Line formation in 3D radiation hydrodynamics simulations of red supergiants

Details Line formation in 3D radiation hydrodynamics simulations of red supergiants Line formation in 3D radiation hydrodynamics simulations of red supergiants

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006sf2a.conf..455c&link_type=abstract

SF2A-2006: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics Eds.: D. Barret, F. Casoli, G.

Astronomy and Astrophysics

Astrophysics

5

Scientific paper

We developed a 3D radiative transfer code which computes emerging spectra and monochromatic maps from radiative-hydrodynamic (RHD) simulations of red supergiant stars. Computed emerging spectra show that our RHD models qualitatively reproduce the velocity amplitude and line asymmetries in observations. However, they cannot reproduce strong and weak lines simultaneously. This is explained by the shallow thermal gradient which weakens the contrast between strong and weak lines. The non-grey treatment of opacity in RHD models is planned in the near future to solve this problem. Moreover, we are now studying the possibility to detect and measure the granulation pattern with interferometers such as VLTI/AMBER, using our monochromatic intensity maps and visibility calculations.

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