354 research outputs found
Thermal evolution and sintering of chondritic planetesimals IV. Temperature dependence of heat conductivity of asteroids and meteorites
Understanding the compaction and differentiation of the planetesimals and
protoplanets from the Asteroid Belt and the terrestrial planet region of the
Solar System requires a reliable modeling of their internal thermal evolution.
An important ingredient for this is a detailed knowledge of the heat
conductivity of the chondritic mixture of minerals and metal in planetesimals.
The temperature dependence of the heat conductivity is evaluated here from the
properties of its mixture components by a theoretical model. This allows to
predict the temperature dependent heat conductivity for the full range of
observed meteoritic compositions and also for possible other compositions. For
this purpose, published results on the temperature dependence of heat
conductivity of the mineral components found in chondritic material are fitted
to the model of Callaway for heat conductivity in solids by phonons. For the
Ni,Fe-alloy published laboratory data are used. The heat conductivity of
chondritic material then is calculated by means of mixing-rules. The role of
micro-cracks is studied which increase the importance of wall-scattering for
phonon-based heat conductivity. The model is applied to published data on heat
conductivity of individual chondrites. The experimental data for the dependence
of the heat conductivity on temperature can be reproduced rather well by the
model if the heat conductivity is calculated for the composition of the
meteorites. It is found that micro-cracks have a significant impact on the
temperature dependence of the heat conductivity because of their reduction of
phonon scattering length.Comment: 18 pages, 7 figures, accepted by Astronomy & Astrophysic
Ar-40 to Ar-39 ages of the large impact structures Kara and Manicouagan and their relevance to the Cretaceous-Tertiary and the Triassic-Jurassic boundary
Since the discovery of the Ir enrichment in Cretaceous-Tertiary boundary clays in 1980, the effects of a 10-km asteroid impacting on the Earth 65 Ma ago have been discussed as the possible reason for the mass extinction--including the extinction of the dinosaurs--at the end of the Cretaceous. But up to now no crater of this age that is large enough (ca. 200 km in diameter) has been found. One candidate is the Kara Crater in northern Siberia. Kolesnikov et al. determined a K-Ar isochron of 65.6 +/- 0.5 Ma, indistinguishable from the age of the K-T boundary and interpreted this as confirmation of earlier proposals that the Kara bolide would have been at least one of the K-T impactors. Koeberl et al. determined Ar-40 to Ar-39 ages ranging from 70 to 82 Ma and suggested an association to the Campanian-Maastrichtian boundary, another important extinction horizon 73 Ma ago. We dated four impact melts, KA2-306, KA2-305, SA1-302, and AN9-182. Results from the investigation are discussed
Early Thermal Evolution of Planetesimals and its Impact on Processing and Dating of Meteoritic Material
Radioisotopic ages for meteorites and their components provide constraints on
the evolution of small bodies: timescales of accretion, thermal and aqueous
metamorphism, differentiation, cooling and impact metamorphism. Realising that
the decay heat of short-lived nuclides (e.g. 26Al, 60Fe), was the main heat
source driving differentiation and metamorphism, thermal modeling of small
bodies is of utmost importance to set individual meteorite age data into the
general context of the thermal evolution of their parent bodies, and to derive
general conclusions about the nature of planetary building blocks in the early
solar system. As a general result, modelling easily explains that iron
meteorites are older than chondrites, as early formed planetesimals experienced
a higher concentration of short-lived nuclides and more severe heating.
However, core formation processes may also extend to 10 Ma after formation of
Calcium-Aluminum-rich inclusions (CAIs). A general effect of the porous nature
of the starting material is that relatively small bodies (< few km) will also
differentiate if they form within 2 Ma after CAIs. A particular interesting
feature to be explored is the possibility that some chondrites may derive from
the outer undifferentiated layers of asteroids that are differentiated in their
interiors. This could explain the presence of remnant magnetization in some
chondrites due to a planetary magnetic field.Comment: 24 pages, 9 figures, Accepted for publication as a chapter in
Protostars and Planets VI, University of Arizona Press (2014), eds. H.
Beuther, R. Klessen, C. Dullemond, Th. Hennin
Thermal history modeling of the L chondrite parent body
The radius of the L chondrite parent body, its formation time, and its
evolution history are determined by fitting theoretical models to empirical
data of radioisotopic chronometers for L chondrites. A simplified evolution
model for the L chondrite parent body is constructed considering sintering of
the initially porous material, temperature dependent heat conductivity, and an
insulating regolith layer. Such models are fitted to thermochronological data
of five meteorites for which precise data for the Hf-W and U-Pb-Pb
thermochronometers have been published. A set of parameters for the L chondrite
parent body is found that yields excellent agreement (within error bounds)
between a thermal evolution model and thermochonological data. Empirical
cooling rate data also agree with the model results within error bounds such
that there is no conflict between cooling rate data and the onion-shell model.
Two models are found to be compatible with the presently available empirical
data: One model with a radius of 115 km and a formation time of 1.89 Ma after
CAI formation, another model with 160 km radius and formation time of 1.835 Ma.
The central temperature of the smaller body remains well below the Ni,Fe-FeS
eutectic melting temperature and is consistent with the apparent non-existence
of primitive achondrites related to the L chondrites. For the bigger model
incipient melting in the central core region is predicted which opens the
possibility that primitive achondrites related to L chondrites could be found.Comment: 22 pages, 11 figures, accepted by Astronomy & Astrophysic
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Isheyevo Meteorite: Genetic link between CH and CB chondrites?
Based on the mineralogy, petrography, bulk chemical, oxygen, and nintrogen isotopic compositions and 40Ar-39Ar age, Isheyevo is genetically related to CH and CB carbonaceous chondrites and provides a link between these group of pristine meteorites
Ar-40 to Ar-39 dating of pseudotachylites from the Witwatersrand basin, South Africa, with implications for the formation of the Vredefort Dome
The formation of the Vredefort Dome, a structure in excess of 100 km in diameter and located in the approximate center of the Witwatersrand basin, is still the subject of lively geological controversy. It is widely accepted that its formation seems to have taken place in a single sudden event, herein referred to as the Vredefort event, accompanied by the release of gigantic amounts of energy. It is debated, however, whether this central event was an internal one, i.e., a cryptoexplosion triggered by volcanic or tectonic processes, or the impact of an extraterrestrial body. The results of this debate are presented
Organic matter in interstellar dust lost at the approach to the heliosphere: Exothermic chemical reactions of free radicals ignited by the Sun
Aims. We tackle the conundrums of organic materials missing from interstellar
dust when measured inside the Solar System, while undoubtedly existing in the
local interstellar cloud (LIC), which surrounds the Solar System.
Methods. We present a theoretical argument that organic compounds sublimate
almost instantaneously by exothermic reactions, when solar insolation triggers
the recombination of free radicals or the rearrangement of carbon bonds in the
compounds.
Results. It turns out that the triggering temperature lies in the range of
2050 K by considering that sublimation of organic materials takes place
beyond the so-called filtration region of interstellar neutral atoms. We find
that in-situ measurements of LIC dust in the Solar System result in an
overestimate for the gas-to-dust mass ratio of the LIC, unless the sublimation
of organic materials is taken into account. We also find that previous
measurements of interstellar pickup ions have determined the total elemental
abundances of gas and organic materials, instead of interstellar gas alone.
Conclusions. We conclude that LIC organic matter suffers from sublimation en
route to the heliosphere, implying that our understanding of LIC dust from
space missions is incomplete. Since space missions inside the orbit of Saturn
cannot give any information on the organic substances of LIC dust, one must
await a future exploration mission to the inner edge of the Oort cloud for a
thorough understanding of organic substances in the LIC. Once our model for the
sublimation of interstellar organic matter by exothermic chemical reactions of
free radicals is confirmed, the hypothesis of panspermia from the diffuse
interstellar medium is ruled out.Comment: 9 pages, 6 figures, to appear in Astronomy & Astrophysic
The formation of the solar system
The solar system started to form about 4.56 Gyr ago and despite the long
intervening time span, there still exist several clues about its formation. The
three major sources for this information are meteorites, the present solar
system structure and the planet-forming systems around young stars. In this
introduction we give an overview of the current understanding of the solar
system formation from all these different research fields. This includes the
question of the lifetime of the solar protoplanetary disc, the different stages
of planet formation, their duration, and their relative importance. We consider
whether meteorite evidence and observations of protoplanetary discs point in
the same direction. This will tell us whether our solar system had a typical
formation history or an exceptional one. There are also many indications that
the solar system formed as part of a star cluster. Here we examine the types of
cluster the Sun could have formed in, especially whether its stellar density
was at any stage high enough to influence the properties of today's solar
system. The likelihood of identifying siblings of the Sun is discussed.
Finally, the possible dynamical evolution of the solar system since its
formation and its future are considered.Comment: 36 pages, 7 figures, invited review in Physica Script
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