Abstract: Two BASIC programs are provided which can be applied to
studies of stellar evolution and nuclear physics. STF is used to simulate
the birth of any star, given certain parameters. At the same time, it tests
the possibility of stellar contraction and the start of fusion. If fusion
becomes possible, STF considers the condensation a star, and it halts. If
condensation proves impossible, then no simulation of birth is given-STF
halts. The second program, STM, is composed of several sub-programs
which represent data concerning a given star. These sub-programs make
it possible to compute a sun-relative model for any star, plot an H-R
Diagram, plot the Mass to Luminosity ratio, or estimate the radius of a
star.
These programs are more applicable to CAI than actual scientific
studies, due to a simplified view of the processes involved.