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Haiku CS20.5 - Weakened magnetic braking supported by asteroseismic rotation

Hall, O. J.; Davies, G. R.; van Saders, J.; Nielsen, M. B.; Lund, M. N.; Chaplin W. J.; Garcia, R. A.; Amard, L.; Breimann, A. A.; Khan, S.; See, V.; Tayar, J.

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<oai_dc:dc xmlns:dc="" xmlns:oai_dc="" xmlns:xsi="" xsi:schemaLocation="">
  <dc:creator>Hall, O. J.</dc:creator>
  <dc:creator>Davies, G. R.</dc:creator>
  <dc:creator>van Saders, J.</dc:creator>
  <dc:creator>Nielsen, M. B.</dc:creator>
  <dc:creator>Lund, M. N.</dc:creator>
  <dc:creator>Chaplin W. J.</dc:creator>
  <dc:creator>Garcia, R. A.</dc:creator>
  <dc:creator>Amard, L.</dc:creator>
  <dc:creator>Breimann, A. A.</dc:creator>
  <dc:creator>Khan, S.</dc:creator>
  <dc:creator>See, V.</dc:creator>
  <dc:creator>Tayar, J.</dc:creator>
  <dc:description>Studies using asteroseismic ages and rotation rates from star-spot rotation have indicated that standard age-rotation relations may break down roughly half-way through the main sequence lifetime, a phenomenon referred to as weakened magnetic braking. While rotation rates from spots can be difficult to determine for older, less active stars, rotational splitting of asteroseismic oscillation frequencies can provide rotation rates for both active and quiescent stars, and so can confirm whether this effect really takes place on the main sequence. In this talk, I’ll show how we obtained asteroseismic rotation rates of 91 main sequence stars showing high signal-to-noise modes of oscillation. Using these new rotation rates, along with effective temperatures, metallicities and seismic masses and ages, we built a hierarchical Bayesian mixture model that showed that our new ensemble more closely agreed with weakened magnetic braking, over a standard rotational evolution scenario.</dc:description>
  <dc:subject>Cool Stars on the main sequence</dc:subject>
  <dc:title>Haiku CS20.5 - Weakened magnetic braking supported by asteroseismic rotation</dc:title>
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