On the sodium enhancement in spectra of slow meteors and the origin of Na-rich meteoroids

Matlovič, Pavol; Tóth, Juraj; Kornoš, Leonard; Loehle, Stefan

doi:10.1016/j.icarus.2020.113817

Cited by 19 publications

(6 citation statements)

References 44 publications

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“…Limits for iron and oxygen are not restrictive (oxygen especially being confounded by emission) so it is not possible to comment further on the composition of the parent body polluting Gaia J0611−6931. While it may be tempting to credit the presence of volatile emission seen for Gaia J0611−6931 to a volatile-rich nature of the parent body it is accreting, it is prudent to wait for complete disk and/or atmospheric abundances before arriving at such a conclusion (e.g., see the cautionary tale for over-interpreting gas emission strength as abundance in Matlovič et al 2020).…”

Section: Gaia J0510+2315mentioning

confidence: 99%

Serendipitous Discovery of Nine White Dwarfs With Gaseous Debris Disks

Melis,

Klein,

Doyle

et al. 2020

Preprint

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Optical spectroscopic observations of white dwarf stars selected from catalogs based on the Gaia DR2 database reveal nine new gaseous debris disks that orbit single white dwarf stars, about a factor of two increase over the previously known sample. For each source we present gas emission lines identified and basic stellar parameters, including abundances for lines seen with low-resolution spectroscopy. Principle discoveries include: (1) the coolest white dwarf (T eff ≈12,720 K) with a gas disk; this star, WD0145+234, has been reported to have undergone a recent infrared outburst; (2) co-location in velocity space of gaseous emission from multiple elements, suggesting that different elements are well-mixed; (3) highly asymmetric emission structures toward SDSS J0006+2858, and possibly asymmetric structures for two other systems; (4) an overall sample composed of approximately 25% DB and 75% DA white dwarfs, consistent with the overall distribution of primary atmospheric types found in the field population; and (5) never-before-seen emission lines from Na in the spectra of Gaia J0611−6931, semi-forbidden Mg, Ca, and Fe lines toward WD 0842+572, and Si in both stars. The currently known sample of gaseous debris disk systems is significantly skewed towards northern hemisphere stars, suggesting a dozen or so emission line stars are waiting to be found in the southern hemisphere.

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Section: Gaia J0510+2315mentioning

confidence: 99%

Serendipitous Discovery of Nine White Dwarfs With Gaseous Debris Disks

Melis,

Klein,

Doyle

et al. 2020

Preprint

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“…However, we did not find clear continuous dependency between meteor speed and Hα line intensity once the lower limit speed (v i ≈ 30 km s -1 ) was achieved. We note that a continuous dependence between the line intensity and meteor speed can be observed for other meteoric elements, most notably the volatile Na, which is favored in low velocity meteors (Borovička et al 2005;Matlovič et al 2020a).…”

Section: Hydrogen Emission In Meteors From Observational Datamentioning

confidence: 65%

Hydrogen emission from meteors and meteorites: mapping traces of H$_{2}$O molecules and organic compounds in small Solar system bodies

Matlovič,

Pisarčíková,

Tóth

et al. 2022

Preprint

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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.

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“…Cr/Na = 3.1 and Cr/Ca = 6.6. Chromium measurements were reported earlier by Russell et al (1956) and lately by Matlovič et al (2020). The measurements of Matlovič et al (2019) were obtained from laboratory measurements on meteorite samples and the high Cr value was attributed to the high values of daubreelite (FeCr2S4) and enstatite (MgSi3O).…”

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confidence: 90%

Spectral Observations at the CILBO Observatory: Calibration and Data Sets

Zender

Koschny

Rudawska

et al. 2022

Preprint

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Abstract. The Canary Island Long-Baseline Observatory (CILBO) is a double station meteor camera setup located on the Canary Islands and operated by ESA’s Meteor Research Group since 2010. Observations of meteors are obtained in the visual wavelength band by intensified video cameras from both stations, supplemented by an intensified video camera mounted with a spectral grating at one of the locations. The cameras observe during cloudless and precipitation-free nights and data are transferred to a main computer located at ESA/ESTEC once a day. The image frames that contain spectral information are calibrated, corrected, and finally processed into line intensity profiles. An ablation simulation, based on Bayesian statistics using a Markov-Chain Monte-Carlo method, allows to determine a parameter space, including the ablation temperatures, chemical elements and their corresponding line intensities, to fit against the line intensity profiles of the observed meteor spectra. The algorithm is presented in this paper and one example is discussed. Several hundred spectra have been processed and made available through the Guest Archive Facility of the Planetary Science Archive of ESA. The data format and meta-data are explained.

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On the sodium enhancement in spectra of slow meteors and the origin of Na-rich meteoroids

Cited by 19 publications

References 44 publications

Serendipitous Discovery of Nine White Dwarfs With Gaseous Debris Disks

Serendipitous Discovery of Nine White Dwarfs With Gaseous Debris Disks

Hydrogen emission from meteors and meteorites: mapping traces of H$_{2}$O molecules and organic compounds in small Solar system bodies

Spectral Observations at the CILBO Observatory: Calibration and Data Sets

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