Kinematic Be disk
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 units of the intensity maps are such that summing over all pixels (wavelength by wavelength) results in a spectral flux profile normalized to 1 in the continuum.Sample output file (.fits)
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)
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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.jmmc.fr/.”
- And citing the article above.
Sample files are available for the following file fields: