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- W2896609119 abstract "The origins of the stellar magnetic fields in accreting binary systems are considered. Observations and theoretical models suggest that the M and K dwarf secondary stars should have dynamo generated magnetic fields, with surface values up to several kG, including large-scale structures. Significant magnetic fields can be generated in the fully convective secondaries, corresponding to the lower mass M dwarfs, even though these stars do not have a tachocline region. Rapid rotation of the tidally synchronized secondary together with strong convective motions leads to effective α2 dynamo action. The higher mass M dwarfs and the K dwarfs have radiative cores and hence will possess an over-shoot tachocline region connecting the core to the convective envelope. This may affect the nature of the dynamo, particularly if some differential rotation remains across this transition layer." @default.
- W2896609119 created "2018-10-26" @default.
- W2896609119 creator A5037574117 @default.
- W2896609119 date "2018-01-01" @default.
- W2896609119 modified "2023-09-27" @default.
- W2896609119 title "Stellar Magnetic Fields" @default.
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- W2896609119 doi "https://doi.org/10.1007/978-3-319-97646-4_12" @default.
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