Line spectra and profiles for ultracool substellar objects

Details Line spectra and profiles for ultracool substellar objects Line spectra and profiles for ultracool substellar objects

Aug 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aipc..926..120j&link_type=abstract

ATOMIC PROCESSES IN PLASMAS: 15th International Conference on Atomic Processes in Plasmas. AIP Conference Proceedings, Volume 9

Physics

Radiative Transfer, Scattering, Line Shapes, Widths, And Shifts, Stellar Atmospheres, Radiative Transfer, Opacity And Line Formation, Atmospheres

Scientific paper

The pressures in the line forming regions of cool stellar and substellar objects increase dramatically with lower effective temperatures. This causes strong pressure broadening of the few remaining atomic lines, with damping wings more than 0.5 μm wide, dominating the emitted spectrum. Therefore, there is an essential need for reasonably accurate line profiles for these lines under high-pressure conditions. We show the results of model atmosphere calculations using detailed line profiles for a number of alkali resonance lines and discuss the need for additional and improved line profile for stellar and planetary atmosphere simulations.

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