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Extra info for Equilibrium plasma properties, outer envelopes(en)(62s)
Sample text
On the other hand, such ions cannot survive in the inner crust; they would immediately disappear there owing to beta captures and pycnonuclear reactions (see Shapiro & Teukolsky 1983 and Chapter 3). Therefore, the appearance of quantum liquid is actually important only for hydrogen and helium in the outer neutron star envelope, where zero-point motion drastically suppresses the crystallization of these ions. 5 The pressure of degenerate electrons with electrostatic corrections For many applications it is sufficient to use a fairly simple EOS of the outer (e) envelope of a neutron star.
At high temperatures the electron heat capacity dominates over the ion one (Fig. 7) because of the large amount of electrons per one ion in the iron and carbon matter. However, with decreasing T the electron heat capacity decreases proportionally to T , while the ion heat capacity is a slow function of T as long as the quantum effects are unimportant. Accordingly, the ion heat capacity dominates in a large temperature interval. However, when the temperature becomes much lower than Tpi , the quantum effects strongly reduce the ion heat capacity, and the electron heat capacity dominates again, as seen in the left insets of both panels of Fig.
It is difficult to find Γm with high precision, because the intersection of the free energy curves is strongly affected by the thermal corrections which are small at Γ ∼ Γm (the free energy curves are nearly parallel). 1% error in Fii shifts the intersection by ∆Γ ≈ 15 (Pollock & Hansen, 1973). According to Fig. 2, the melting in the envelopes of middle-aged neutron stars takes place at ρ 106 g cm−3 . Therefore, the model of the rigid electron background presents a good starting approximation for calculating Γm in most cases.
Equilibrium plasma properties, outer envelopes(en)(62s)
by Daniel
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