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Do Magnetic Fields Actually Inflate Low-Mass Stars?
Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Physics and Astronomy. Dartmouth College.ORCID iD: 0000-0002-2012-7215
Dartmouth College.
2013 (English)In: International Astronomical Union Symposium 302: Magnetic Fields Throughout Stellar Evolution / [ed] M. Jardine, P. Petit, & H. Spruit, 2013Conference paper, Published paper (Other academic)
Abstract [en]

Magnetic fields have been hypothesized to inflate the radii of low-mass stars---defined as less than 0.8 solar masses---in detached eclipsing binaries (DEBs). We evaluate this hypothesis using the magnetic Dartmouth stellar evolution code. Results suggest that magnetic suppression of thermal convection can inflate low-mass stars that possess a radiative core and convective outer envelope. A scaling relation between X-ray luminosity and surface magnetic flux indicates that model surface magnetic field strength predictions are consistent with observations. This supports the notion that magnetic fields may be inflating these stars. However, magnetic models are unable to reproduce radii of fully convective stars in DEBs. Instead, we propose that model discrepancies below the fully convective boundary are related to metallicity.

Place, publisher, year, edition, pages
2013.
Series
IAU Symposium, 302
National Category
Astronomy, Astrophysics and Cosmology
Research subject
Astronomy; Astronomy with specialization in Astrophysics
Identifiers
URN: urn:nbn:se:uu:diva-212629OAI: oai:DiVA.org:uu-212629DiVA: diva2:678580
Conference
Magnetic Fields Throughout Stellar Evolution
Available from: 2013-12-12 Created: 2013-12-12 Last updated: 2016-04-15

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Feiden, Gregory

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