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Model of flare lightcurve profile observed in soft X-rays

Published online by Cambridge University Press:  09 September 2016

Magdalena Gryciuk ,
Marek Siarkowski ,
Szymon Gburek ,
Piotr Podgorski ,
Janusz Sylwester ,
Anna Kepa  and
Tomasz Mrozek
Magdalena Gryciuk
Affiliation:
Solar Physics Division, Space Research Centre Polish Academy of Sciences, Kopernika 11, 51-622 Wroclaw, Poland email: mg@cbk.pan.wroc.pl Astronomical Institute, University of Wroclaw, Poland
Marek Siarkowski
Affiliation:
Solar Physics Division, Space Research Centre Polish Academy of Sciences, Kopernika 11, 51-622 Wroclaw, Poland email: mg@cbk.pan.wroc.pl
Szymon Gburek
Affiliation:
Solar Physics Division, Space Research Centre Polish Academy of Sciences, Kopernika 11, 51-622 Wroclaw, Poland email: mg@cbk.pan.wroc.pl
Piotr Podgorski
Affiliation:
Solar Physics Division, Space Research Centre Polish Academy of Sciences, Kopernika 11, 51-622 Wroclaw, Poland email: mg@cbk.pan.wroc.pl
Janusz Sylwester
Affiliation:
Solar Physics Division, Space Research Centre Polish Academy of Sciences, Kopernika 11, 51-622 Wroclaw, Poland email: mg@cbk.pan.wroc.pl
Anna Kepa
Affiliation:
Solar Physics Division, Space Research Centre Polish Academy of Sciences, Kopernika 11, 51-622 Wroclaw, Poland email: mg@cbk.pan.wroc.pl
Tomasz Mrozek
Affiliation:
Solar Physics Division, Space Research Centre Polish Academy of Sciences, Kopernika 11, 51-622 Wroclaw, Poland email: mg@cbk.pan.wroc.pl Astronomical Institute, University of Wroclaw, Poland
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Abstract

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We propose a new model for description of solar flare lightcurve profile observed in soft X-rays. The method assumes that single-peaked ‘regular’ flares seen in lightcurves can be fitted with the elementary time profile being a convolution of Gaussian and exponential functions. More complex, multi-peaked flares can be decomposed as a sum of elementary profiles. During flare lightcurve fitting process a linear background is determined as well. In our study we allow the background shape over the event to change linearly with time. Presented approach originally was dedicated to the soft X-ray small flares recorded by Polish spectrophotometer SphinX during the phase of very deep solar minimum of activity, between 23rd and 24th Solar Cycles. However, the method can and will be used to interpret the lightcurves as obtained by the other soft X-ray broad-band spectrometers at the time of both low and higher solar activity level. In the paper we introduce the model and present examples of fits to SphinX and GOES 1-8 Å channel observations as well.

Keywords

Sun: coronaflaresX-rays
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S320: Solar and Stellar Flares and their Effects on Planets , August 2015 , pp. 89 - 94
Copyright
Copyright © International Astronomical Union 2016 

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