3D simulations of m star atmosphere velocities and their influence on molecular feh lines

Astronomy and Astrophysics

Volumn 508, Issue 3, 2009, Pages 1429-1442

  Wende, S ^a   Reiners, A ^a   Ludwig, H G ^b  

^a UNIVERSITY OF GÖTTINGEN   (Germany)

^b UNIVERSITÉ PARIS DIDEROT   (France)

Author keywords

Hydrodynamics: Stars: low mass, brown dwarfs; Line: profiles; Stars: late type; Turbulence

Indexed keywords

3D MODELS; 3D SIMULATIONS; 3D-VELOCITY; BROADENING METHOD; CONVECTIVE MOTIONS; COOL STARS; CURVE-OF-GROWTH; EARLY-TO-LATE; EFFECTIVE TEMPERATURE; EQUIVALENT WIDTH; GAUSSIAN VELOCITY PROFILE; GAUSSIANS; HYDRODYNAMIC MODEL; HYDRODYNAMIC VELOCITY; LINE BROADENING; LINE OF SIGHT; LINE SHAPE; LINE: PROFILES; M STARS; MOLECULAR LINES; PARAMETER RANGE; SLOW ROTATION; SPECTRAL SYNTHESIS; STANDARD DEVIATION; STAR STRUCTURE; STARS: LATE-TYPE; STARS: LOW-MASS , BROWN DWARFS; SYNTHESIS CODE; TURBULENT VELOCITY; VELOCITY FIELD; WEAK MAGNETIC FIELDS; STRUCTURE MODELS;

FLUID DYNAMICS; HARMONIC ANALYSIS; HYDRODYNAMICS; MAGNETIC FIELDS; SIMULATORS; SPECTROSCOPY; STARS; THREE DIMENSIONAL COMPUTER GRAPHICS; TURBULENCE; VELOCITY; CODES (SYMBOLS); THREE DIMENSIONAL;

THREE DIMENSIONAL; VELOCITY;

EID: 72849150911     PISSN: 00046361     EISSN: 14320746     Source Type: Journal    
DOI: 10.1051/0004-6361/200913149     Document Type: Article

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