. We derive simple fitting formulae that feature all structural characteristics of protoplanetary discs during the evolution of several Myr. These fits are straightforward for applying to modelling any growth stage of planets where detailed knowledge of the underlying disc structure is required. (Less)
Please use this url to cite or link to this publication:
https://lup.lub.lu.se/record/5297079
- author
- Bitsch, Bertram LU ; Johansen, Anders LU ; Lambrechts, Michiel LU and Morbidelli, Alessandro
- organization
- publishing date
- 2015
- type
- Contribution to journal
- publication status
- published
- subject
- keywords
- planet-disk interactions, accretion disks, accretion, planets and satellites: formation, radiative transfer, hydrodynamics
- in
- Astronomy & Astrophysics
- volume
- 575
- article number
- A28
- publisher
- EDP Sciences
- external identifiers
-
- wos:000350249100028
- scopus:84922983194
- ISSN
- 0004-6361
- DOI
- 10.1051/0004-6361/201424964
- language
- English
- LU publication?
- yes
- id
- a4c9403a-c693-4be3-99b7-af27f2a23c0a (old id 5297079)
- date added to LUP
- 2016-04-01 13:51:43
- date last changed
- 2022-12-11 20:34:36
@article{a4c9403a-c693-4be3-99b7-af27f2a23c0a,
abstract = {{The formation of planets with gaseous envelopes takes place in protoplanetary accretion discs on time scales of several million years. Small dust particles stick to each other to form pebbles, pebbles concentrate in the turbulent flow to form planetesimals and planetary embryos and grow to planets, which undergo substantial radial migration. All these processes are influenced by the underlying structure of the protoplanetary disc, specifically the profiles of temperature, gas scale height, and density. The commonly used disc structure of the minimum mass solar nebula (MMSN) is a simple power law in all these quantities. However, protoplanetary disc models with both viscous and stellar heating show several bumps and dips in temperature, scale height, and density caused by transitions in opacity, which are missing in the MMSN model. These play an important role in the formation of planets, since they can act as sweet spots for forming planetesimals via the streaming instability and affect the direction and magnitude of type-I migration. We present 2D simulations of accretion discs that feature radiative cooling and viscous and stellar heating, and they are linked to the observed evolutionary stages of protoplanetary discs and their host stars. These models allow us to identify preferred planetesimal and planet formation regions in the protoplanetary disc as a function of the disc's metallicity, accretion rate, and lifetime. We derive simple fitting formulae that feature all structural characteristics of protoplanetary discs during the evolution of several Myr. These fits are straightforward for applying to modelling any growth stage of planets where detailed knowledge of the underlying disc structure is required.}},
author = {{Bitsch, Bertram and Johansen, Anders and Lambrechts, Michiel and Morbidelli, Alessandro}},
issn = {{0004-6361}},
keywords = {{planet-disk interactions; accretion disks; accretion; planets and satellites: formation; radiative transfer; hydrodynamics}},
language = {{eng}},
publisher = {{EDP Sciences}},
series = {{Astronomy & Astrophysics}},
title = {{The structure of protoplanetary discs around evolving young stars}},
url = {{http://dx.doi.org/10.1051/0004-6361/201424964}},
doi = {{10.1051/0004-6361/201424964}},
volume = {{575}},
year = {{2015}},
}