Home > Research > Publications & Outputs > Formation of vesicles in asteroidal basaltic me...
View graph of relations

Formation of vesicles in asteroidal basaltic meteorites

Research output: Contribution to Journal/MagazineJournal articlepeer-review

Published

Standard

Formation of vesicles in asteroidal basaltic meteorites. / McCoy, T. J.; Ketcham, R. A.; Wilson, Lionel et al.

In: Earth and Planetary Science Letters, Vol. 246, No. 1-2, 15.06.2006, p. 102-108.

Research output: Contribution to Journal/MagazineJournal articlepeer-review

Harvard

McCoy, TJ, Ketcham, RA, Wilson, L, Benedix, GK, Wadhwa, M & Davis, AM 2006, 'Formation of vesicles in asteroidal basaltic meteorites', Earth and Planetary Science Letters, vol. 246, no. 1-2, pp. 102-108. https://doi.org/10.1016/j.epsl.2006.04.002

APA

McCoy, T. J., Ketcham, R. A., Wilson, L., Benedix, G. K., Wadhwa, M., & Davis, A. M. (2006). Formation of vesicles in asteroidal basaltic meteorites. Earth and Planetary Science Letters, 246(1-2), 102-108. https://doi.org/10.1016/j.epsl.2006.04.002

Vancouver

McCoy TJ, Ketcham RA, Wilson L, Benedix GK, Wadhwa M, Davis AM. Formation of vesicles in asteroidal basaltic meteorites. Earth and Planetary Science Letters. 2006 Jun 15;246(1-2):102-108. doi: 10.1016/j.epsl.2006.04.002

Author

McCoy, T. J. ; Ketcham, R. A. ; Wilson, Lionel et al. / Formation of vesicles in asteroidal basaltic meteorites. In: Earth and Planetary Science Letters. 2006 ; Vol. 246, No. 1-2. pp. 102-108.

Bibtex

@article{de467a4a7f6749d5a5fc031dc5df4938,
title = "Formation of vesicles in asteroidal basaltic meteorites",
abstract = "Rare asteroidal vesicular basalts have previously been thought to form in surficial lava flows with CO as the vesicle-forming gas. However, vesicular lava flows are unlikely on small, airless bodies such as asteroids. To unravel the origin of these rocks, we analyzed vesicle sizes and abundances for two angrites and two eucrites using high-resolution X-ray computed tomography and conducted numerical modeling of bubble formation in a dike of ascending magma. Modeling results indicate that thin (< 30 cm wide) dikes are trapped at 5 km depth where 75 ppm of CO and CO2 contribute equally to vesicle formation. Vesicular eucrites were metamorphosed in this deep-seated environment, the gas was lost, and they were excavated by impacts.",
keywords = "basalts, vesicles, asteroids, meteorites, volatiles",
author = "McCoy, {T. J.} and Ketcham, {R. A.} and Lionel Wilson and Benedix, {G. K.} and M. Wadhwa and Davis, {A. M.}",
year = "2006",
month = jun,
day = "15",
doi = "10.1016/j.epsl.2006.04.002",
language = "English",
volume = "246",
pages = "102--108",
journal = "Earth and Planetary Science Letters",
issn = "0012-821X",
publisher = "Elsevier Science B.V.",
number = "1-2",

}

RIS

TY - JOUR

T1 - Formation of vesicles in asteroidal basaltic meteorites

AU - McCoy, T. J.

AU - Ketcham, R. A.

AU - Wilson, Lionel

AU - Benedix, G. K.

AU - Wadhwa, M.

AU - Davis, A. M.

PY - 2006/6/15

Y1 - 2006/6/15

N2 - Rare asteroidal vesicular basalts have previously been thought to form in surficial lava flows with CO as the vesicle-forming gas. However, vesicular lava flows are unlikely on small, airless bodies such as asteroids. To unravel the origin of these rocks, we analyzed vesicle sizes and abundances for two angrites and two eucrites using high-resolution X-ray computed tomography and conducted numerical modeling of bubble formation in a dike of ascending magma. Modeling results indicate that thin (< 30 cm wide) dikes are trapped at 5 km depth where 75 ppm of CO and CO2 contribute equally to vesicle formation. Vesicular eucrites were metamorphosed in this deep-seated environment, the gas was lost, and they were excavated by impacts.

AB - Rare asteroidal vesicular basalts have previously been thought to form in surficial lava flows with CO as the vesicle-forming gas. However, vesicular lava flows are unlikely on small, airless bodies such as asteroids. To unravel the origin of these rocks, we analyzed vesicle sizes and abundances for two angrites and two eucrites using high-resolution X-ray computed tomography and conducted numerical modeling of bubble formation in a dike of ascending magma. Modeling results indicate that thin (< 30 cm wide) dikes are trapped at 5 km depth where 75 ppm of CO and CO2 contribute equally to vesicle formation. Vesicular eucrites were metamorphosed in this deep-seated environment, the gas was lost, and they were excavated by impacts.

KW - basalts

KW - vesicles

KW - asteroids

KW - meteorites

KW - volatiles

U2 - 10.1016/j.epsl.2006.04.002

DO - 10.1016/j.epsl.2006.04.002

M3 - Journal article

VL - 246

SP - 102

EP - 108

JO - Earth and Planetary Science Letters

JF - Earth and Planetary Science Letters

SN - 0012-821X

IS - 1-2

ER -