All Meteorites Are From Mars
Astronomers believe and teach that meteorites originate in the main asteroid belt where extremely infrequent collisions (astronomers calculate 1 km bodies collide approximately every 10 million years) occur causing pieces to be scattered. These bodies would have to collide again to enter Earth-approaching orbits and fall as meteorites. The presence of four distinct classes: carbonaceous chondrites; stony; stony-iron; and nickel-iron meteorites; implies that many of the meteorites originate from bodies that were large enough to become completely differentiated, like a terrestrial planet. The carbonaceous chondrites being surface rocks, the stony being mantle rocks, the stony-irons being from the mantle-core boundaries and the nickel iron from the liquid outer cores. Unfortunately, there is only one main-belt asteroid today, that is even spherical, which is Ceres. But the mass of all the objects of the main asteroid belt, lying between the orbits of Mars and Jupiter, is estimated to be about 4 percent of the mass of the Moon. Of this, Ceres comprises 32 percent of the total.
If Ceres is only 1.28% of the mass of our Moon, it is difficult to imagine that this small body could have become hot and differentiated sufficiently to have an iron core, moreover how it could collide with another body large enough to release iron from its core. The average minimum distance between 10 km diameter asteroids in the main belt is 1,000,000 km and of the half dozen space probes which have traversed the asteroid belt none recorded a single hit of any magnitude, not even a dust particle.
Some 5.7% of all meteorites found on Earth are solid nickel-iron but comprise a total mass of 300 tons. The nickel-iron meteorites can be sliced and polished to reveal Thompson or Widmannstatten patterns resulting from the formation of two types of crystals, Kamacite and Taenite. Because these patterns have never been produced in any laboratory, it is believed that they only form when the cooling rate is very slow, e.g. less than 100 degrees per million years.
Main belt asteroids are grouped into three classes based only on their general coloration, since no spectral resolution is available from solid material. These are called C (carbonaceous), S (from silicate) and M (metal-like). The extremely tentative nature of these classifications is illustrated by the following quotes from published papers:
“Theories of asteroid formation predict that objects the size of Vesta or larger should form crusts and mantles, which would be composed mainly of basaltic rock, resulting in more than half of all asteroids being composed either of basalt or olivine. Observations, however, suggest that 99 percent of the predicted basaltic material is missing.” 1
“The orbital parameters of a satellite revolving around 22 Kalliope indicate that the bulk density of this main-belt asteroid is 2.37 +/- 0.4 grams per cubic centimeter. M-type asteroids such as Kalliope are thought to be the disrupted metallic cores of differentiated bodies. The low density indicates that Kalliope cannot be predominantly composed of metal and may be composed of chondritic material with ~30% porosity.” 2
P. Descamps et al, just published a paper (Feb. Icarus) on radar observations of an M-type asteroid, Kleopatra, previously thought to be part of a metallic core, which concludes:
“This translates into a bulk density of 3.6 ± 0.4 g/cm3, which implies a macroscopic porosity for Kleopatra of 30-50%, typical of a rubble-pile asteroid.”
Meteorites cannot have come from the asteroid belt because the main asteroid belt only condensed in the last 6,000 years from material (primarily water) ejected by an enormous jet of hot gases that shot out of the crater on Jupiter out of which proto-Venus was born. Their resulting low density, porous or cinder-like nature is typical of any solid which condenses from a gas in a weightless state, as confirmed in the last two quotes above. As the unexpectedly low densities of more main belt asteroids are determined, they are explained away by the term ‘rubble piles’, that is, as a loose conglomerations of rocks. This is directly contradicted by radar images, such as that of Kleopatra, the ‘dog bone’ asteroid shown at the left. The measured low densities of the main belt asteroids do not resemble the solid rock meteorites, which consequently did not originate in the main asteroid belt.
The reason for the great number and variety of meteorites is because priori-Mars (Mars and Mercury combined) spent a total of 1500 years in a geostationary orbit only 37,000 km from the Earth between 3700 and 700 BC. It was repeatedly convulsed when passing through alignments with the Moon and the Moon/Sun combined, causing the ejection of large hot rocks from its mantle and allowing liquid nickel-iron from its outer core to boil out through volcanic vents aided by the tidal force of the nearby Earth. These convulsions carried innumerable surface rocks with them as well as dust, water, atmosphere, vegetation and seeds included in manna which fell around the globe.
The near side of the Moon is covered by several kilometers of regolith ejected from priori-Mars during the periods of cyclic catastrophism. Although Mercury only entered into its current orbit at the end of the period of cyclic catastrophism, it has become covered with even more regolith because so much of the ejected material from priori-Mars and Jupiter has gradually fallen toward the Sun. The continual impact of dust blasted from priori-Mars is evidenced by the common type of lunar rock known as a breccia returned by NASA astronauts, which comprises fine rock particles of many types cemented together by the heat generated by repeated impacts. Contrary to current beliefs, these are all Mars dust and rocks. Breccias were also formed on priori-Mars during the convulsions, so the notion that all brecciated meteorites are from the Moon is not true.
In 1976 the NASA Viking Mars landers measured the ratio of several isotopes of oxygen on Mars surface and transmitted the information to the Earth. As a result, scientists have been forced to accept the idea that the meteorites found on Earth, whose isotope ratios are similar, are from Mars. However, Mars underwent such massive convulsions, bringing the interior elements to the surface during the cyclic catastrophism, that the isotope ratios changed radically in just a few thousand years. Thus the meteorites which do not have the Viking isotope signature are thought to be from the main asteroid belt, but are actually also from Mars.
Scientists believe that nickel-iron meteorites originated from broken-up main belt asteroids, such as 216 Kalliopi and 22 Kleopatra, and have traveled billions of km to the Earth, over many millions of years. This has led to the belief that the Widmannstatten patterns can only form under ridiculously low cooling rates. But these meteorites were ejected from the outer core of priori-Mars between 3700 and 700 BC, so the patterns are not due to the long time in orbit. They are obviously due to the fact that they cooled in a weightless state.
The ancient Egyptians observed liquid iron flowing out of priori-Mars when close to the Earth. They called the meteorite iron the ‘celestial metal’, using instruments fashioned from it in a funerary ceremony called ‘touching of the mouth’ which mimicked events they observed on priori-Mars at the time of Horus’ ‘death’, i.e. its separation from the Earth. These instruments date from 3000 BC, long before the Iron Age.
So, collectors save your meteorites, they are All From Mars.
1 Than, Ker (2007). “Strange Asteroids Baffle Scientists”. space.com.
2 Margot J.; Brown M., A Low-Density M-type Asteroid in the Main Belt, Science 300