Multi-wavelength observations of a giant flare on CN Leonis. II. Chromospheric modelling with PHOENIX

Details Multi-wavelength observations of a giant flare on CN Leonis. II. Chromospheric modelling with PHOENIX Multi-wavelength observations of a giant flare on CN Leonis. II. Chromospheric modelling with PHOENIX

Feb 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010a%26a...511a..83f&link_type=abstract

Astronomy and Astrophysics, Volume 511, id.A83

Astronomy and Astrophysics

Astrophysics

4

Stars: Atmospheres, Stars: Late-Type, Stars: Individual: Cn Leonis, Stars: Chromospheres, Stars: Flare

Scientific paper

Aims: In M dwarfs, optical emission lines and continua are sensitive to changing chromospheric conditions, e.g., during flares. To study flare conditions for an observed spectrum, a comparison to synthesised spectra from model atmospheres is needed. Methods: Using the stellar atmosphere code PHOENIX, we computed a set of 41 1D NLTE parameterised chromospheric models including the photosphere and parts of the transition region. By comparison of a linear combination of the synthesised spectra and a quiescent (observed) chromosphere to observed UVES/VLT spectra of a giant flare of the M 5.5 dwarf CN Leo (Gl406), we find the best-fitting flare model chromosphere. Results: Our model spectra give a fairly good overall description of the observed continua and emission lines. In the best-fitting model, the temperature minimum is deep in the atmosphere resulting in high electron pressure for the chromospheric flaring area. The inferred chromospheric filling factor of the flare is about 3 percent, which declines during the flare. The photospheric flare filling factor is about 0.3 percent.
Based on observations collected at the European Southern Observatory, Paranal, Chile, 077.D-0011(A) and on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA.

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