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Impulsivity Parameter for Solar Flares View all abstracts by submitter

Wilmar German Fajardo Mendieta   Submitted: 2016-02-22 19:16

Three phases are typically observed during solar flares: the preflare, impulsive, and decay phases. During the impulsive phase, it is believed that the electrons and other particles are accelerated after the stored energy in the magnetic field is released by reconnection. The impulsivity of a solar flare is a quantifiable property that shows how quickly this initial energy release occurs. It is measured via the impulsivity parameter, which we define as the inverse of the overall duration of the impulsive phase. We take the latter as the raw width of the most prominent nonthermal emission of the flare. We computed this observable over a work sample of 48 M-class events that occurred during the current Solar Cycle 24 by using three different methods. The first method takes into account all of the nonthermal flare emission and gives very accurate results, while the other two just cover fixed energy intervals (30-40 keV and 25-50 keV) and are useful for fast calculations. We propose an alternative way to classify solar flares according to their impulsivity parameter values, defining three different types of impulsivity, namely, high, medium, and low. This system of classification is independent of the manner used to calculated the impulsivity parameter. Lastly, we show the relevance of this tool as a discriminator of different HXR generation processes.

Authors: W. G. Fajardo-Mendieta1,2, J.C. Martínez-Oliveros3, J.D. Alvarado-Gómez4,5, B. Calvo-Mozo1
1. Observatorio Astronómico Nacional, Universidad Nacional de Colombia, Bogotá, Colombia
2. Departamento de Física, Universidad Nacional de Colombia
3. Space Sciences Laboratory, UC Berkeley
4. European Southern Observatory
5. Universitäts-Sternwarte München, Ludwig-Maximilians-Universität
Projects: None

Publication Status: Published
Last Modified: 2016-02-22 20:42
Go to main E-Print page  Resolving the Fan-Spine Reconnection Geometry of a Small-Scale Chromospheric Jet Event with the New Solar Telescope  Structure and Stability of Magnetic Fields in Solar Active Region 12192 Based on Nonlinear Force-Free Field Modeling  Edit Entry  Download Preprint  Delete Entry 

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