Geologic mapping of ejecta deposits in Oppia Quadrangle, Asteroid (4) Vesta

Garry, W. B.; Williams, D. A.; Yingst, R. A.; Mest, S. C.; Buczkowski, D. L.; Tosi, F.; Schäfer, Michael; Corre, Lucille Le; Reddy, V.; Jaumann, R.; Pieters, C. M.; Russell, C. T.; Raymond, C. A.

doi:10.1016/j.icarus.2014.08.046

Cited by 13 publications

(6 citation statements)

References 51 publications

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“…30. Vesta crater formation ages from data by Kneissl et al (2014), Krohn et al (2014, Williams et al (2014a), and Garry et al (2014). Results for the lunar-based crater count calibration by Schmedemann et al (2014) are shown as black dots, while grey dots show those ages in the asteroid-based chronology by Marchi et al (2012) andO'Brien et al (2014).…”

Section: Discussionmentioning

confidence: 99%

The Sariçiçek howardite fall in Turkey: Source crater of HED meteorites on Vesta and impact risk of Vestoids

Ünsalan

Jenniskens

Yin

et al. 2019

Meteorit & Planetary Scien

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The Saric ßic ßek howardite meteorite shower consisting of 343 documented stones occurred on September 2, 2015 in Turkey and is the first documented howardite fall. Cosmogenic isotopes show that Saric ßic ßek experienced a complex cosmic-ray exposure history, exposed during~12-14 Ma in a regolith near the surface of a parent asteroid, and that añ 1 m sized meteoroid was launched by an impact 22 AE 2 Ma ago to Earth (as did one-third of all HED meteorites). SIMS dating of zircon and baddeleyite yielded 4550.4 AE 2.5 Ma and 4553 AE 8.8 Ma crystallization ages for the basaltic magma clasts. The apatite U-Pb age of 4525 AE 17 Ma, K-Ar age of~3.9 Ga, and the U,Th-He ages of 1.8 AE 0.7 and 2.6 AE 0.3 Ga are interpreted to represent thermal metamorphic and impact-related resetting ages, respectively. Petrographic; geochemical; and O-, Cr-, and Ti-isotopic studies confirm that Saric ßic ßek belongs to the normal clan of HED meteorites. Petrographic observations and analysis of organic material indicate a small portion of carbonaceous chondrite material in the Saric ßic ßek regolith and organic contamination of the meteorite after a few days on soil. Video observations of the fall show an atmospheric entry at 17.3 AE 0.8 km s À1 from NW; fragmentations at 37, 33, 31, and 27 km altitude; and provide a pre-atmospheric orbit that is the first dynamical link between the normal HED meteorite clan and the inner Main Belt. Spectral data indicate the similarity of Saric ßic ßek with the Vesta asteroid family (V-class) spectra, a group of asteroids stretching to delivery resonances, which includes (4) Vesta. Dynamical modeling of meteoroid delivery to Earth shows that the complete disruption of ã 1 km sized Vesta family asteroid or a~10 km sized impact crater on Vesta is required to provide sufficient meteoroids ≤4 m in size to account for the influx of meteorites from this HED clan. The 16.7 km diameter Antionia impact crater on Vesta was formed on terrain of the same age as given by the 4 He retention age of Saric ßic ßek. Lunar scaling for crater production to crater counts of its ejecta blanket show it was formed~22 Ma ago.A field expedition to the area was conducted by the

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Section: Discussionmentioning

confidence: 99%

The Sariçiçek howardite fall in Turkey: Source crater of HED meteorites on Vesta and impact risk of Vestoids

Ünsalan

Jenniskens

Yin

et al. 2019

Meteorit & Planetary Scien

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“…Orange materials are widespread in the Gegania quadrangle, at 25°S-5°N 0-25°E, and in the Lucaria quadrangle, at 30°S-20°N 70-135°E (Garry et al, 2014). They are associated with ejecta, but their origin is still debated: according to LeCorre et al (2013) they have been generated by the Rheasilvia impact, whereas Garry et al (2014) propose the Oppia and Octavia impacts as possible sources.…”

Section: Lobate Orange Materialsmentioning

confidence: 99%

“…They are associated with ejecta, but their origin is still debated: according to LeCorre et al (2013) they have been generated by the Rheasilvia impact, whereas Garry et al (2014) propose the Oppia and Octavia impacts as possible sources. The Oppia crater gives the name to the quadrangle westward of Gegania: a detailed spectral analysis of this feature is reported in Tosi et al (this issue).…”

Section: Lobate Orange Materialsmentioning

confidence: 99%

Mineralogical and spectral analysis of Vesta’s Gegania and Lucaria quadrangles and comparative analysis of their key features

Longobardo

Palomba

Sanctis

et al. 2015

Icarus

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“…3 exhibit a variety of color units. Yellow areas are associated with high-reflectance crater ejecta, orange corresponds to the Oppia ejecta (see Le Corre et al, 2013;Garry et al, 2014;Tosi et al, 2015, this issue), violet highlights low-reflectance areas, and blue is associated with the ridges. As mentioned above, green intensity is controlled by the strength of band I, while red-to-blue variations correspond with steeper-to-shallower visible spectral slope.…”

Section: General Mineralogy Of Av-13 and Av-14mentioning

confidence: 99%

“…1). These quadrangles contain several geological units, and part of the Rheasilvia basin (McSween et al, 2013;Ammannito et al, 2015, this issue), the Vestalia Terra highlands (Frigeri et al, 2015a), and enigmatic ''orange'' materials (Le Corre et al, 2011;Garry et al, 2014;Tosi et al, 2015, this issue). Moreover Av-13 and Av-14 contain numerous ridges and grooves also present in other quadrangles (see Longobardo et al, 2015;McFadden et al, 2015).…”

Section: Introductionmentioning

confidence: 99%