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Also a nonspherically symmetric accretion of matter may substantially change the upper limit of the accretion rate. In most cases, however, realistic accretion rates will be below ~/~. 2. Accretion Rates Let us, as a first instructive example, consider the accretion of interstellar gas by a single neutron star. Effects of a magnetic field will also be neglected. This problem has been treated by various authors and is discussed in detail in Chapter 13 of the book by Zel'dovich and Novikov (1971): Consider a system of noninteracting particles (with density 0~, speed v~) far from a star.

2) The domain of validity of this equation of state does, of course, not necessarily reach down to densities around 1015 g/cm 3, where there are just the first few species of known baryons and the statistical formula for the level density is not applicable. Thus Frautschi et al. point out that their formula may only be valid above 10 iv g/cm 3. This argument then leaves essentially all the problems for neutron star matter unsolved, because stable neutron stars contain matter only up to densities of about 1016 g/cm 3 (for the most extreme case of Leung and Wang, 1971).

I would expect this density to be unrealistically high, however, maybe 103o g/cm 3 or so. This naturally would rob the bootstrap concept of any validity in the case of cold, dense matter. Although no experimental evidence exists at very high densities, there are difficulties in arguing the repulsive forces away, and if they stay, then the bootstrap approach is neglecting the dominant feature at high densities and is therefore inadequate. 3. Manybody Treatment of a Hyperon Gas The many-body treatment of repulsive baryon-baryon interactions suffers from several uncertainties.

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