Broadband Imaging to Study the Spectral Distribution of Meteor Radio Afterglows. (arXiv:2103.03347v2 [astro-ph.EP] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Varghese_S/0/1/0/all/0/1">S. S. Varghese</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dowell_J/0/1/0/all/0/1">J. Dowell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Obenberger_K/0/1/0/all/0/1">K. S. Obenberger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Taylor_G/0/1/0/all/0/1">G. B. Taylor</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Malins_J/0/1/0/all/0/1">J. Malins</a>

We present observations of 86 meteor radio afterglows (MRAs) using the new
broadband imager at the Long Wavelength Array Sevilleta (LWA-SV) station. The
MRAs were detected using the all-sky images with a bandwidth up to 20 MHz. We
fit the spectra with both a power law and a log-normal function. When fit with
a power law, the spectra varied from flat to steep and the derived spectral
index distribution from the fit peaked at -1.73. When fit with a log-normal
function, the spectra exhibits turnovers at frequencies between 30-40 MHz, and
appear to be a better functional fit to the spectra. We compared the spectral
parameters from the two fitting methods with the physical properties of MRAs.
We observe a weak correlation between the log-normal turnover frequency and the
altitude of MRAs. The spectral indices from the power law fit do not show any
strong correlations with the physical properties of MRAs. However, the full
width half maximum (FWHM) duration of MRAs is correlated with the local time,
incidence angle, luminosity and optically derived kinetic energy of parent
meteoroid. Also, the average luminosity of MRAs seems to be correlated with the
kinetic energy of parent meteoroid and the altitude at which they occur.

We present observations of 86 meteor radio afterglows (MRAs) using the new
broadband imager at the Long Wavelength Array Sevilleta (LWA-SV) station. The
MRAs were detected using the all-sky images with a bandwidth up to 20 MHz. We
fit the spectra with both a power law and a log-normal function. When fit with
a power law, the spectra varied from flat to steep and the derived spectral
index distribution from the fit peaked at -1.73. When fit with a log-normal
function, the spectra exhibits turnovers at frequencies between 30-40 MHz, and
appear to be a better functional fit to the spectra. We compared the spectral
parameters from the two fitting methods with the physical properties of MRAs.
We observe a weak correlation between the log-normal turnover frequency and the
altitude of MRAs. The spectral indices from the power law fit do not show any
strong correlations with the physical properties of MRAs. However, the full
width half maximum (FWHM) duration of MRAs is correlated with the local time,
incidence angle, luminosity and optically derived kinetic energy of parent
meteoroid. Also, the average luminosity of MRAs seems to be correlated with the
kinetic energy of parent meteoroid and the altitude at which they occur.

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