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Astrophysical consequences of diquark formation on the surface of strange star

Compactness of some stars is explained if they are strange stars (SS) as shown by Dey et al.(1998) (D98) and Li et al. (1999a,b). In D98, a realistic potential was used in a Fock mean field approximation within Dirac phenomenology, thereby simplifying the spinorial structure of the quarks. Using the plane wave states for the beta equilibrated u, d and s quark Fermi seas from D98 and the conventional spin dependent force between these quarks, we now find energy lowering in some specific spin-aligned states. This is a short range pairing between quarks of different flavours and may lower the energy by several MeV for each diquark pair. The accretion driven X-ray and γ ray bursts in compact objects are believed to be due to thermonuclear or some other explosions which are short lived. These may in fact destroy the spin alignment of the quarks if these stars are SS. The subsequent alignment and production of copious diquark pairing may produce sufficient energy to produce recurrent very long bursts seen in some such stars. The long time involved in these processes, we claim, is due to the weak interactions which are responsible for the equilibration of strange quark matter. In such a the case the elusive properties of some of the most massive objects in nature, the compact stars, can be accounted for by spin alignment of pairs of the smallest components of matter, namely the quarks.