Are Magnetically Active Low-Mass M Dwarfs Completely Convective?

By D. J. Mullan, J. Macdonald. 2001

196 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/1510f86bb546207224822cd0e06fc7dcf812c613

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In Astronomy and Astrophysics

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Citations in the corpus

• METALLICITY AND TEMPERATURE INDICATORS IN M DWARF K-BAND SPECTRA: TESTING NEW AND UPDATED CALIBRATIONS WITH OBSERVATIONS OF 133 SOLAR NEIGHBORHOOD M DWARFS (2011, background): “…constraints on M dwarf parameters have been similarly difficult to achieve: accurately modeling the deep convective zones in M dwarf interiors (Mullan & MacDonald 2001; Browning 2008) and the mixture of molecules – 4 – and grains that dominate M dwarf atmospheres (Tsuji et al. 1996; Allard et…”
• The dependence of differential rotation on temperature and rotation (2004, background): “Additionally, Mullan & MacDonald (2001) have shown that the internal strength of the magnetic field can modify stellar structure significantly such that stars become fully convective at later spectral type than is predicted by standard evolution models.”
• The Habitability of Planets Orbiting M-dwarf Stars (2016, methodology): “Such spectra rely on detailed, computationally intensive modeling of convection in low-mass stellar interiors (Mullan & MacDonald, 2001; Browning, 2008) and complete lists of the complex array of molecules and grains that reside in their atmospheres (Tsuji et al., 1996; Allard et al., 2000).”
• Evolution of low-mass star and brown dwarf eclipsing binaries (2007, methodology): “Applying this criterion to LMS interiors yields field strengths >∼ 10 7 G for the inhibition of convection in the core of a 0.3 M⊙ star (Mullan & MacDonald 2001).”
• M dwarfs: effective temperatures, radii and metallicities (2008, background): “Strong magnetic fields are expected to inhibit convection, thus giving larger radii for a given Teff or lower Teff for a given radius (Mullan & MacDonald 2001).”
• Brown Dwarfs and the TW Hydrae Association (2002, background): “I note that Mullan & MacDonald (2001) have presented nonstandard interior models with strong magnetic fields, in which magnetically active L dwarfs might actually be stars.”
• Radio Observations of a Large Sample of Late M, L, and T Dwarfs: The Distribution of Magnetic Field Strengths (2006, background): “It is also possible that the magnetic field itself acts to reduce the mass at which the transition to fully convective structure takes place (Mullan & MacDonald 2001).”
• STELLAR DIAMETERS AND TEMPERATURES. II. MAIN-SEQUENCE K- AND M-STARS (2012, background): “Strong magnetic fields within the stellar interior have been shown to inhibit convection in fully convective M-type stars (Mullan & MacDonald 2001).”
• PLANET HUNTERS: A TRANSITING CIRCUMBINARY PLANET IN A QUADRUPLE STAR SYSTEM (2012, background): “This enhances their activity, which is usually manifested by modulations in the light curve produced by spots, X-ray emission, and other phenomena, and leads to the observed effects (e.g., Mullan & MacDonald 2001; Chabrier et al. 2007).”
• Accurate masses and radii of normal stars: modern results and applications (2009, background): “Some headway on this front has already been made (see, e.g., D’Antona et al. 2000; Mullan & MacDonald 2001; Chabrier et al. 2007).”
• On the Correlation between the Magnetic Activity Levels, Metallicities, and Radii of Low-Mass Stars (2007, background): “The theoretical work by Mullan & MacDonald (2001) concludes that inhibition of convection in fast-rotating stars may be the cause of their larger radii.”
• Dynamical Simulations of Magnetically Channeled Line-driven Stellar Winds. I. Isothermal, Nonrotating, Radially Driven Flow (2002, methodology): “However there have been models based on active generation in the convective core (MacGregor & Cassinelli 2003; MacGregor & Charbonneau 1999) or envelope (Mullan & MacDonald 2001, 2005).”
• The Evolution of X-Ray Emission in Young Stars (2005, background): “These issues are further discussed in Mullan & MacDonald (2001), Feigelson et al. (2003), Barnes (2003b), and Preibisch et al. (2005).”
• HOW TO CONSTRAIN YOUR M DWARF: MEASURING EFFECTIVE TEMPERATURE, BOLOMETRIC LUMINOSITY, MASS, AND RADIUS (2015, background): “The leading hypothesis is that magnetic phenomena (magneto-convection or spots) are responsible for the observed discrepancies, motivated by theoretical predictions (e.g., Mullan & MacDonald 2001) and bolstered by observational evidence (e.g., López-Morales & Shaw 2007).”
• TESTING A PREDICTIVE THEORETICAL MODEL FOR THE MASS LOSS RATES OF COOL STARS (2011, background): “0.35M⊙) are likely to be fully convective, and thus their dynamos are likely to be driven by fundamentally different processes than exist in more massive stars (Mullan & MacDonald 2001; Reiners & Basri 2007; Irwin et al. 2011).”