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Rapid destruction of protoplanetary discs due to external photoevaporation in star-forming regions

Nicholson, Rhana B; Parker, Richard J; Church, Ross P LU ; Davies, Melvyn B LU ; Fearon, Niamh M and Walton, Sam R J (2019) In Monthly Notices of the Royal Astronomical Society 485. p.4893-4905
Abstract
We analyse N-body simulations of star-forming regions to investigate the effects of external
far- and extreme-ultraviolet photoevaporation from massive stars on protoplanetary discs. By
varying the initial conditions of simulated star-forming regions, such as the spatial distribution,
net bulk motion (virial ratio), and density, we investigate which parameters most affect the rate
at which discs are dispersed due to external photoevaporation. We find that disc dispersal due to
external photoevaporation is faster in highly substructured star-forming regions than in smooth
and centrally concentrated regions. Subvirial star-forming regions undergoing collapse also
show higher rates of disc dispersal than regions... (More)
We analyse N-body simulations of star-forming regions to investigate the effects of external
far- and extreme-ultraviolet photoevaporation from massive stars on protoplanetary discs. By
varying the initial conditions of simulated star-forming regions, such as the spatial distribution,
net bulk motion (virial ratio), and density, we investigate which parameters most affect the rate
at which discs are dispersed due to external photoevaporation. We find that disc dispersal due to
external photoevaporation is faster in highly substructured star-forming regions than in smooth
and centrally concentrated regions. Subvirial star-forming regions undergoing collapse also
show higher rates of disc dispersal than regions that are in virial equilibrium or are expanding.
In moderately dense (∼100 M pc −3 ) regions, half of all protoplanetary discs with radii
≥100 au are photoevaporated within 1 Myr, three times faster than is currently suggested by
observational studies. Discs in lower density star-forming regions (∼10 M pc −3 ) survive for
longer, but half are still dispersed on short time-scales (∼2 Myr). This demonstrates that the
initial conditions of the star-forming regions will greatly impact the evolution and lifetime of
protoplanetary discs. These results also imply that either gas giant planet formation is extremely
rapid and occurs before the gas component of discs is evaporated, or gas giants only form
in low-density star-forming regions where no massive stars are present to photoevaporate gas
from protoplanetary discs. (Less)
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organization
publishing date
type
Contribution to journal
publication status
published
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in
Monthly Notices of the Royal Astronomical Society
volume
485
pages
4893 - 4905
publisher
Oxford University Press (OUP)
external identifiers
  • scopus:85070085365
ISSN
0035-8711
DOI
10.1093/mnras/stz606
language
English
LU publication?
yes
id
8a77121a-13a9-4607-9b48-3a72c5705c37
alternative location
https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/stz606/5420762
date added to LUP
2019-06-05 14:06:56
date last changed
2019-11-15 01:53:10
@article{8a77121a-13a9-4607-9b48-3a72c5705c37,
  abstract     = {We analyse N-body simulations of star-forming regions to investigate the effects of external<br/>far- and extreme-ultraviolet photoevaporation from massive stars on protoplanetary discs. By<br/>varying the initial conditions of simulated star-forming regions, such as the spatial distribution,<br/>net bulk motion (virial ratio), and density, we investigate which parameters most affect the rate<br/>at which discs are dispersed due to external photoevaporation. We find that disc dispersal due to<br/>external photoevaporation is faster in highly substructured star-forming regions than in smooth<br/>and centrally concentrated regions. Subvirial star-forming regions undergoing collapse also<br/>show higher rates of disc dispersal than regions that are in virial equilibrium or are expanding.<br/>In moderately dense (∼100 M  pc −3 ) regions, half of all protoplanetary discs with radii<br/>≥100 au are photoevaporated within 1 Myr, three times faster than is currently suggested by<br/>observational studies. Discs in lower density star-forming regions (∼10 M  pc −3 ) survive for<br/>longer, but half are still dispersed on short time-scales (∼2 Myr). This demonstrates that the<br/>initial conditions of the star-forming regions will greatly impact the evolution and lifetime of<br/>protoplanetary discs. These results also imply that either gas giant planet formation is extremely<br/>rapid and occurs before the gas component of discs is evaporated, or gas giants only form<br/>in low-density star-forming regions where no massive stars are present to photoevaporate gas<br/>from protoplanetary discs.},
  author       = {Nicholson, Rhana B and Parker, Richard J and Church, Ross P and Davies, Melvyn B and Fearon, Niamh M and Walton, Sam R J},
  issn         = {0035-8711},
  language     = {eng},
  pages        = {4893--4905},
  publisher    = {Oxford University Press (OUP)},
  series       = {Monthly Notices of the Royal Astronomical Society},
  title        = {Rapid destruction of protoplanetary discs due to external photoevaporation in star-forming regions},
  url          = {http://dx.doi.org/10.1093/mnras/stz606},
  volume       = {485},
  year         = {2019},
}