A theory of meteors

Abstract

High Speed Molecular Impacts —The energy of impact between a molecule of atmospheric nitrogen and a meteor moving 4×10 6 em per sec is sufficient to vaporize 56 molecules of iron from the solid state to a gas at a temperature of 3000° K , or is equal to the energy of an electron dropped through about 200 volts. It is assumed that where such energies are involved, we should expect the impact to result in a miniature explosion, which would drive from 10 to 100 molecules out of the main mass of the meteor. Total Energy of a Meteor —The energy of the average meteor is observed to be dissipated within roughly 1.5 seconds after entering the upper atmosphere. It is shown that the resistance of the air to the solid mass of the meteor can account for only about one per cent of the total energy loss, and that radiation from the surface of the meteor can account for less than one per cent of the total radiation. It is concluded that most of the energy of the meteor is dissipated and changed to radiant energy by the high energy atoms and molecules which escape from the meteor and communicate their energy to the air by collision with air molecules. Development of the trail —The meteor flashes into view when the energy of molecules escaping from it is sufficient to support the radiation of the trail. Impacts between air‐molecules in the path of the meteor and escaping molecules prevent an increase in brilliancy as the meteor moves from the height of appearance to denser strata of air. At a height of about 60 to 80 km a compressed air‐cap is formed in front of the meteor which prevents further direct impacts between stationary air‐molecules and the meteor.