First radio evidence for impulsive heating contribution to the quiet solar corona. (arXiv:2004.04399v3 [astro-ph.SR] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Mondal_S/0/1/0/all/0/1">Surajit Mondal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oberoi_D/0/1/0/all/0/1">Divya Oberoi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mohan_A/0/1/0/all/0/1">Atul Mohan</a>
This letter explores the relevance of nanoflare based models for heating the
quiet sun corona. Using metrewave data from the Murchison Widefield Array, we
present the first successful detection of impulsive emissions down to flux
densities of $sim$mSFU, about two orders of magnitude weaker than earlier
attempts. These impulsive emissions have durations $lesssim 1$s and are
present throughout the quiet solar corona. The fractional time occupancy of
these impulsive emissions at a given region is $lesssim 10%$. The histograms
of these impulsive emissions follow a powerlaw distribution and show signs of
clustering at small timescales. Our estimate of the energy which must be dumped
in the corona to generate these impulsive emissions is consistent with the
coronal heating requirements. Additionally, the statistical properties of these
impulsive emissions are very similar to those recently determined for magnetic
switchbacks by the Parker Solar Probe (PSP). We hope that this work will lead
to a renewed interest in relating these weak impulsive emissions to the energy
deposited in the corona, the quantity of physical interesting from a coronal
heating perspective, and explore their relationship with the magnetic
switchbacks observed by the PSP.
This letter explores the relevance of nanoflare based models for heating the
quiet sun corona. Using metrewave data from the Murchison Widefield Array, we
present the first successful detection of impulsive emissions down to flux
densities of $sim$mSFU, about two orders of magnitude weaker than earlier
attempts. These impulsive emissions have durations $lesssim 1$s and are
present throughout the quiet solar corona. The fractional time occupancy of
these impulsive emissions at a given region is $lesssim 10%$. The histograms
of these impulsive emissions follow a powerlaw distribution and show signs of
clustering at small timescales. Our estimate of the energy which must be dumped
in the corona to generate these impulsive emissions is consistent with the
coronal heating requirements. Additionally, the statistical properties of these
impulsive emissions are very similar to those recently determined for magnetic
switchbacks by the Parker Solar Probe (PSP). We hope that this work will lead
to a renewed interest in relating these weak impulsive emissions to the energy
deposited in the corona, the quantity of physical interesting from a coronal
heating perspective, and explore their relationship with the magnetic
switchbacks observed by the PSP.
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