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• W1626761104 endingPage "108" @default.
• W1626761104 startingPage "108" @default.
• W1626761104 abstract "The magnetism and rotation of white dwarf (WD) stars are investigated in relation to a hydromagnetic dynamo operating in the progenitor during shell burning phases. The downward pumping of angular momentum in the convective envelope, in combination with the absorption of a planet or tidal spin-up from a binary companion, can trigger strong dynamo action near the core-envelope boundary. Several arguments point to the outer core as the source for a magnetic field in the WD remnant: the outer third of a $sim 0.55,M_odot$ WD is processed during the shell burning phase(s) of the progenitor; the escape of magnetic helicity through the envelope mediates the growth of (compensating) helicity in the core, as is needed to maintain a stable magnetic field in the remnant; and the intense radiation flux at the core boundary facilitates magnetic buoyancy within a relatively thick tachocline layer. The helicity flux into the growing core is driven by a dynamical imbalance with a latitude-dependent rotational stress. The magnetic field deposited in an isolated massive WD is concentrated in an outer shell of mass $lesssim 0.1,M_odot$ and can reach $sim 10,$MG. A buried toroidal field experiences moderate ohmic decay above an age $sim 0.3$ Gyr, which may lead to growth or decay of the external magnetic field. The final WD spin period is related to a critical spin rate below which magnetic activity shuts off, and core and envelope decouple; it generally sits in the range of hours to days. WD periods ranging up to a year are possible if the envelope re-expands following a late thermal pulse." @default.
• W1626761104 created "2016-06-24" @default.
• W1626761104 creator A5006526357 @default.
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• W1626761104 date "2015-08-13" @default.
• W1626761104 modified "2023-10-09" @default.
• W1626761104 title "SPIN AND MAGNETISM OF WHITE DWARFS" @default.
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• W1626761104 doi "https://doi.org/10.1088/0004-637x/809/2/108" @default.
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