Near Optimal Ground Support in Multi-Spacecraft Missions: A GA Model and its Results

This study addresses the optimal allotment of ground station support time to low Earth orbit (LEO) spacecraft with clashing radio visibilities. LEOs now form a critical global infrastructure for natural resource management, rescue, crop yield estimation, flood control, communication, and space research and travel support. In the multi-spacecraft scenario, ground support becomes complex because of spacecraft-specific constraints, station configuration, spacecraft priorities and priorities of payload and special operations. A generalization of the classical product mix problem, spacecraft support is NP-complete and more complex than the former because of arbitrarily defined profitability profile. Genetic algorithms (GA) are used to near optimally resolve visibility clashes. It concludes with the illustration of real life spacecraft support optimization problems routinely faced by mission managers. A spin-off of this work is that it can enable the decision maker to also determine optimal ground station locations and support capability deployment in diverse planning scenarios.     

Strange star Equation of State with a modified Richardson potential

Richardson potential is an phenomenological interquark interaction taking care of two aspects of QCD, namely the asymptotic freedom and the confinement. The original potential has a scale parameter having value 400 MeV and is well tested in hadronic property calculations. This potential was then used in strange star calculation. Strange stars are very compact stars composed of strange quark matter, i.e. a very high density strange quark phase consisting of deconfined u, d and s quarks. Here the value of the scale parameter was taken as 100 MeV. The argument was that for a deconfined quark system like a strange star, the scale parameter may have a value quite different from that used in hadronic sector. To remove this discrepancy we introduced two scale parameters in the potential, one for the asymptotic freedom part and the other for the confining part. With suitable values of the parameters, this modified potential has been successfully used in both baryonic property and strange star calculations. The Equation of States obtained with the modified potential are also used to obtain mass–radius relations for the strange stars.