From UB paper 49.
49.3.3 Millions upon millions of meteorites enter the atmosphere of Urantia daily, coming in at the rate of
almost two hundred miles a second.
Science has always said this. "The highest meteor velocity is about 26.1 miles per second. Higher
velocities are not possible since they exceed the escape velocity of the solar system." That's a long way
from "almost 200 miles a second."
Then I said to myself, what if the earth runs into one of these meteors?
The earth's velocity in it's orbit is about 18.6 miles per second. This adds to the maximum meteor velocity
of 26.1 miles per second to give a maximum 44.6 miles per second fall rate on the earth. That's still a long
way from 200 miles a second.
Then I said to myself, what if the meteors referred to by the UB are not in orbit around the sun.
The sun (and the solar system) is revolving about the center of the Milky Way at about 150 miles per
second. If you add this 150 mps to the 44.6 mps you get 194.6 mps, almost 200 miles per second.
But I kept looking to see if scientists had detected any of these. Finally (WHEW), in 2006, they did. When
you read below remember that 300 km/s equals 186.4 miles per second, i.e., almost 200 mps.
Detection of an intergalactic meteor particle with the 6-m telescope
Authors: V.L. Afanasiev (1), V.V. Kalenichenko (2), I.D. Karachentsev (1) ((1) Special Astrophysical
Observatory Russian Academy of Sciences (2) Astronomical Observatory, Kyiv Taras Shevchenko
(Submitted on 10 Dec 2007)
Abstract: On July 28, 2006 the 6-m telescope of the Special Astrophysical Observatory of the Russian
Academy of Sciences recorded the spectrum of a faint meteor. We confidently identify the lines of FeI and
MgI, OI, NI and molecular-nitrogen N_2 bands. The entry velocity of the meteor body into the Earth's
atmosphere estimated from radial velocity is equal to 300 km/s. The body was several tens of a millimeter
in size, like chondrules in carbon chondrites. The radiant of the meteor trajectory coincides with the sky
position of the apex of the motion of the Solar system toward the centroid of the Local Group of galaxies.
Observations of faint sporadic meteors with FAVOR TV CCD camera confirmed the radiant at a higher
than 96% confidence level. We conclude that this meteor particle is likely to be of extragalactic origin. The
following important questions remain open: (1) How metal-rich dust particles came to be in the
extragalactic space? (2) Why are the sizes of extragalactic particles larger by two orders of magnitude
(and their masses greater by six orders of magnitude) than common interstellar dust grains in our Galaxy?
(3) If extragalactic dust surrounds galaxies in the form of dust (or gas-and-dust) aureoles, can such
formations now be observed using other observational techniques (IR observations aboard Spitzer
satellite, etc.)? (4) If inhomogeneous extragalactic dust medium with the parameters mentioned above
actually exists, does it show up in the form of irregularities on the cosmic microwave background (WMAP
By Paul Herrick