The Effect of Magnetic Variability on Stellar Angular Momentum Loss II: The Sun, 61 Cygni A, ϵ\epsilon Eridani, ξ\xi Bootis A and τ\tau Bootis A

The magnetic fields of low-mass stars are observed to be variable on decadal timescales, ranging in behaviour from cyclic to stochastic. The changing strength and geometry of the magnetic field should modify the efficiency of angular momentum loss by stellar winds, but this has not been well quantified. In Finley et al. (2018) we investigated the variability of the Sun, and calculated the time-varying angular momentum loss rate in the solar wind. In this work, we focus on four low-mass stars that have all had their surface magnetic fields mapped for multiple epochs. Using mass loss rates determined from astrospheric Lyman-$\alpha$ absorption, in conjunction with scaling relations from the MHD simulations of Finley & Matt (2018), we calculate the torque applied to each star by their magnetised stellar winds. The variability of the braking torque can be significant. For example, the largest torque for $\epsilon$ Eri is twice its decadal averaged value. This variation is comparable to that observed in the solar wind, when sparsely sampled. On average, the torques in our sample range from 0.5-1.5 times their average value. We compare these results to the torques of Matt et al. (2015), which use observed stellar rotation rates to infer the long-time averaged torque on stars. We find that our stellar wind torques are systematically lower than the long-time average values, by a factor of ~3-30. Stellar wind variability appears unable to resolve this discrepancy, implying that there remain some problems with observed wind parameters, stellar wind models, or the long-term evolution models, which have yet to be understood.Comment: 15 pages + 8 figures, accepted for publication to Ap

On the static length of relaxation and the origin of dynamic heterogeneity in fragile glass-forming liquids

The most puzzling aspect of the glass transition observed in laboratory is an apparent decoupling of dynamics from structure. In this paper we recount the implication of various theories of glass transition for the static correlation length in an attempt to reconcile the dynamic and static lengths associate with the glass problem. We argue that a more recent characterization of the static relaxation length based on the bond ordering scenario, as the typical length over which the energy fluctuations are correlated, is more consistent with, and indeed in perfect agreement with the typical linear size of the dynamically heterogeneous domains observed in deeply supercooled liquids. The correlated relaxation of bonds in terms of energy is therefore identified as the physical origin of the observed dynamic heterogeneity.Comment: 6 pages, 1 figur