To overcome degeneracy in a transportation problem, one common approach is to introduce a small positive epsilon value to the supply or demand values, ensuring that all basic variables are positive. Alternatively, the Modified Distribution Method (MODI) can be used to identify and adjust the solution, allowing for a feasible solution without degeneracy. Ensuring that there are enough routes or allocations can also help in resolving any issues that arise from degeneracy.
Degeneracy in a transport problem arises when the number of occupied cells is less then: (number of columns + number of rows)-1
Degeneracy in transportation problems occurs when there are redundant allocations or when there is more than one optimal solution with the same cost. It can make solving the problem more complex and may require additional computational effort to resolve.
the phenomenon of obtaining a degenerate basic feasible solution in a linear programming problem known as degeneracy.
It depends on what it is.
you learn linear programming before you learn the transportation problem.
There is no problem *****
When the gravity of a massive star overcomes neutron degeneracy pressure, it can result in the star collapsing further to form a black hole. This occurs when the mass of the star is above a certain threshold known as the Tolman–Oppenheimer–Volkoff limit, causing the neutron degeneracy pressure to be insufficient to support the star against gravity.
Leave it
She was blind!
Racism
To succeed in dealing with (a problem or difficulty).
Because the gravity is not enough to overcome electron degeneracy pressure. White dwarf star material is so dense that in order for it to get any denser the electrons in the atoms making it up would have to be squeezed together. For a star the mass of the Sun, this density occurs when the star becomes about the size of Earth. Stars that are more than about one and a half times the mass of the Sun do have enough gravitational pull to overcome electron degeneracy pressure, and they shrink even more, winding up a dozen miles or so across. At this density (which is comparable to the density of an atomic nucleus), they are neutron stars and are kept from collapsing any further by neutron degeneracy pressure. Stars that are even larger have enough mass to overcome even that and wind up as a black hole; once you've passed the neutron degeneracy pressure, there's really nothing left to keep you from collapsing all the way into a singularity.