The physics of strange matter Page: 4 of 27
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2 * m.
where the chemical potential for each species is (i = u,d, s,e), and pR is the
renormalization point (see ref. 2). The number density of each species is n; =
dPi/dp-i' The total pressure, energy density, and baryon number of the system will
Chemical equilibrium is insured by the following weak interactions: u —► d(
or a) + e+ + i?, <f(s) + e—*u + viu + e~ —*■ <f(a) + u, d(a) —* u -f e- + and
u + d ++ u + which imply pu + fit — pd = where the neutrinos are assumed to
escape the system (//„ = 0). Charge neutrality imposes one more constraint upon
the system: 2nu — nd — n, — 3ne = 0. These two constraints leave the system with
only one free parameter, say p = pd = pt.
Strange matter is stable at zero pressure if the energy per baryon number of
strange matter is less than the nucleon mass, i.e., pjnR = e3qm < 939 MeV. (Ac-
tually, for strange matter to be the ground state of matter, we require < 930
MeV, the energy per baryon number of 58 .Fe.) Using the equations above, we can
calculate Z3QM & function of Bymt, and ae. In Fig. 1, we show contours of fixed
f3qm in the m, versus B plane (with ac = 0). There is a wide range of values of
B and m, within which strange matter is stable. The binding energy of strange
matter relative to s«Fe is A = 930 MeV-e3gM. For ac = 0, 145 MeV < BV* < 165
MeV, and mt < 300 MeV, there are stable solutions for strange matter. The lower
P = B 1
P = -Pi) + B ,
nu + nj + n
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Olinto, A. V. The physics of strange matter, article, December 1, 1991; Batavia, Illinois. (digital.library.unt.edu/ark:/67531/metadc1092177/m1/4/: accessed November 19, 2018), University of North Texas Libraries, Digital Library, digital.library.unt.edu; crediting UNT Libraries Government Documents Department.