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Kinematic Be disk

Description

Model of the geometry (size and shape) and kinematics (rotation and expansion) of circumstellar disks, especially of Be stars. It is suited to interpret spectro-interferometric data (combination of high angular and high spectral resolutions) obtained on emission lines formed in the disk. The disk is assumed to be geometrically flat and its rotation and expansion velocities are defined by parameterized analytical laws. The intensity contribution from the continuum and line emissions are also given by parameterized laws.

The Kinematic Be disk model was created by A. Meilland.

It is described in the following article:

  • Kinematics and geometrical study of the Be stars 48 Persei and ψ Persei with the VEGA/CHARA interferometer
    O. Delaa, Ph. Stee, A. Meilland, J. Zorec, D. Mourard, Ph. Bério, D. Bonneau, O. Chesneau, J. M. Clausse, P. Cruzalebes, K. Perraut, A. Marcotto, A. Roussel, A. Spang, H. McAlister, T. ten Brummelaar, J. Sturmann, L. Sturmann, N. Turner, C. Farrington and P. J. Goldfinger
    A&A 529, A87 (2011)
    DOI | ads

AMHRA's Kinematic Be disk 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]:

Global parameters

D
Å
Å

Central star

deg
R
pc

Disk geometry in the continuum

D
deg

Disk geometry in the line

Å
D

Kinematics

km/s
km/s
km/s

Non-coherent scattering

Å