Der Mond als Mutterkörper der Bronzit-Chondrite

1966 ◽  
Vol 21 (1-2) ◽  
pp. 93-110 ◽  
Author(s):  
H. Wänke

Knowing the cosmic ray exposure ages of a sufficiently large number of meteorites and using the earth as analyser with special assumptions, criteria can be found to distinguish between a lunar or asteroidal origin of meteorites. Several of the following arguments are based on new and unpublished results of rare gas measurements by HINTENBERGER, SCHULTZ und WÄNKE70.Bronzite-chondrites :1. Arguments for an origin near the surface of the parent body. a) Porosity of the chondrites 0—20%. b) Many bronzite-chondrites contain light primordial rare gases, originating from the exposure of the single meteorite grains to the solar wind. c) Primordial rare gas content always connected with light-dark structure. d) In the distribution of the cosmic ray exposure ages certain groupings can be distinguished. The age distribution of bronzite-chondrites with light primordial rare gases is identical with the distribution of the cosmic ray exposure ages of all bronzite-chondri-tes. The bronzite-chondrites containing primordial gas therefore are probably coming from the very upper layers, and the other bronzite-chondrites from somewhat deeper layers of their parent body.2. Arguments for an origin close to the earth’s orbit. a) Bronzite-chondrites with high cosmic ray exposure ages show a slight tendency to fall in the afternoon (noon until midnight) . b) For the bronzite-chondrites, which are morning falls (midnight until noon), diffusion losses of 3He and 4He are higher and more frequent compared to the afternoon falls. The reason for this can be found in a closer approach to the sun of the first ones. Hypersthene-chondrites do not show this effect. c) Bronzite-chondrites with light primordial rare gas content concentrate among the afternoon falls. d) The mean cosmic ray exposure age of the bronzite-chondrites is considerably lower than that of the hypersthene-chondrites.3. Arguments concerning the size of the parent body. Light primordial rare gas and their connection with light-dark structure indicate a parent body of the size of the moon or a large asteroid.None of these arguments are strictly conclusive. In some cases they are based on observations, which can only be obtained by using statistical methods. Most of these effects are close to the mean error. Adding, however, all observations together, a lunar origin of the bronzite-chondrites becomes nearly undoubtable. A lunar origin of stone meteorites was in recent times first proposed by URET 3.Hypersthene-chondrites :Hypersthene-chondrites with low cosmic ray exposure ages are rare among the morning falls. Their parent body therefore probably has to be found outside the earth’s orbit. Their distribution of the cosmic ray exposure ages may also lead to this conclusion. As proposed by ANDERS 4, the Mars asteroids could possibly be the parent bodies for the hypersthene-chondrites. Mars itself might however be considered also. A lunar origin of the hypersthene-chondrites seems to be completely out of question.

1965 ◽  
Vol 20 (8) ◽  
pp. 983-989 ◽  
Author(s):  
H. Hintenberger ◽  
H. König ◽  
L. Schultz ◽  
H. Wanke

The total content as well as the isotopic composition of helium and neon of 36 stone meteorites have been determined. Except for meteorites with primordial rare gas content, the radiogenic component of 4He has been calculated by subtracting the fourfold amount of 3He from the total 4He in order to allow for the spallation fraction of 4He. From the content of radiogenic 4He the U-Th-He-ages of the investigated meteorites have been calculated.From the content of 3He and 21Ne cosmic ray exposure ages were calculated for all meteorites also.With the new data of the 36 stone meteorites, presented in this paper, the total number of stone meteorites, of which rare gas measurements were carried out so far, amounts to 70 bronzitechondrites and 93 hypersthene-chondrites. The earlier indications for marked differences in the distribution of the U-Th-He-ages as well as for the cosmic ray exposure ages between the bronzitechondrites and the hypersthene-chondrites proved to be undoubtedly correct.During our investigations, we found Elm Creek as one additional bronzite-diondrite with high amounts of primordial rare gases. In two other bronzite-chondrites (Cavour and Dimmit) primordial rare gases were also detected, but in rather small amounts.


1964 ◽  
Vol 19 (3) ◽  
pp. 327-341 ◽  
Author(s):  
H. Hintenberger ◽  
H. König ◽  
L. Schultz ◽  
H. Wanke

The total content as well as the isotopic composition of helium and neon of 47 stone meteorites have been determined. The concentrations of 3He, 4He, 20Ne, 21Ne and 22Ne are included in the tables. For meteorite samples without primordial rare gas content, the radiogenic component of 4He has been calculated by subtracting the fourfold amount of 3He from the total 4He in order to allow for the spallation fraction of 4He. From radiogenic 4He the U-Th-He ages of the investigated meteorites have been calculated using an average uranium content of 1.1·10-8 g/g (except those cases were uranium determinations existed) and the 3.5 fold amount for thorium.The cosmic ray exposure ages were calculated using the average production rates for 3He and 21Ne derived from the decay rate of tritium and 22Na measured in some meteorites. The calculated values for the exposure ages lie between 0.5·106 years and 40· 106 years.Some of the meteorites show very low 3He/21Ne ratios which indicate diffusion loss of the spallogenic rare gases.Our results indicate differences in the distribution of the U-Th-He ages as well as of the cosmic ray exposure ages between the chondrites of the low iron group (L) and the chondrites of the high iron group (H). On the average the U-Th-He ages of the H group chondrites are considerably higher than those of the L group. In fact, there are only a few H group chondrites with low U-Th-He ages, and for most of these exceptions we show that they lost their radiogenic 4He during the time of cosmic ray exposure. The cosmic ray exposure ages of the H group chondrites are below 10 million years in 74% of the cases, while for those of the L group only 40% are below this value.Investigations on the 47 meteorites also disclosed two additional meteorites (Pultusk and Vigarano) which exhibit a high content of light primordial rare gases, as was earlier found by us for Pantar, Breitscheid and Tabor.


1962 ◽  
Vol 17 (5) ◽  
pp. 422-432 ◽  
Author(s):  
H. Voshage

The use of iron meteorites for the establishment of possible long-time variations (108 —109 years) of the cosmic ray intensity in interplanetary space is based upon the study of the production rates of nuclides which are formed by the interaction of cosmic ray particles with nuclei in meteorites. Mass spectrometric measurements of the isotopic composition of meteoritic potassium * are combined with data on cosmogenic rare gases and other elements to give K41-K40-exposure ages and rare gas production rates. The K41-K40-exposure ages are larger than the exposure ages obtained from the study of short-lived activities (e. g. Cl36, A39), by a factor 1.3 to 1.8. This result indicates that the cosmic ray intensity increased during the bombardment history of the meteorites. The data, for example, are consistent with the following assumptions: 1) The cosmic ray intensity was constant during most of the bombarding time and increased by a factor of about 1.5 only a few million years ago. 2) The intensity rose as I(t) =I0 e— γt with —1.1·10-9 ≦ γ ≦ —0.6 · 10-9 a–1. The consequences of this result for the interpretation of meteorite data are discussed.


1997 ◽  
Vol 32 (6) ◽  
pp. 891-902 ◽  
Author(s):  
KEES C. WELTEN ◽  
LOUIS LINDNER ◽  
KLAAS BORG ◽  
THOMAS LOEKEN ◽  
PETER SCHERER ◽  
...  

1971 ◽  
Vol 13 ◽  
pp. 343-343 ◽  
Author(s):  
George W. Wetherill

Monte Carlo calculations indicate excellent agreement between observed and predicted orbits of Prairie network fireballs, if it is assumed that fireballs are derived from remnants of short period comets of Jupiter’s family. No such satisfactory agreement has been found for any other proposed source. The distribution of radiants and time of fall observed for chondrites will also be reproduced by this source, provided that consideration is given to the fact that the Earth’s atmosphere will permit low velocity bodies to survive but will destroy high velocity bodies. Again, no other proposed source has been found to be adequate.It now appears likely that the mean lifetime of chondrites is limited to ˜107 yr by the high probability of complete fragmentation following impact by smaller bodies. This improves the agreement between the observed cosmic ray exposure ages and those predicted for a cometary source. This also requires some modification of the earlier discussions of alternative sources, but does not result in them becoming more satisfactory.


1965 ◽  
Vol 70 (6) ◽  
pp. 1491-1496 ◽  
Author(s):  
R. L. Fleischer ◽  
C. W. Naeser ◽  
P. B. Price ◽  
R. M. Walker ◽  
M. Maurette

2011 ◽  
Vol 46 (9) ◽  
pp. 1397-1417 ◽  
Author(s):  
Ekaterina V. KOROCHANTSEVA ◽  
Susanne P. SCHWENZER ◽  
Alexei I. BUIKIN ◽  
Jens HOPP ◽  
Ulrich OTT ◽  
...  

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