Analysis of bright Taurid fireballs and their ability to produce meteorites

Madiedo, J. M.; Ortiz, J. L.; Trigo-Rodríguez, J. M.; Dergham, J.; Castro-Tirado, A. J.; Cabrera-Caño, J.; Pujols, P.

doi:10.1016/j.icarus.2013.12.025

Cited by 26 publications

(22 citation statements)

References 30 publications

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“…The entry velocities of these meteorite falls are around 28 km/s, which is also the average speed of Taurid meteors, and very close to the cut-off velocity suggested by modeling for meteorite production (ReVelle, 1979). While the Taurids remain the most promising major meteor shower candidate for meteorite recovery (Brown et al, 2013;Madiedo et al, 2014;Brown et al, 2016), the low strengths of its meteoroids, though in the upper limits comparable to the carbonaceous chondrites, would require significant initial mass of the impacting body.…”

Section: Dynamic Pressuresupporting

confidence: 71%

Spectra and physical properties of Taurid meteoroids

Matlovič

Tóth

Rudawska

et al. 2017

Planetary and Space Science

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Taurids are an extensive stream of particles produced by comet 2P/Encke, which can be observed mainly in October and November as a series of meteor showers rich in bright fireballs. Several near-Earth asteroids have also been linked with the meteoroid complex, and recently the orbits of two carbonaceous meteorites were proposed to be related to the stream, raising interesting questions about the origin of the complex and the composition of 2P/Encke. Our aim is to investigate the nature and diversity of Taurid meteoroids by studying their spectral, orbital, and physical properties determined from video meteor observations. Here we analyze 33 Taurid meteor spectra captured during the predicted outburst in November 2015 by stations in Slovakia and Chile, including 14 multi-station observations for which the orbital elements, material strength parameters, dynamic pressures, and mineralogical densities were determined. It was found that while orbits of the 2015 Taurids show similarities with several associated asteroids, the obtained spectral and physical characteristics point towards cometary origin with highly heterogeneous content. Observed spectra exhibited large dispersion of iron content and significant Na intensity in all cases. The determined material strengths are typically cometary in the K B classification, while P E criterion is on average close to values characteristic for carbonaceous bodies. The studied meteoroids were found to break up under low dynamic pressures of 0.02 -0.10 MPa, and were characterized by low mineralogical densities of 1.3 -2.5 g cm -3 . The widest spectral classification of Taurid meteors to date is presented.

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Section: Dynamic Pressuresupporting

confidence: 71%

Spectra and physical properties of Taurid meteoroids

Matlovič

Tóth

Rudawska

et al. 2017

Planetary and Space Science

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“…This shows the break-up height and velocity for each meteoroid, together with the inferred tensile strength. The atmospheric density in equation (3) (Madiedo et al 2014a). So, the calculated strength values suggest that RGE meteoroids are composed by tough cometary materials and so their parent body must be a comet.…”

Section: Meteoroid Strengthmentioning

confidence: 99%

The ρ-Geminid meteoroid stream: orbits, spectroscopic data and implications for its parent body

Madiedo

2015

Monthly Notices of the Royal Astronomical Society

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By using an array of high-sensitivity CCD video devices and spectrographs, the activity of meteor events from the poorly-known ρ-Geminid meteoroid stream has been monitored during January 2012 and 2013. As a result of this research, the atmospheric trajectory and radiant position of 10 of these events has been obtained, but also the orbital parameters of the progenitor meteoroids and the tensile strength of these particles. The data reveal that the progenitor of this stream must be a comet. In addition, the emission spectra produced by three ρ-Geminid meteors were also recorded. These are the first ρ-Geminid spectra discussed in the scientific literature, and have provided clues about the chemical nature of these meteoroids and their parent body.

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“…The perihelion distance is 0.33 AU, and the semimajor axis is 2.2178 AU. The meteoroid bulk densities are assumed to be the same as for Taurid meteoroids ρ = 1.6 g cm −3 (Babadzhanov & Kokhirova 2009;Madiedo et al 2014). Three sizes of meteoroids, corresponding to equivalent spheres of diameters 1 mm, 1 cm, and 10 cm were studied.…”

Section: Model Parameters and Computation Detailsmentioning

confidence: 99%

Rotation of cometary meteoroids

Čapek

2014

A&A

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Aims. The rotation of meteoroids caused by gas drag during the ejection from a cometary nucleus has not been studied yet. The aim of this study is to estimate the rotational characteristics of meteoroids after their release from a comet during normal activity. Methods. The basic dependence of spin rate on ejection velocity and meteoroid size is determined analytically. A sophisticated numerical model is then applied to meteoroids ejected from the 2P/Encke comet. The meteoroid shapes are approximated by polyhedrons, which have been determined by a 3D laser scanning method of 36 terrestrial rock samples. These samples come from three distinct sets with different origins and characteristics, such as surface roughness or angularity. Two types of gas-meteoroid interactions and three gas ejection models are assumed. The rotational characteristics of ejected meteoroid population are obtained by numerical integration of equations of motion with random initial conditions and random shape selection. Results. It is proved that the results do not depend on a specific set of shape models and that they are applicable to the (unknown) shapes of real meteoroids. A simple relationship between the median of meteoroid spin frequenciesf (Hz), ejection velocities v ej (m s −1 ), and sizes D (m) is determined. For diffuse reflection of gas molecules from meteoroid's surface it reads asf 2×10 −3 v ej D −0.88 , and for specular reflection of gas molecules from meteoroid's surface it isf 5 × 10 −3 v ej D −0.88 . The distribution of spin frequencies is roughly normal on log scale, and it is relatively wide: a 2σ-interval can be described as (0.1, 10) ×f . Most of the meteoroids are non-principal axis rotators. The median angle between angular momentum vector and spin vector is 12 • . About 60% of meteoroids rotate in long-axis mode. The distribution of angular momentum vectors is not random. They are concentrated in the perpendicular direction with respect to the gas flow direction. These results have been determined for the 2P/Encke comet, but their validity is general.

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Analysis of bright Taurid fireballs and their ability to produce meteorites

Cited by 26 publications

References 30 publications

Spectra and physical properties of Taurid meteoroids

Spectra and physical properties of Taurid meteoroids

The ρ-Geminid meteoroid stream: orbits, spectroscopic data and implications for its parent body

Rotation of cometary meteoroids

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