Meteoritic, Asteroidal, and Theoretical Constraints on the 500 Ma Disruption of theLChondrite Parent Body

Haack, H.; Farinella, P.; Scott, E. R. D.; Keil, K.

doi:10.1006/icar.1996.0010

Cited by 81 publications

(67 citation statements)

References 32 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Nesvorný et al (2009) found a possible link between this family (located at 2.7-2.82 AU) and L ordinary chondrites. Asteroids in the Gefion family are thought to have originated after an impact event that disrupted its parent body ∼ 470 million years ago (Haack et al, 1996;Korochantseva et al, 2007). This group of objects exhibit spectral characteristics compatible with S-complex asteroids .…”

Section: Discussionmentioning

confidence: 99%

Surface composition and taxonomic classification of a group of near-Earth and Mars-crossing asteroids

Sanchez

Michelsen

Reddy

et al. 2013

Icarus

View full text Add to dashboard Cite

In the past, constraining the surface composition of near-Earth asteroids (NEAs) has been difficult due to the lack of high quality near-IR spectral data (0.7-2.5 µm) that contain mineralogically diagnostic absorption bands. Here we present visible (∼ 0.43-0.95 µm) and nearinfrared (∼ 0.7-2.5 µm) spectra of nine NEAs and five Mars-crossing asteroids (MCs). The YT1) as a V-type was made on the basis of its near-infrared spectrum since no visible spectrum is available for this asteroid. A mineralogical analysis was performed on six of the asteroids (those for which near-IR spectra were obtained or previously available). We found that three asteroids (241662 (2000 KO44), 19764 (2000 NF5), 138404 (2000) have mafic silicate compositions consistent with ordinary chondrites, while three others (4055 Magellan, 164121 (2003 YT1), 5407 (1992 AX)) are pyroxene-dominated basaltic achondrite assemblages. In the case of 5407 (1992 AX) we found that its basaltic surface composition contrasts its taxonomic classification as a S-type.

show abstract

Section: Discussionmentioning

confidence: 99%

Surface composition and taxonomic classification of a group of near-Earth and Mars-crossing asteroids

Sanchez

Michelsen

Reddy

et al. 2013

Icarus

View full text Add to dashboard Cite

show abstract

“…About 50% of the H chondrites with measured cosmic ray exposure ages have ages between 7 and 8 Myr suggesting a similar origin (Eugster et al 2006). Similarly, about two-thirds of L chondrite meteorites were heavily shocked and degassed with 39 Ar-40 Ar ages near 470 Myr (Korochantseva et al, 2007) implying a common parent body for those meteorites (Haack et al 1996).…”

Section: Asteroid "Clones" As a Natural Outcome Of Planetesimal Formamentioning

confidence: 98%

“…They are subdivided into three groups (H, L, and LL) based on variations in bulk composition, such as molecular ratios [FeO/(FeO+MgO)] in olivine and pyroxene (Mason 1963;Keil & Fredriksson 1964) and the ratio of metallic Fe to total Fe (Dodd et al 1967). Their study, along with those of other chondrite classes, has provided numerous constraints on the formation and early evolution of the solar system, including (1) the migration processes that occurred in the protoplanetary disk prior to primary accretion (i.e., planetesimal formation) and their associated timescales (Cuzzi et al 2001;Cuzzi & Weidenschilling 2006), (2) the post-(and syn-) accretional heating events (Huss et al 2006;Ghosh et al 2006), and (3) the collisional events that occurred since their accretion (Hutchison 2004;Haack et al 1996, and references therein):…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Multiple and Fast: The Accretion of Ordinary Chondrite Parent Bodies

Vernazza

Zanda

Binzel

et al. 2014

ApJ

125

View full text Add to dashboard Cite

Although petrologic, chemical, and isotopic studies of ordinary chondrites and meteorites in general have largely helped establish a chronology of the earliest events of planetesimal formation and their evolution, there are several questions that cannot be resolved via laboratory measurements and/or experiments alone. Here, we propose the rationale for several new constraints on the formation and evolution of ordinary chondrite parent bodies (and, by extension, most planetesimals) from newly available spectral measurements and mineralogical analysis of main-belt S-type asteroids (83 objects) and unequilibrated ordinary chondrite meteorites (53 samples). Based on the latter, we suggest that spectral data may be used to distinguish whether an ordinary chondrite was formed near the surface or in the interior of its parent body. If these constraints are correct, the suggested implications include that: (1) large groups of compositionally similar asteroids are a natural outcome of planetesimal formation and, consequently, meteorites within a given class can originate from multiple parent bodies; (2) the surfaces of large (up to ∼200 km) S-type main-belt asteroids mostly expose the interiors of the primordial bodies, a likely consequence of impacts by small asteroids (D < 10 km) in the early solar system; (3) the duration of accretion of the H chondrite parent bodies was likely short (instantaneous or in less than ∼10 5 yr, but certainly not as long as 1 Myr); (4) LL-like bodies formed closer to the Sun than H-like bodies, a possible consequence of the radial mixing and size sorting of chondrules in the protoplanetary disk prior to accretion.

show abstract

“…Second, the range in 21 Ne concentrations by a factor of between 11 and 12 (1.0-11.5 × 10 −8 cm 3 STP/g) requires a variation in depth of >120 cm during 2π irradiation, although the 21 Ne data alone do not constrain at what depth. Assuming that irradiation took place after the main collision event on the L-chondrite parent bodỹ 480 Ma ago (Haack et al 1996), the maximum depth of the least shielded samples is ~400 g/cm 2 , i.e., a little over 1 meter. The third (and most important) constraint is provided by the finding that the correlation of neutron-capture 36 Ar versus cosmogenic 21 Ne shows a maximum around sample #369 (Fig.…”

Section: Cosmic-ray Exposure Historymentioning

confidence: 99%

The complex exposure history of the Jiddat al Harasis 073 L‐chondrite shower

Huber

Gnos

Hofmann

et al. 2008

Meteorit & Planetary Scien

View full text Add to dashboard Cite

36 Ar is predominantly released between 1000-1200 °C. All these results are consistent with a first-stage exposure of ~65 Ma within ~20 cm of the surface of the L-chondrite parent body, followed by ejection of a 1.5-2 m large object, which was then delivered to Earth within about 0.5 and 0.7 Ma. The cosmogenic nuclide data in JaH 073 thus corroborate the trend that many of the large chondrites studied so far experienced a complex exposure history. The observed 3 He/ 21 Ne ratios of 2.5-3.0 in the most shielded samples (including those of the main mass) are lower than predicted by model calculations, but similar to the lowest values found in the large Gold Basin L-chondrite shower. The Bern plot, which gives a linear correlation for 3 He/ 21 Ne versus 22 Ne/ 21 Ne, is evidently not valid for very high shielding. Some of our measured 22 Ne/ 21 Ne ratios in JaH 073 are lower than 1.06, which is not well understood, but might be explained by loss of cosmogenic neon from shocked sodium-rich plagioclase during terrestrial weathering. The amount of trapped atmospheric argon in the JaH 073 fragments varies by almost two orders of magnitude and shows only a weak correlation with the size of the fragments, which range from <100 g to >50 kg. Finally, low concentrations of radiogenic 4 He and 40 Ar indicate incomplete degassing <1 Ga ago, probably at the main collision event on the L-chondrite parent body ~480 Ma ago.

show abstract

Meteoritic, Asteroidal, and Theoretical Constraints on the 500 Ma Disruption of theLChondrite Parent Body

Cited by 81 publications

References 32 publications

Surface composition and taxonomic classification of a group of near-Earth and Mars-crossing asteroids

Surface composition and taxonomic classification of a group of near-Earth and Mars-crossing asteroids

Multiple and Fast: The Accretion of Ordinary Chondrite Parent Bodies

The complex exposure history of the Jiddat al Harasis 073 L‐chondrite shower

Contact Info

Product

Resources

About