Core electrons Critical temperature

The commonly accepted pulsar model is a neutron star of about one solar mass and a radius of the order of ten kilometers. A neutron star consists of a crust, which is about 1 km thick, and a high-density core. In the crust free neutrons and electrons coexist with a lattice of nuclei. The star s core consists mainly of neutrons and a few percents of protons and electrons. The central part of the core may contain some exotic states of matter, such as quark matter or a pion condensate. Inner parts of a neutron star cool up to temperatures 108iT in a few days after the star is formed. These temperatures are less than the critical temperatures Tc for the superfluid phase transitions of neutrons and protons. Thus, the neutrons in the star s crust and the core from a superfluid, while the protons in the core form a superconductor. The rotation of a neutron superfluid is achieved by means of an array of quantized vortices, each carrying a quantum of vorticity... 

A different situation arises when studying PMMA-latexes swollen by a nonpolar monomer like styrene which exhibits at ambient temperature a much lower solubihty in water (0.2 g/1) than MMA (15.9 g/1) [55]. Styrene has a very low electron density (see Table 1) in comparison to soUd PMMA and both an enrichment or a depletion of this monomer in the surface layer are easily discernible in a SAXS-experiment [55]. In comparison to the above system PMMA/MMA a critical test of the influence of entropic versus enthalpic forces becomes possible if the entropic wall-repulsion effect prevails styrene should be enriched in a surface layer. Because of the lower electron density of styrene this surface layer must exhibit a lower electron density than the core of the particle. If, on the other hand, the unfavorable enthalpic interactions between styrene and water are decisive, the more polar polymeric component PMMA should be enriched in a surface layer. In that case a surface layer with an enhanced electron density is expected. 

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