The Paris meteorite, the least altered CM chondrite so far

We have assembled data on thirteen cases of meteorite falls with accurate tracking data on atmospheric passage. In all cases we estimate the bulk strength of the object corresponding to its earliest observed or inferred fragmentation in the high atmosphere, and can compare these values with measured strengths of meteorites in the taxonomic class for that fall. In all thirteen cases the strength corresponding to earliest observed or inferred fragmentation is much less than the compressive or tensile strength reported for that class of stony meteorites. We find a more random relation between bulk sample strength and sample mass than is suggested by a commonly used empirical power law. We estimate bulk strengths on entry being characteristically of the order of 10 -1 to 10 -2 times the tensile strengths of recovered samples.

/pdf/very-low-strengths-of-interplanetary-meteoroids-and-small-29i4atjb86.pdf

Very low strengths of interplanetary meteoroids and small asteroids

The physical properties of the stone meteorites provide important clues to understanding the formation and physical evolution of material in the Solar protoplanetary disk as well providing indications of the properties of their asteroidal parent bodies. Knowledge of these properties is essential for modeling a number of Solar System processes, such as bolides in planetary atmospheres, the thermal inertia of atmosphereless solid body surfaces, and the internal physical and thermal evolution of asteroids and rock-rich icy bodies. In addition, insight into the physical properties of the asteroids is important for the design of robotic and crewed reconnaissance, lander, and sample return spacecraft missions to the asteroids. One key property is meteorite porosity, which ranges from 0% to more than 40%, similar to the range of porosities seen in asteroids. Porosity affects many of the other physical properties including thermal conductivity, speed of sound, deformation under stress, strength, and response to impact. As a result of the porosity, the properties of most stone meteorites differ significantly from those of compact terrestrial rocks, whose physical properties have been used in many models of asteroid behavior. A few physical properties, such as grain density, magnetic susceptibility, and heat capacity are not functions of porosity. Taken together, the grain density and the magnetic susceptibility can be used to classify unweathered or minimally weathered ordinary chondrites. This provides a rapid screening technique to identify heterogeneous samples, classify new samples, and identify misclassified meteorites or interlopers in strewn fields.

Physical properties of the stone meteorites: Implications for the properties of their parent bodies

The chemical composition of carbonaceous chondrites: Implications for volatile element depletion, complementarity and alteration

The concept of a cosmic-ray exposure (CRE) age for a meteorite is based on a simple but useful picture of meteorite evolution, the one-stage irradiation model. CRE ages have implications for several interrelated questions. From how many different parent bodies do meteorites come? How well do meteorites represent the population of their source region? How many distinct collisions on each parent body have created the known meteorites of each type? How often do parent bodies collide? How big and how energetic were the collisions that produced meteoroids? What factors control the CRE age of a meteorite and how do meteoroid orbits evolve through time? This chapter touches on these questions as it examines the data. In recent years, CRE ages also have become important for interpreting small variations in the abundances of stable isotopes.

Cosmic-Ray Exposure Ages of Meteorites

– The Moss meteorite is the first CO chondrite fall after a time period of 70 yr and the least terrestrially contaminated member of its group. Its cosmic-ray exposure (CRE) age (T3 ∼ 13.5 Ma; T21 ∼ 14.6 Ma) is distinct among CO chondrites and, within witnessed falls is the shortest after Lance, which we have reanalyzed. Gas retention ages are approximately 3.95 × 109 yr (U/Th-He) and approximately 4.43 × 109 yr (K/Ar), respectively. Trapped Ar, Kr, and Xe are present in Moss in abundances typical for CO chondrites, with “planetary” elemental and isotopic compositions. Presence of HL-xenon from presolar diamonds is observed in the stepwise release analysis of Lance. It may also be present in Moss, but it is difficult to ascertain in single-step bulk analyses. It follows from our new data combined with a survey of the literature that the abundance of trapped gases in CO chondrites is not a good indicator of their petrological subtype.

https://onlinelibrary.wiley.com/doi/pdf/10.1111/j.1945-5100.2010.01102.x

Noble gas record and cosmic-ray exposure history of the new CO3 chondrite Moss – Comparison with Lancé and other CO chondrite falls

Jesenice (L6)-A recent meteorite fall from Slovenia

Noble gases in two meteorites that fell in Denmark and Slovenia in 2009

The European Fireball Network (EN) has been
continuously operating since 1966 (Figure 1).
Beginning in 1995, observing stations in Germany
have been managed and operated by the DLR
Institute of Planetary Research, Berlin.
The stations in Germany are of the classical type,
consisting of cameras on a tripod, looking down and
taking images of a paraboloidal mirror. Rotating
shutters mounted in front of the camera lens provide
velocity information for the fast-moving meteors.
Cameras are equipped with film. Typically, one longexposure
image is taken every night, covering the
whole sky (Figure 1).
In 2011, 14 cameras were in regular operation. 59
fireballs on 81 photographs could be recorded,
representing an extraordinary “fireball yield”. The
number of 78 fireball co-registrations with other
central-European camera systems was extraordinary
as well. Data reduction and orbit reconstruction
(carried out at Ondřejov Observatory, P. Spurný and
team) was possible for 6 meteors. The brightest
meteor, registered on May 4, had a magnitude of -10.
In the area monitored by the cameras, one fireball
was recorded (Figure 1), following which, with high
probability, a meteorite fall occurred. Unfortunately,
due to terrain conditions within the urban area of
Berlin no meteorites could be recovered.

The European Fireball Network 2011 - Status of Cameras and Observation Results in Germany

– On April 9, 2009, at 3:00 CEST, a very bright fireball appeared over Carinthia and the Karavanke Mountains. The meteoroid entered the atmosphere at a very steep angle and disintegrated into a large number of objects. Two main objects were seen as separate fireballs up to an altitude of approximately 5 km, and witnesses reported loud explosions. Three stones were found with a total weight of approximately 3.611 kg. The measured activity of short-lived cosmogenic radionuclides clearly indicates that two specimens result from a very recent meteorite fall. All cosmogenic radionuclide concentrations suggest a rather small preatmospheric radius of 1.7 Ga (4He) and approximately 4.3 Ga (40Ar), Jesenice seems not to have been strongly affected by the catastrophic disruption of the L-chondrite parent body approximately 500 Ma ago.

https://onlinelibrary.wiley.com/doi/pdf/10.1111/j.1945-5100.2011.01191.x

Jesenice-A new meteorite fall from Slovenia

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