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Binary spiral model

Description

Phenomenological model mimicking the shock caused by the collision between the winds from massive stars (e.g. the WR and OB stars) and that results in the dusty spirals. This model provides also a reasonable match to the flux of the inner part of the spiral. Several parameters can be set in order to define the central binary and the apparent size and geometry of the dust spiral created by the wind collision.

The Binary spiral model is described in the following documents:

  • Binary spiral model documentation
  • SPHERE view of Wolf-Rayet 104., Direct detection of the Pinwheel and the link with the nearby star
    A. Soulain, F. Millour, B. Lopez, A. Matter, E. Lagadec, M. Carbillet, A. La Camera, A. Lamberts, M. Langlois, J. Milli, H. Avenhaus, Y. Magnard, A. Roux, T. Moulin, M. Carle, A. Sevin, P. Martinez, L. Abe and J. Ramos
    A&A 618, A108 (2018)
    DOI | ads

AMHRA's Binary spiral model service can be acknowledged by:

  • Mentioning “This research has made use of the Jean-Marie Mariotti Center (JMMC) — MOIO AMHRA service at https://amhra.oca.eu/.”
  • And citing the article above.

Submit your request

To submit your parameters, you can either:
  • Manually fill the fields below
  • Pre-fill the fields with default values:
  • Upload a parameters file [sample file]:

Model parameters

deg
mas
deg
deg
mas
mas
K
K
K

Image size and spectral coverage

px
mas
µm
µm