Abstract:Aims. Prior to 2019, the June epsilon Ophiuchids (JEO) were known as a minor unconfirmed meteor shower with activity that was considered typically moderate for bright fireballs. An unexpected bout of enhanced activity was observed in June 2019, which even raised the possibility that it was linked to the impact of the small asteroid 2019 MO near Puerto Rico. Early reports also point out the similarity of the shower to the orbit of the comet 300P/Catalina. We aim to analyze the orbits, emission spectra, and mate… Show more
“…The meteor and meteor spectra observations used in this work were captured by the global All-sky Meteor Orbit System (AMOS) network. The AMOS network, operated by the Comenius University in Bratislava, currently consists of 14 standard AMOS systems providing trajectory and orbital data (Tóth et al 2015(Tóth et al , 2019 and 8 spectral systems AMOS-Spec providing spectral data (Rudawska et al 2016;Matlovič et al 2019Matlovič et al , 2020b. AMOS systems are located at five stations in Slovakia, two stations in the Canary Islands, two stations in Chile, two stations in Hawaii and three stations in Australia.…”
The hydrogen emission from meteors is assumed to originate mainly from the meteoroid composition, making it a potential tracer of H 2 O molecules and organic compounds. Hα line was previously detected in individual fireballs, but its variation in a larger meteor dataset and dependency on the dynamical origin and physical properties have not yet been studied. Here we investigate the relative intensity of Hα within 304 meteor spectra observed by the AMOS network. We demonstrate that Hα emission is favored in faster meteors (v i >> 30 km s -1 ) which form the high-temperature spectral component. Hα was found to be a characteristic spectral feature of cometary meteoroids with ∼ 92% of all meteoroids with detected Hα originating from Halleytype and long-period orbits. Our results suggest that hydrogen is being depleted from meteoroids with lower perihelion distances (q < 0.4 au). No asteroidal meteoroids with detected H emission were found. However, using spectral data from simulated ablation of different meteorite types, we show that H emission from asteroidal materials can occur, and apparently correlates with their water and organic matter content. Strongest H emission was detected from carbonaceous chondrites (CM and CV) and achondrites (ureilite and aubrite), while it was lacking in most ordinary chondrites. The detection of Hα in asteroidal meteoroids could be used to identify meteoroids of carbonaceous or achondritic composition. Overall, our results suggest that Hα emission correlates with the emission of other volatiles (Na and CN) and presents a suitable tracer of water and organic matter in meteoroids.
“…The meteor and meteor spectra observations used in this work were captured by the global All-sky Meteor Orbit System (AMOS) network. The AMOS network, operated by the Comenius University in Bratislava, currently consists of 14 standard AMOS systems providing trajectory and orbital data (Tóth et al 2015(Tóth et al , 2019 and 8 spectral systems AMOS-Spec providing spectral data (Rudawska et al 2016;Matlovič et al 2019Matlovič et al , 2020b. AMOS systems are located at five stations in Slovakia, two stations in the Canary Islands, two stations in Chile, two stations in Hawaii and three stations in Australia.…”
The hydrogen emission from meteors is assumed to originate mainly from the meteoroid composition, making it a potential tracer of H 2 O molecules and organic compounds. Hα line was previously detected in individual fireballs, but its variation in a larger meteor dataset and dependency on the dynamical origin and physical properties have not yet been studied. Here we investigate the relative intensity of Hα within 304 meteor spectra observed by the AMOS network. We demonstrate that Hα emission is favored in faster meteors (v i >> 30 km s -1 ) which form the high-temperature spectral component. Hα was found to be a characteristic spectral feature of cometary meteoroids with ∼ 92% of all meteoroids with detected Hα originating from Halleytype and long-period orbits. Our results suggest that hydrogen is being depleted from meteoroids with lower perihelion distances (q < 0.4 au). No asteroidal meteoroids with detected H emission were found. However, using spectral data from simulated ablation of different meteorite types, we show that H emission from asteroidal materials can occur, and apparently correlates with their water and organic matter content. Strongest H emission was detected from carbonaceous chondrites (CM and CV) and achondrites (ureilite and aubrite), while it was lacking in most ordinary chondrites. The detection of Hα in asteroidal meteoroids could be used to identify meteoroids of carbonaceous or achondritic composition. Overall, our results suggest that Hα emission correlates with the emission of other volatiles (Na and CN) and presents a suitable tracer of water and organic matter in meteoroids.
“…In the High Enthalpy Flow Diagnostics Group (HEFDiG) of the Institute of Space Systems at the University of Stuttgart, meteoroid entry scenarios are investigated in order to provide datasets needed by observers and meteor physicists and to support the fundamental study of meteoroids. The recording of meteor spectra helps in understanding the elemental composition of meteoroids 7 and possible estimation of their trajectory and orbital parameters 8 and ultimately identifying their parent bodies such as asteroids and comets. Meteor spectra have been recorded by direct observation during meteor showers and by constant monitoring of the night sky, for example, using the global All-sky Meteor Orbit System (AMOS) meteor network 9 and at a few other locations across the world.…”
Section: Meteorite Ablation In Plasma Wind Tunnelsmentioning
Absolute x-ray calibration of a gated x-ray framing camera for the Laser MegaJoule facility in the 0.1 keV-1 keV spectral range Review of Scientific Instruments 92, 035101 (2021);
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