Wavelet-based characterization of small-scale solar emission features at low radio frequencies

Suresh, A. ; Sharma, R. ; Oberoi, D. ; Das, S. B. ; Pankratius, V. ; Timar, B. ; Lonsdale, C. J. ; Bowman, J. D. ; Briggs, F. ; Cappallo, R. J. ; Corey, B. E. ; Deshpande, A. A. ; Emrich, D. ; Goeke, R. ; Greenhill, L. J. ; Hazelton, B. J. ; Johnston-Hollitt, M. ; Kaplan, D. L. ; Kasper, J. C. ; Kratzenberg, E. ; Lynch, M. J. ; McWhirter, S. R. ; Mitchell, D. A. ; Morales, M. F. ; Morgan, E. ; Ord, S. M. ; Prabu, T. ; Rogers, A. E. E. ; Roshi, A. ; Udaya Shankar, N. ; Srivani, K. S. ; Subrahmanyan, R. ; Tingay, S. J. ; Waterson, M. ; Wayth, R. B. ; Webster, R. L. ; Whitney, A. R. ; Williams, A. ; Williams, C. L. (2017) Wavelet-based characterization of small-scale solar emission features at low radio frequencies The Astrophysical Journal, 843 (1). Article ID 19. ISSN 0004-637X

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Official URL: http://iopscience.iop.org/article/10.3847/1538-435...

Related URL: http://dx.doi.org/10.3847/1538-4357/aa774a


Low radio frequency solar observations using the Murchison Widefield Array have recently revealed the presence of numerous weak short-lived narrowband emission features, even during moderately quiet solar conditions. These nonthermal features occur at rates of many thousands per hour in the 30.72 MHz observing bandwidth and hence necessarily require an automated approach for their detection and characterization. Here, we employ continuous wavelet transform using a mother Ricker wavelet for feature detection from the dynamic spectrum. We establish the efficacy of this approach and present the first statistically robust characterization of the properties of these features. In particular, we examine distributions of their peak flux densities, spectral spans, temporal spans and peak frequencies. We can reliably detect features weaker than 1 SFU, making them, to the best of our knowledge, the weakest bursts reported in literature. The distribution of their peak flux densities follows a power law with an index of −2.23 in the 12–155 SFU range, implying that they can provide an energetically significant contribution to coronal and chromospheric heating. These features typically last for 1–2 s and possess bandwidths of about 4–5 MHz. Their occurrence rate remains fairly flat in the 140–210 MHz frequency range. At the time resolution of the data, they appear as stationary bursts, exhibiting no perceptible frequency drift. These features also appear to ride on a broadband background continuum, hinting at the likelihood of them being weak type-I bursts.

Item Type:Article
Source:Copyright of this article belongs to American Astronomical Society.
ID Code:114369
Deposited On:21 May 2018 06:43
Last Modified:21 May 2018 06:43

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