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Paper: Stellar granulation
Volume: 9, Cool Stars, Stellar Systems, and the Sun: Sixth Cambridge Workshop
Page: 27
Authors: Dravins, Dainis
Abstract: Numerical simulations of the three-dimensional structure and time evolution of stellar surface convection are now feasible. Using the output from such simulations as sets of spatially and temporally varying model atmospheres, synthetic images of the stellar surface structure (granulation) as well as photospheric line profiles can be computed, and compared to observations. Such models are free from the classical ad hoc parameters of 'mixing-length', 'micro-' or 'macro-turbulence'. Challenges for the future include detailed modeling of early-type, giant, and other nonsolar type stars. Signatures of stellar granulation are primarily observed as asymmetries and wavelength shifts in photospheric absorption lines. Observational challenges include identifying such asymmetries and shifts throughout the HR-diagram, monitoring lineshift variations during stellar activity cycles, and ultimately achieving spectroscopy across spatially resolved stellar disks.
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