scholarly journals Further measurements on isotopic anomalies of 196Hg/202Hg ratio in some of acid insoluble residues of Sikhote Alin and other iron meteorites.

1992 ◽  
Vol 26 (2) ◽  
pp. 51-61 ◽  
Author(s):  
Pradeep Kumar ◽  
P. S. Goel
2020 ◽  
Author(s):  
Ramon Brasser ◽  
Stephen Mojzsis

<p>Mass-independent isotopic anomalies in planets and meteorites define two cosmochemically distinct regions: the carbonaceous and non-carbonaceous meteorites, implying that the non-carbonaceous (terrestrial) and carbonaceous (jovian) reservoirs were kept separate during and after planet formation. The iron meteorites show a similar dichotomy.</p><p>The formation of Jupiter is widely invoked to explain this compositional dichotomy by acting as an effective barrier between the two reservoirs. Jupiter’s solid kernel possibly grew to ~20 Mearth in ~1 Myr from the accretion of sub meter-sized objects (termed “pebbles”), followed by slower accretion via planetesimals. Subsequent gas envelope contraction is thought to have led to Jupiter’s formation as a gas giant.</p><p>We show using dynamical simulations that the growth of Jupiter from pebble accretion is not fast enough to be responsible for the inferred separation of the terrestrial and jovian reservoirs. We propose instead that the dichotomy was caused by a pressure maximum in the disk near Jupiter’s location, which created a ringed structure such as those detected by the Atacama Large Millimeter/submillimeter Array(ALMA). One or multiple such long-lived pressure maxima almost completely prevented pebbles from the jovian region reaching the terrestrial zone, maintaining a compositional partition between the two regions. We thus suggest that our young solar system’s protoplanetary disk developed at least one and likely multiple rings, which potentially triggered the formation of the giant planets [1].</p><p><br>[1] Brasser, R. and Mojzsis, S.J. (2020) Nature Astronomy doi: 10.1038/s41550-019-0978-6</p>


1961 ◽  
Vol 16 (4) ◽  
pp. 379-384 ◽  
Author(s):  
Else Vilcsek ◽  
H. Wanke

Chlorine 36, which is produced by the interaction of cosmic ray particles with nuclei in meteorites, was measured in seven iron meteorites and in one stone meteorite. The decay rates for chlorine-36 in iron meteorites varied between 6.5 and 20.2 dpm/kg. From these and from the concentration of stable spallation products, the exposure ages of these meteorites were calculated. In this way we found for six of the meteorites examined exposure ages close to 500 million years. Only for the Sikhote Alin meteorite the quite different exposure age of 60 million years was measured. As this value is also definitely lower than that found by other authors for this meteorite, it is suggested that the Sikhote Alin had been part of a bigger meteorite which was broken into pieces about 60 million years ago by a collision with another meteorite.


2006 ◽  
Vol 70 (18) ◽  
pp. A668
Author(s):  
M.D. Varner ◽  
M.E. Wieser ◽  
J.R. De Laeter

2009 ◽  
Vol 73 (5) ◽  
pp. 1461-1471 ◽  
Author(s):  
J.H. Chen ◽  
D.A. Papanastassiou ◽  
G.J. Wasserburg

1988 ◽  
Vol 70 (1-2) ◽  
pp. 24
Author(s):  
J.H. Chen ◽  
G.J. Wasserburg

2008 ◽  
Vol 35 (1) ◽  
Author(s):  
David L. Cook ◽  
Robert N. Clayton ◽  
Meenakshi Wadhwa ◽  
Philip E. Janney ◽  
Andrew M. Davis

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