Analysis of the September ε-Perseid outburst in 2013

Abstract

We analyze the outburst experienced by the September ε-Perseid meteor shower on 9 September 2013. As a result of our monitoring the atmospheric trajectory of 60 multistation events observed over Spain was obtained and accurate orbital data were derived from them. On the basis of these orbits, we have tried to determine the likely parent body of this meteoroid stream by employing orbital dissimilarity criteria. In addition, the emission spectra produced by two events belonging to this meteor shower were also recorded. The analysis of these spectra has provided information about the chemical nature of their progenitor meteoroids. We also present an estimation of the tensile strength for these particles.

September epsilon Perseids observed by the Czech Fireball Network

“…2). Almost the same dependencies were described by Madiedo et al (2018) for video meteors. The linear dependencies in Fig.…”

“…The orbital period, P, ranges from 380 to 1100 yr with the most probable value around 720 yr. The most probable orbital periods on the basis of data published by Gajdoš et al (2014) and Madiedo et al (2018) were 70 and 200 yr, respectively. We conclude that these authors underestimated the eccentricity of the orbit.…”

“…Part B was drifted by 28 km (in nine minutes) in the azimuth of 348 • with the corresponding mean speed of 51 ms −1 , and part C was drifted by 36 km (nine minutes) in the azimuth of 7 • with the corresponding mean speed of 66 ms −1 ( (Gajdoš & Porubčan 2005). 2013-G and 2013-M are mean parameters of 2013 SPE by Gajdoš et al (2014) and Madiedo et al (2018), respectively. Values of individual entries are given with an accuracy of one last digit or with one standard deviation.…”

“…The predicted 2013 outburst peak is then September 9, 2013 at 22h15m UT. The geocentric radiant position from double-station video observations of the 2013 SPE outburst was determined by Gajdoš et al (2014) at RA = 47.6 • and Dec = 39.4 • (v G = 64.3 kms −1 ) and by Madiedo et al (2018) at RA = 47.7 • and Dec = 39.6 • (v G = 64.6 kms −1 ). The corresponding parameters of the heliocentric orbit are (q, e, i) = (0.714 AU, 0.959, 139.1 • ) (Gajdoš et al 2014) Physical properties of SPE meteors have only been studied by Madiedo et al (2018) using a sample of video meteors of brightnesses ranging from 1.8 to −6.4 absolute peak magnitude.…”

“…The geocentric radiant position from double-station video observations of the 2013 SPE outburst was determined by Gajdoš et al (2014) at RA = 47.6 • and Dec = 39.4 • (v G = 64.3 kms −1 ) and by Madiedo et al (2018) at RA = 47.7 • and Dec = 39.6 • (v G = 64.6 kms −1 ). The corresponding parameters of the heliocentric orbit are (q, e, i) = (0.714 AU, 0.959, 139.1 • ) (Gajdoš et al 2014) Physical properties of SPE meteors have only been studied by Madiedo et al (2018) using a sample of video meteors of brightnesses ranging from 1.8 to −6.4 absolute peak magnitude. They studied beginning and terminal heights and found that beginning height increases with increasing meteoroid mass and terminal height decreases with increasing meteoroid mass, which has been found earlier for other meteor showers with a cometary origin (see e.g., Koten et al 2004).…”