Astronomy and Astrophysics – Astronomy
Scientific paper
May 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21840701g&link_type=abstract
American Astronomical Society, AAS Meeting #218, #407.01; Bulletin of the American Astronomical Society, Vol. 43, 2011
Astronomy and Astrophysics
Astronomy
Scientific paper
We study the influence of the spatial resolution of solar and stellar surface magnetic field maps on global MHD solar and stellar wind models, and on a model of coronal heating and X-ray emission. For the Sun, we compare the solutions driven by a low-resolution WSO map, the same map with spatial resolution artificially increased by a refinement algorithm, and a high-resolution MDI map. We perform a similar test for the planet-bearing K1-2V star HD 189733, comparing MHD wind solutions and X-ray morphology and flux for a Zeeman-Doppler imaging magnetic map, and the same map with artificially enhanced spatial resolution. In both solar and stellar cases, the large-scale wind structure is dominated by the lower-order magnetic components and is little affected by fine-scale surface magnetic structure. Provided the low-order field is properly resolved, MHD wind models applied to solar-like stars should be reliable. Instead, the X-ray morphology is dominated by the closed loop structure between mixed polarities on smaller scales and shows significant changes between high and low resolution maps. We conclude that three-dimensional modelling of coronal X-ray emission has greater surface magnetic field spatial resolution requirements than wind modeling, and can be unreliable unless the dominant mixed polarity magnetic flux is properly resolved.
Cohen Ofer
Downs Cooper
Drake Jeremy J.
Garraffo Cecilia
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