Statistical Signatures of Nanoflare Activity. I. Monte Carlo Simulations
DRAFT VERSION FEBRUARY 28, 2019 Typeset using LATEX twocolumn style in AASTeX62 Statistical Signatures of Nanoflare Activity. I. Monte Carlo Simulations and Parameter-space Exploration D. B. JESS,1, 2 C. J. DILLON,1 M. S. KIRK,3 F. REALE,4, 5 M. MATHIOUDAKIS,1 S. D. T. GRANT,1 D. J. CHRISTIAN,2 P. H. KEYS,1 S. KRISHNA PRASAD,1 AND S. J. HOUSTON1 1Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, Belfast, BT7 1NN, UK 2Department of Physics and Astronomy, California State University Northridge, Northridge, CA 91330, USA 3NASA Goddard Space Flight Center, Code 670, Greenbelt, MD 20771, USA 4Dipartimento di Fisica & Chimica, Universita` di Palermo, Piazza del Parlamento 1, I-90134 Palermo, Italy 5INAF-Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, I-90134 Palermo, Italy (Received December 12, 2017; Revised February 28, 2019; Accepted February 28, 2019) ABSTRACT Small-scale magnetic reconnection processes, in the form of nanoflares, have become increasingly hypoth- esized as important mechanisms for the heating of the solar atmosphere, for driving propagating disturbances along magnetic field lines in the Sun’s corona, and for instigating rapid jet-like bursts in the chromosphere. Un- fortunately, the relatively weak signatures associated with nanoflares places them below the sensitivities of cur- rent observational instrumentation. Here, we employ Monte Carlo techniques to synthesize realistic nanoflare intensity time series from a dense grid of power-law indices and decay timescales. Employing statistical tech- niques, which examine the modeled intensity fluctuations with more than 107 discrete measurements, we show how it is possible to extract and quantify nanoflare characteristics throughout the solar atmosphere, even in the presence of significant photon noise.
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