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Disc wind models for FU Ori objects

Abstract:

We present disc wind models aimed at reproducing the main features of the strong Na I resonance line P Cygni profiles in the rapidly accreting pre-main-sequence FU Ori objects. We conducted Monte Carlo radiative transfer simulations for a standard magnetocentrifugally driven wind (MHD) model and our own ‘Genwind’ models, which allows for a more flexible wind parametrization. We find that the fiducial MHD wind and similar Genwind models, which have flows emerging outward from the inner disc ed...

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Publication status:
Published
Peer review status:
Peer reviewed

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Publisher copy:
10.1093/mnras/sty3197

Authors


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Institution:
University of Oxford
Division:
MPLS Division
Department:
Physics
Sub department:
Astrophysics
Role:
Author
ORCID:
0000-0002-3493-7737
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Role:
Author
ORCID:
0000-0003-1430-8519
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Funding agency for:
Matthews, JH
Grant:
ST/N000919/1
University of Michigan, Ann Arbor More from this funder
National Science Foundation More from this funder
Publisher:
Oxford University Press Publisher's website
Journal:
Monthly Notices of the Royal Astronomical Society Journal website
Volume:
483
Issue:
2
Pages:
1663–1673
Publication date:
2018-11-28
Acceptance date:
2018-11-21
DOI:
EISSN:
1365-2966
ISSN:
0035-8711
Source identifiers:
949586
Language:
English
Keywords:
Pubs id:
pubs:949586
UUID:
uuid:f1806b95-4259-448f-881a-b0e6c7aff2e5
Local pid:
pubs:949586
Deposit date:
2018-12-03

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