By Hoffmann K.A., Chiang S.T.
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Translated and revised from the 1986 Russian version.
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Extra resources for Computaitional Fluid Dynamics (Vol. I)
Neutron stars, and hence pulsars, are formed in supernovae, the spectacular final stage of stellar evolution for stars of many times the sun’s mass. When the nuclear fuel of such a massive star is finally consumed, the resulting collapse of the stellar core produces a neutron star together with a cataclysmic explosion which expels the remaining stellar envelope. The origin of pulsars in supernova explosions explains why in 1973 at the start of my thesis it was not considered surprising that all the pulsars detected to that point were solitary stars, despite the fact that a high 50 Physics 1993 fraction of normal stars are found in orbiting multiple star systems.
And, yes, Joe’s proposal to the National Science Foundation seeking funding for a computer for this search indeed pointed out, amongst these other motivations, that the discovery of “even one example of a pulsar in a binary system” would be quite valuable as it “could yield the pulsar mass”. ) 52 Physics 1993 THE ARECIBO TELESCOPE Since pulsars are relatively weak radio sources which must be observed at high time resolution in order to resolve their individual pulses, large radio telescopes are needed to collect as much signal as possible.
The computer itself had a core memory of 16K 16 bit words. There was no floating point hardware, as all the calculations were done in scaled integer representations for speed. The teletype served for interactive input/output, while the tape drive provided the necessary data mass storage and the ability to communicate with other computers. What you can’t see in the picture is that this machine was programmed entirely in assembly language. Over 4000 statements on punch cards were eventually written for the analysis codes.