MIST
Magnetosphere, Ionosphere and Solar-Terrestrial
The dependence of solar wind burst size on burst duration and its invariance across solar cycles 23 and 24
By Liz Tindale, CFSA, Department of Physics, University of Warwick, UK.
Time series of solar wind variables, such as the interplanetary magnetic field strength, are characteristically “bursty”: they take irregularly spaced excursions to values far higher than their average [Consolini et al., 1996; Hnat et al., 2002]. These bursts can be associated with a range of physical structures, from coronal mass ejections [Nieves-Chinchilla et al., 2018] and corotating interaction regions [Tsurutani et al., 2006] on large scales, down to small-scale transient structures [Viall et al., 2010] and turbulent fluctuations [Pagel and Balogh, 2002]. Over the course of the 11-year solar cycle, changing coronal activity causes the prevalence of these structures in the solar wind to vary [Behannon et al., 1989; Luhmann et al., 2002]. As energetic bursts in the solar wind are often the drivers of increased space weather activity [Gonzales et al., 1994], it is important to understand their characteristics and likelihood, as well as their variation over the solar cycle and between cycles with different peak activity levels.
Tindale et al. [2018] use data from NASA’s Wind satellite to study bursts in the time series of solar wind magnetic energy density, Poynting flux, proton density and proton temperature during 1-year intervals around the minima and maxima of solar cycles 23 and 24. For each variable, the duration of a burst and its integrated size are related via a power law; the scaling exponent of this power law is unique to each parameter, but importantly is invariant over the two solar cycles. However, the statistical distributions of burst sizes and durations do change over the solar cycle, with an increased likelihood of encountering a large burst at solar maximum. This indicates that while the likelihood of observing a burst of a given size varies with solar activity, its characteristic duration will remain the same. This result holds at all phases of the solar cycle and across a wide range of event sizes, thus providing a constraint on the possible sizes and durations of bursts that can exist in the solar wind.
For more information, please see the paper below:
Figure: Scatter plots of burst size, S, against burst duration, τD, for bursts in the time series of solar wind magnetic energy density, B2, extracted from one-year time series spanning i) the minimum of solar cycle 23, ii) the cycle 23 maximum, iii) the minimum of cycle 24, and iv) the cycle 24 maximum. The colours denote bursts extracted over increasingly high thresholds: the 75th, 85th and 95th percentiles of each B2 time series. The solid black line shows the regression of log10(S) onto log10(τD) for bursts over the 85th percentile threshold; the gradient of the regression for bursts over each threshold, alongside the 95% confidence interval, is denoted by α.