The orbit of the Dhajala meteorite

Ballabh, G. M.; Bhatnagar, A.; Bhandari, N.

doi:10.1016/0019-1035(78)90156-2

Cited by 18 publications

(8 citation statements)

References 4 publications

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“…The second one occurred in Neuschwanstein (Germany) in 2002, where an enstatite chondrite was recovered ). In addition, fifteen much less accurate orbits have been derived from visual observations (Wylie 1948;La Paz 1949;Fesenkov 1951;Krinov 1960;Folinsbee et al 1969;Levin et al 1976;Ballabh et al 1978;Brown et al 1996;Halliday and McIntosh 1990;Jenniskens et al 1992;Gounelle et al 2006). Considering that the number of reported falls and known meteorites until 1999 was respectively 1005 and 22,507 (Grady 2000), we can conclude that our knowledge on the origin of these objects is very limited.…”

Section: Contribution Of the Villalbeto De La Peña Fall To Well-knownmentioning

confidence: 99%

The Villalbeto de la Peña meteorite fall: II. Determination of atmospheric trajectory and orbit

Trigo-Rodríguez

Borovička

Spurný

et al. 2006

Meteorit & Planetary Scien

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have determined the atmospheric trajectory of the meteoroid. The initial fireball velocity, calculated from measurements of 86 video frames, was 16.9 ± 0.4 km/s. The slope of the trajectory was 29.0 ± 0.6° to the horizontal, the recorded velocity during the main fragmentation at a height of 27.9 ± 0.4 km was 14.2 ± 0.2 km/s, and the fireball terminal height was 22.2 ± 0.2 km. The heliocentric orbit of the meteoroid resided in the ecliptic plane (i = 0.0 ± 0.2°), having a perihelion distance of 0.860 ± 0.007 AU and a semimajor axis of 2.3 ± 0.2 AU. Therefore, the meteorite progenitor body came from the Main Belt, like all previous determined meteorite orbits. The Villalbeto de la Peña fireball analysis has provided the ninth known orbit of a meteorite in the solar system.

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Section: Contribution Of the Villalbeto De La Peña Fall To Well-knownmentioning

confidence: 99%

The Villalbeto de la Peña meteorite fall: II. Determination of atmospheric trajectory and orbit

Trigo-Rodríguez

Borovička

Spurný

et al. 2006

Meteorit & Planetary Scien

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“…Less precise orbits could also be deduced from visual observations for the Farmington (Kansas 1890 [Levin et al 1976]), Abee (Canada 1952 [Griffin et al 1992]), Vilna (Canada 1967 [Folinsbee et al 1969]), Murchison (Australia 1969 [Halliday and McIntosh 1990]), Dhajala (India 1976 [Ballabh et al 1978]), Omolon (Russia 1981 [Bronshten et al 1999), Mbale (Uganda 1992 [Jenniskens et al 1992]), and Pilia Kalan meteorites (India 1996 [Bhandari et al 1998]). Research on that topic anterior to 1969 is reviewed in Millman (1969) and Levin and Simonenko (1969).…”

Section: Introductionmentioning

confidence: 99%

The orbit and atmospheric trajectory of the Orgueil meteorite from historical records

Gounelle

Spurný

Bland

2006

Meteorit & Planetary Scien

116

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Abstract— Using visual observations that were reported 140 years ago in the Comptes Rendus de l'Académie des Sciences de Paris, we have determined the atmospheric trajectory and the orbit of the Orgueil meteorite, which fell May 14, 1864, near Montauban, France. Despite the intrinsic uncertainty of visual observations, we were able to calculate a reasonably precise atmospheric trajectory and a moderately precise orbit for the Orgueil meteoroid. The atmosphere entry point was ˜70 km high and the meteoroid terminal point was ˜20 km high. The calculated luminous path was ˜150 km with an entry angle of 20°. These characteristics are broadly similar to that of other meteorites for which the trajectory is known. Five out of six orbital parameters for the Orgueil orbit are well constrained. In particular, the perihelion lies inside the Earth's orbit (q ˜0.87 AU), as is expected for an Earth‐crossing meteorite, and the orbital plane is close to the ecliptic (i ˜0°). The aphelion distance (Q) depends critically on the pre‐atmospheric velocity. From the calculated atmospheric path and the fireball duration, which was reported by seven witnesses, we have estimated the pre‐atmospheric velocity to be larger than 17.8 km/sec, which corresponds to an aphelion distance Q larger than 5.2 AU, the semi‐major axis of Jupiter orbit. These results suggest that Orgueil has an orbit similar to that of Jupiter‐family comets (JFCs), although an Halley‐type comet cannot be excluded. This is at odds with other meteorites that have an asteroidal origin, but it is compatible with 140 years of data‐gathering that has established the very special nature of Orgueil compared to other meteorites. A cometary origin of the Orgueil meteorite does not contradict cosmochemistry data on CI1 chondrites. If CI1 chondrites originate from comets, it implies that comets are much more processed than previously thought and should contain secondary minerals. The forthcoming return of cometary samples by the Stardust mission will provide a unique opportunity to corroborate (or contradict) our hypothesis.

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“…Regarding the second assumption, by using this assumption, Anders (1975) and Wieler et al (1989) inferred that meteorite parent bodies are located in the asteroid belt. This is also inferred from reflectance spectra (e.g., Pieters and McFadden 1994) and calculations of meteoroid trajectories (Lowrey 1971;Levin et al 1976;Wetherill 1976;Ballabh et al 1978;Brown et al 2000), which also indicate that meteorites originate in the asteroid belt.…”

Section: Assumptions For the R P Calculationmentioning

confidence: 99%

Cosmic-ray exposure age and heliocentric distance of the parent bodies of enstatite chondrites ALH 85119 and MAC 88136

Nakashima

Nakamura

Okazaki

2006

Meteoritics &Amp; Planetary Science

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The orbit of the Dhajala meteorite

Cited by 18 publications

References 4 publications

The Villalbeto de la Peña meteorite fall: II. Determination of atmospheric trajectory and orbit

The Villalbeto de la Peña meteorite fall: II. Determination of atmospheric trajectory and orbit

The orbit and atmospheric trajectory of the Orgueil meteorite from historical records

Cosmic-ray exposure age and heliocentric distance of the parent bodies of enstatite chondrites ALH 85119 and MAC 88136

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