High-Velocity Impact Ejecta: Tektites and Martian Meteorites

Artemieva, N. A.

doi:10.1007/978-1-4020-6452-4_8

Cited by 10 publications

(9 citation statements)

References 78 publications

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“…The energy required for source rock melting was attributed to various processes including direct shock, jetting, bow shock, etc., by different researchers -for a review see Montanari and Koeberl (2000). Transport of melt particles from the impact site has been relatively satisfactorily, though rather qualitatively (see above), described by Artemieva et al (2002), Stö ffler et al (2002), and Artemieva (2008).…”

Section: Notes On the Moldavite Formation Processmentioning

confidence: 85%

“…A fast spreading thermal layer associated with the radiation emitted due to the terminal phase of the flight of the projectile then may help to transport tektites from the impact site. Once formed, melt was subsequently transported on ballistic trajectories at high altitudes, where it was then solidified as inferred from low gas pressure in bubbles (Artemieva, 2008).…”

Section: Notes On the Moldavite Formation Processmentioning

confidence: 99%

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Moldavites from the Cheb Basin, Czech Republic

Skála

Strnad

McCammon

et al. 2009

Geochimica et Cosmochimica Acta

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Section: Notes On the Moldavite Formation Processmentioning

confidence: 85%

Section: Notes On the Moldavite Formation Processmentioning

confidence: 99%

Moldavites from the Cheb Basin, Czech Republic

Skála

Strnad

McCammon

et al. 2009

Geochimica et Cosmochimica Acta

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“…The impact origin of LDG, dictated by the presence of the meteoric component, can be considered in two versions: (1) the formation by compression in a shock wave and subsequent decompression and ejection into the atmosphere and (2) heating by radiation from an aerial burst. The first version is similar to the formation of tektites, for which the corresponding craters were found (with the exception of Australasian tektites), and the main processes were explained by theory, including numerical simulations (see Koeberl 1990; Artemieva 2002; Stöffler et al 2002; Melosh and Artemieva 2004; Artemieva 2008). However, the source crater for LDG has not been identified.…”

Section: Introductionmentioning

confidence: 85%

Formation of Libyan Desert Glass: Numerical simulations of melting of silica due to radiation from near‐surface airbursts

Svetsov

Шувалов

Kosarev

2020

Meteorit & Planetary Scien

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Libyan Desert Glass contains meteoritic material and, therefore, its origin is most likely associated with an impact event. However, the impact crater has not been found. We performed numerical simulations of impacts of stony and cometary bodies in order to confirm the version that this glass was formed from silica heated by radiation from aerial bursts near the ground. Asteroids were treated as strengthless bodies from dunite with a density of 3.3 g cm À3 , and comets as icy bodies with a density of 1 g cm À3 . The simulations based on hydrodynamic equations included the equations of radiation transfer. Melting and vaporization of a silica target under action of radiation incident on a planar surface were modeled using a one-dimensional hydrodynamic equation of energy and equations of radiation transfer in two-flux approximation. We selected those variants of simulations in which a crater is not formed, a fireball touches the earth surface, and the area of a molten target corresponds to the area of the Libyan Desert Glass strewn field. Appropriate options include the impact of an asteroid with a diameter of 300 m, an entry speed of 35 km s À1 , and an entry angle of 8°, and cometary bodies with diameters from 150 to 300 m, speeds of 50-70 km s À1 , and entry angles from 15°to 45°. Impact options with crater formation are also discussed. The maximum depth of molten silica at ground zero reaches 10 cm with the cometary impacts and 3-4 cm with the asteroidal impact. Melting occurs during a period of time from 50 to 400 s.

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“…The transport of melt particles from the impact site has been described satisfactorily by Stöffler et al. (2002) and Artemieva (2008). Some studies indicate (e.g., Kieffer and Simonds 1980; Artemieva 2007; also reviewed by Howard 2011) that a high content of water in surface sediments of the target area can enhance the production of high‐velocity ejected melt by an order of magnitude.…”

Section: General Characteristics Of Moldavites and Their Strewn Fieldmentioning

confidence: 99%

A review of volatile compounds in tektites, and carbon content and isotopic composition of moldavite glass

Žák

Skála

Řanda

et al. 2012

Meteorit & Planetary Scien

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Abstract-Tektites, natural silica-rich glasses produced during impact events, commonly contain bubbles. The paper reviews published data on pressure and composition of a gas phase contained in the tektite bubbles and data on other volatile compounds which can be released from tektites by either high-temperature melting or by crushing or milling under vacuum. Gas extraction from tektites using high-temperature melting generally produced higher gas yield and different gas composition than the low-temperature extraction using crushing or milling under vacuum. The high-temperature extraction obviously releases volatiles not only from the bubbles, but also volatile compounds contained directly in the glass. Moreover, the gas composition can be modified by reactions between the released gases and the glass melt. Published data indicate that besides CO 2 and ⁄ or CO in the bubbles, another carbon reservoir is present directly in the tektite glass. To clarify the problem of carbon content and carbon isotopic composition of the tektite glass, three samples from the Central European tektite strewn field-moldavites-were analyzed. The samples contained only 35-41 ppm C with d 13 C values in the range from )28.5 to )29.9& VPDB. This indicates that terrestrial organic matter was a dominant carbon source during moldavite formation.

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High-Velocity Impact Ejecta: Tektites and Martian Meteorites

Cited by 10 publications

References 78 publications

Moldavites from the Cheb Basin, Czech Republic

Moldavites from the Cheb Basin, Czech Republic

Formation of Libyan Desert Glass: Numerical simulations of melting of silica due to radiation from near‐surface airbursts

A review of volatile compounds in tektites, and carbon content and isotopic composition of moldavite glass

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