2010/12/14 by Richard I. Anderson, Ansgar Reiners, Anderson, Richard I. +3
Physics and Astronomy · #FOS: Physical sciences #Instrumentation and Methods for Astrophysics (astro-ph.IM) #Solar and Stellar Astrophysics (astro-ph.SR) #astro-ph.IM #astro-ph.SR
paper · pdf · doi:10.48550/arxiv.1012.2968
4 pages, 1 figure. Proceedings of the 16th Workshop on Cool Stars, Stellar Systems, and the Sun (Seattle, WA, Aug 29 - Sep 2, 2010)
arxiv created 2010/12/14 · arxiv updated 2010/12/15
We present our analysis aimed at inferring average magnetic fields in slowly-rotating solar-like stars. Using the spectral line inversion code SPINOR, we perform high-accuracy line profile fitting and investigate whether Zeeman broadening can be reliably detected in optical data of unprecedented quality. We argue that our usage of both high- and low-geff lines does provide a certain sensitivity to magnetic fields that may, indeed, be detected. However, the measurement is subject to a model dependence and prone to ambiguities, e.g. due to spectral blends. Hence, while a field may be successfully recovered, the quantification of this field is subject to large uncertainties, even for the highest-quality optical data.