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The curvature of space-time as described by
Einstein in the General Theory of Relativity
creates several phenomena around massive
bodies like Black Hole’s. For example time
near a Black Hole runs slower than time far
from any source of gravity. This dilation of
time near a Black Hole works as a function of
the size of the Black Hole and the distance
from the singularity an observer is who is
experiencing this slowing of time. The
closer you approach to the event horizon the
slower and slower time dilates, and theoretical
“stops” at the actual horizon. However inside
the event horizon, time does not act in the
same way as is it does outside of the horizon,
and is therefore incredibly more complicated to understand.



The curvature of space-time as described by Einstein in the General Theory of Relativity creates several phenomena around massive bodies like Black Hole’s. For example time near a Black Hole runs slower than time far from any source of gravity. This dilation of time near a Black Hole works as a function of the size of the Black Hole and the distance from the singularity an observer is who is experiencing this slowing of time. The closer you approach to the event horizon the slower and slower time dilates, and theoretical “stops” at the actual horizon. However inside the event horizon, time does not act in the same way as is it does outside of the horizon, and is therefore incredibly more complicated to understand.	Time near a Black Hole Program S.U. Cluster Dos Version
These are two identical programs for calculating time near a Black Hole. The one uses a graphics library only supported at Syracuse University computer clusters, and the other is a boring dos version which can be run anywhere.