Multiple electron acceleration instances during a series of solar |
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Marina Battaglia Submitted: 2021-09-28 07:10
Even small solar flares can display a surprising level of complexity
regarding their morphology and temporal evolution. Many of their properties,
such as energy release and electron acceleration can be studied using highly
complementary observations at X-ray and radio wavelengths. We present X-ray
observations from the Reuven Ramaty High Energy Solar Spectroscopic Imager
(RHESSI) and radio observations from the Karl G. Jansky Very Large Array (VLA)
of a series of GOES A3.4 to B1.6 class flares observed on 2013 April 23. The
flares, as seen in X-ray and extreme ultraviolet (EUV), originated from
multiple locations within active region NOAA 11726. A veritable zoo of
different radio emissions between 1 GHz and 2 GHz was observed co-temporally
with the X-ray flares. In addition to broad-band continuum emission, broad-band
short-lived bursts and narrow-band spikes, indicative of accelerated electrons,
were observed. However, these sources were located up to 150 arcsec away from
the flaring X-ray sources but only some of these emissions could be explained
as signatures of electrons that were accelerated near the main flare site. For
other sources, no obvious magnetic connection to the main flare site could be
found. These emissions likely originate from secondary acceleration sites
triggered by the flare, but may be due to reconnection and acceleration
completely unrelated to the co-temporally observed flare. Thanks to the
extremely high sensitivity of the VLA, not achieved with current X-ray
instrumentation, it is shown that particle acceleration happens frequently and
at multiple locations within a flaring active region.
Authors: Marina Battaglia, Rohit Sharma, Yingjie Luo, Bin Chen, Sijie Yu, Säm Krucker
Projects: RHESSI,Very Large Array (VLA)
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Publication Status: accepted for publication in ApJ
Last Modified: 2021-09-29 08:54
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