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Modelling UX Ori star eclipses based on spectral observations with the Nordic Optical Telescope − I. RR Tau

Grinin, V.P. ; Tambotseva, L. V. ; Djupvik, A. A. ; Gahm, Gösta ; Grenman, T. ; Weber, H. ; Bengtsson, H. ; De Angelis, H. ; Duszanowicz, G. and Heinonen, D. , et al. (2023) In Monthly Notices of the Royal Astronomical Society 524(3). p.4047-4061
Abstract
Based on observations obtained with the Nordic Optical Telescope (NOT) we investigate the spectral variability of the Herbig Ae star RR Tau. This star belongs to the UX Ori family, characterized by very deep fadings caused by the screening of the star with opaque fragments (clouds) of the protoplanetary discs. At the moments of such minima one observes strong spectral variability due to the fact that the dust cloud occults, for an observer, not only the star but also a part of the region where the emission spectrum originates. We calculated a series of obscuration models to interpret the observed variability of the H α line parameters. We consider two main obscuration scenarios: (1) the dust screen rises vertically above the circumstellar... (More)
Based on observations obtained with the Nordic Optical Telescope (NOT) we investigate the spectral variability of the Herbig Ae star RR Tau. This star belongs to the UX Ori family, characterized by very deep fadings caused by the screening of the star with opaque fragments (clouds) of the protoplanetary discs. At the moments of such minima one observes strong spectral variability due to the fact that the dust cloud occults, for an observer, not only the star but also a part of the region where the emission spectrum originates. We calculated a series of obscuration models to interpret the observed variability of the H α line parameters. We consider two main obscuration scenarios: (1) the dust screen rises vertically above the circumstellar disc, and (2) the screen intersects the line-of-sight moving azimuthally with the disc. In both cases, the model of the emission region consists of a compact magnetosphere and a magnetocentrifugal disc wind. Comparison with observations shows that the first scenario explains well the variability of the radiation flux, the equivalent width, as well as the asymmetry of the H α line during eclipses, while the second scenario explains them only partly. This permits us to suggest that in the case of RR Tau, the main causes of the eclipses are either a structured disc wind, or the charged dust lifted along the field lines of the poloidal component of the magnetic field of the circumstellar disc. (Less)
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publishing date
type
Contribution to journal
publication status
published
subject
keywords
line: formation, techniques: spectroscopic, stars: individual, RR Tau, stars: pre-main-sequence, stars: winds, outflows
in
Monthly Notices of the Royal Astronomical Society
volume
524
issue
3
pages
24 pages
publisher
Oxford University Press
external identifiers
  • scopus:85168162770
ISSN
1365-2966
DOI
10.1093/mnras/stad2108
language
English
LU publication?
no
id
20a3e46e-627b-415a-8b04-dd4fabf5d04b
date added to LUP
2024-02-25 11:49:15
date last changed
2024-02-26 13:05:34
@article{20a3e46e-627b-415a-8b04-dd4fabf5d04b,
  abstract     = {{Based on observations obtained with the Nordic Optical Telescope (NOT) we investigate the spectral variability of the Herbig Ae star RR Tau. This star belongs to the UX Ori family, characterized by very deep fadings caused by the screening of the star with opaque fragments (clouds) of the protoplanetary discs. At the moments of such minima one observes strong spectral variability due to the fact that the dust cloud occults, for an observer, not only the star but also a part of the region where the emission spectrum originates. We calculated a series of obscuration models to interpret the observed variability of the H α line parameters. We consider two main obscuration scenarios: (1) the dust screen rises vertically above the circumstellar disc, and (2) the screen intersects the line-of-sight moving azimuthally with the disc. In both cases, the model of the emission region consists of a compact magnetosphere and a magnetocentrifugal disc wind. Comparison with observations shows that the first scenario explains well the variability of the radiation flux, the equivalent width, as well as the asymmetry of the H α line during eclipses, while the second scenario explains them only partly. This permits us to suggest that in the case of RR Tau, the main causes of the eclipses are either a structured disc wind, or the charged dust lifted along the field lines of the poloidal component of the magnetic field of the circumstellar disc.}},
  author       = {{Grinin, V.P. and Tambotseva, L. V. and Djupvik, A. A. and Gahm, Gösta and Grenman, T. and Weber, H. and Bengtsson, H. and De Angelis, H. and Duszanowicz, G. and Heinonen, D. and Holmberg, G. and Karlsson, T. and Larsson, Magnus and Warell, J. and Wikander, T.}},
  issn         = {{1365-2966}},
  keywords     = {{line: formation; techniques: spectroscopic; stars: individual; RR Tau; stars: pre-main-sequence; stars: winds; outflows}},
  language     = {{eng}},
  month        = {{07}},
  number       = {{3}},
  pages        = {{4047--4061}},
  publisher    = {{Oxford University Press}},
  series       = {{Monthly Notices of the Royal Astronomical Society}},
  title        = {{Modelling UX Ori star eclipses based on spectral observations with the Nordic Optical Telescope − I. RR Tau}},
  url          = {{http://dx.doi.org/10.1093/mnras/stad2108}},
  doi          = {{10.1093/mnras/stad2108}},
  volume       = {{524}},
  year         = {{2023}},
}