The Surface Tension of Magnetized Quark Matter

The surface tension of quark matter plays a crucial role for the possibility of quark matter nucleation during the formation of compact stellar objects and also for the existence of a mixed phase within hybrid stars. However, despite its importance, this quantity does not have a well established numerical value. Some early estimates have predicted that, at zero temperature, the value falls within the wide range $γ_0\approx10-300{\rm\ MeV/fm^2}$ but, very recently, different model applications have reduced these numerical values to fall within the range $γ_0\approx5-30{\rm\ MeV/fm^2}$ which would favor the phase conversion process as well as the appearance of a mixed phase in hybrid stars. In magnetars one should also account for the presence of very high magnetic fields which may reach up to about $eB\approx 3-30\, m_π^2$ ($B \approx 10^{19}-10^{20} \,G$) at the core of the star so that it may also be important to analyze how the presence of a magnetic field affects the surface tension. With this aim we consider magnetized two flavor quark matter, described by the Nambu--Jona-Lasinio model. We show that although the surface tension oscillates around its B=0 value, when $0 < eB \lesssim 10 \, m_π^2$, it only reaches values which are still relatively small. For $eB \approx 5\, m_π^2$ the B=0 surface tension value drops by about 30% while for $eB \gtrsim 10\, m_π^2$ it quickly raises with the field intensity so that the phase conversion and the presence of a mixed phase should be suppressed if extremely high fields are present. We also investigate how thermal effects influence the surface tension for magnetized quark matter.

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