Rapid Reconnection and Field Line Topology

Parker, E. N.; Rappazzo, A. F.

doi:10.1007/978-3-319-26432-5_5

Cited by 1 publication

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“…The analysis also shows that while the larger temporal scales present multifractality, the multiscaling is lost at the smaller temporal scales. While a proper comparison would be between the observational data and synthetic time series for 171 Å emission, this initial result is important in that in this case the detailed impulsive heating mechanism is not prescribed a priori but is determined self-consistently by the development of the turbulent nonlinear dynamics as put forward in the Parker model for coronal heating (Einaudi et al 1996;Dmitruk & Gómez 1997, Velli et al 2015Parker & Rappazzo 2016).…”

Section: Summary and Discussionmentioning

confidence: 99%

Multifractal Solar Euv Intensity Fluctuations and Their Implications for Coronal Heating Models

Cadavid

Lawrence

Christian

et al. 2016

ApJ

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We investigate the scaling properties of the long-range temporal evolution and intermittency of Atmospheric Imaging Assembly/Solar Dynamics Observatoryintensity observations in four solar environments: anactive region core, a weak emission region, and two core loops. We use two approaches: the probability distribution function (PDF) of time series incrementsand multifractal detrended fluctuation analysis (MF-DFA). Noise taints the results, so we focus on the 171 Å waveband, which has the highest signal-to-noise ratio. The lags between pairs of wavebands distinguish between coronal versus transition region (TR) emission. In all physical regions studied, scaling in the range of 15-45 minutes is multifractal, and the time series are anti-persistent on average. The degree of anti-correlation in the TR time series is greater than that for coronal emission. The multifractality stems from long-term correlations in the data rather than the wide distribution of intensities. Observations in the 335 Å waveband can be described in terms of a multifractal with added noise. The multiscaling of the extreme-ultraviolet data agrees qualitatively with the radiance from a phenomenological model of impulsive bursts plus noise, and also from ohmic dissipation in a reduced magnetohydrodynamic model for coronal loop heating. The parameter space must be further explored to seek quantitative agreement. Thus, the observational "signatures" obtained by the combined tests of the PDF of increments and the MF-DFA offer strong constraints thatcan systematically discriminate among models for coronal heating.

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Section: Summary and Discussionmentioning

confidence: 99%