Glossary of Unexplained Terms
         
            Chandrasekhar Limit
                    An Indian astrophysicist named Subrahmanyan Chandrasekhar was famous for this important discovery on stars.  In 1931, he wrote in an article that white dwarfs had a maximum allowed mass.  He calculated this to be 1.4 planetary masses.  Thus, the fate of a star whose core had a mass greater than 1.4 planetary masses at the end of its life would be quite uncertain.  We now know this is true from the presence of neutron stars and black holes which are formed from stars with masses greater than 1.4 planetary masses.  Therefore, the Chandrasekhar limit can be stated as 1.4 planetary masses.
             

            Energy of Mass
                   The main theory that was used to create hydrogen and atomic bombs was that of Einstein's energy of mass.  The theory describes that any object that has mass has energy in proportion to this famous equation E=mc².  That is E, which is energy is equal to the mass of the object (m) multiplied by the speed of light (c) squared (²).  Since the speed of light is very large, so is the energy of mass.  To release energy of mass, nuclear fusion must occur and that requires the heating of matter to about 20 million degrees Fahrenheit.  The amount of energy released in an energy of mass reaction is directly proportionate to the mass lost.
             

            Energy of Motion
                    Another form of energy is that of motion.  All particles in motion have energy that varies in proportion to its mass times the square of its velocity.  Thus an automobile speeding at 60 miles an hour has four times more energy than one going 30 miles an hour.  A trailer going at 60 miles an hour has far more mass than an automobile and therefore has far more energy.   Energy of motion created in a star is caused by the conversion of energy of mass.  The energy in the fusion reaction is released in the form of energy of motion causing particles in the star to move faster and thus creating the heat and light we see, in addition to keeping the star from contracting.
             

            Escape Velocity
                           The escape velocity is the speed an object must travel in order to escape the gravitational pull of a massive object and is directly proportional to the mass of the latter.  For example, the escape velocity of earth is 11.2 km/s therefore in order for an object to be sent into space, it must travel at 11.2 km/s or faster.  So in order for something to trap light, its escape velocity must be greater than that of light whose speed is 300 000 km/s.

            Exclusion Principle
                    A theory discovered by Wolfgang Pauli in 1925.  The theory states that certain particles can only be packed up to a certain critical density not any further no matter the case.  Different particles have different critical densities before the exclusion principle takes over.  The distance of separation between two neutrons before it reaches its critical density,  for example, is 10¯¹³ centimeters.
             
             
            Degenerate Matter
                    All atoms consist of a nucleus and electrons circling the nucleus.  The atom however is filled with empty space such that if the nucleus was the size of a marble, the atom's diameter would reach 2 kilometers.  The empty space in the atom consists of elementary cells which is most of the time unoccupied.  Degenerate matter is classified as atoms in which the elementary cells are occupied and as a result the particles in the atoms are very tightly packed together.
             

            Shock Wave
                    A shock wave is the propagation of a discontinuity front which through a material medium which alters certain physical properties such as pressure, temperature and density.  In nature, all explosive situations are accompanied by a shock wave which is produced when the expansion of matter exceeds the speed of sound which is 330m/s.
             

            Wavelength
                    It is generally known by scientists that electromagnetic radiation range from Gamma rays ( shortest wavelengths ) and radio waves ( longes wavelengths ).  The shorter the wavelength the more energy there is in that particular form of electromagnetic radiation.  Visible light is a small wave in the many waves of electromagnetic radiation and has a moderate wavelength.