2012
DOI: 10.1088/0004-637x/751/2/98
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An3He-DRIVEN INSTABILITY NEAR THE FULLY CONVECTIVE BOUNDARY

Abstract: We report on the discovery of an instability in low mass stars just above the threshold (∼ 0.35 M ⊙ ) where they are expected to be fully convective on the main sequence. Non-equilibrium 3 He burning creates a convective core, which is separated from a deep convective envelope by a small radiative zone. The steady increase in central 3 He causes the core to grow until it touches the surface convection zone, which triggers fully convective episodes in what we call the "convective kissing instability". These epi… Show more

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Cited by 39 publications
(13 citation statements)
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“…The present model builds upon many previous works, including: theoretical developments of how magnetized stellar winds remove angular momentum (Schatzman 1962;Mestel 1968;Weber & Davis 1967;Kawaler 1988;Matt et al 2012); models for the evolution of stellar spin rate in time (e.g., MacGregor & Brenner 1991;Denissenkov et al 2010;Scholz et al 2011;Reiners & Mohanty 2012;Gallet & Bouvier 2013;van Saders & Pinsonneault 2013;Brown 2014); and gyrochronology relations (Barnes 2003(Barnes , 2010Mamajek & Hillenbrand 2008;Meibom et al 2009).…”
Section: Introductionmentioning
confidence: 99%
“…The present model builds upon many previous works, including: theoretical developments of how magnetized stellar winds remove angular momentum (Schatzman 1962;Mestel 1968;Weber & Davis 1967;Kawaler 1988;Matt et al 2012); models for the evolution of stellar spin rate in time (e.g., MacGregor & Brenner 1991;Denissenkov et al 2010;Scholz et al 2011;Reiners & Mohanty 2012;Gallet & Bouvier 2013;van Saders & Pinsonneault 2013;Brown 2014); and gyrochronology relations (Barnes 2003(Barnes , 2010Mamajek & Hillenbrand 2008;Meibom et al 2009).…”
Section: Introductionmentioning
confidence: 99%
“…This 3 He instabilities are caused by stars with a thin radiative zone, slightly above the transition to fully convective stars. These instabilities can produce energy fluctuations and a dip in the luminosity function (van Saders & Pinsonneault 2012;MacDonald & Gizis 2018). In Fig.…”
Section: M-dwarfs In the Context Of Gaiamentioning
confidence: 95%
“…where ξ is a uniformly distributed random number on the interval [0, 1), t ms, 0 is the MS lifetime of the primary. We determine the MS lifetimes by interpolating the logarithmic lifetimes on a grid of stellar models run with the Yale Rotating Evolution Code with input physics described in van Saders & Pinsonneault (2011). We multiply by the second factor in Equation (4) in order to randomize exactly when the primary evolves off the main sequence to avoid any correlations of the start of mass loss between different triple systems in our sample.…”
Section: Evolutionary Phasesmentioning
confidence: 99%