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What can magnetic early B-type stars tell us about early B-type stars in general?

  • Matthew Shultz (a1), Gregg Wade (a2), Thomas Rivinius (a3), Coralie Neiner (a4), Evelyne Alecian (a5) (a6) (a7), Véronique Petit (a8), Jason Grunhut (a9) and the MiMeS & BinaMIcS Collaborations...

Abstract

Some magnetic early B-type stars display Hα emission originating in their Centrifugal Magnetospheres (CMs). To determine the rotational and magnetic properties necessary for the onset of emission, we analyzed a large spectropolarimetric dataset for a sample of 51 B5-B0 magnetic stars. New rotational periods were found for 15 stars. We determined physical parameters, dipolar magnetic field strengths, magnetospheric parameters, and magnetic braking timescales. Hα-bright stars are more rapidly rotating, more strongly magnetized, and younger than the overall population. We use the high sensitivity of magnetic braking to the mass-loss rate to test the predictions of Vink et al. (2001) and Krtička (2014) by comparing ages t to maximum spindown ages t S, max. For stars with M * < 10 M this comparison favours the Krtička recipe. For the most massive stars, both prescriptions yield tt S, max, a discrepancy which is difficult to explain via incorrect mass-loss rates alone.

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References

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Keywords

What can magnetic early B-type stars tell us about early B-type stars in general?

  • Matthew Shultz (a1), Gregg Wade (a2), Thomas Rivinius (a3), Coralie Neiner (a4), Evelyne Alecian (a5) (a6) (a7), Véronique Petit (a8), Jason Grunhut (a9) and the MiMeS & BinaMIcS Collaborations...

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