A mixing interpolation method to mimic pasta phases in compact star matter

Abstract

We present a new method to interpolate between two matter phases that allows for a description of mixed phases and can be used, e.g., for mimicking transitions between pasta structures occuring in the crust as well as in the inner core of compact stars. This interpolation method is based on assuming switch functions that are used to define a mixture of subphases while fulfilling constraints of thermodynamic stability. The width of the transition depends on a free parameter, the pressure increment relative to the critical pressure of a Maxwell construction. As an example we present a trigonometric function ansatz for the switch function together with a pressure increment during the transition. We note that the resulting mixed phase equation of state bears similarities with the appearance of substitutional compounds in neutron star crusts and with the sequence of transitions between different pasta phases in the hadron-to-quark matter transition. We apply this method to the case of a hadron-to-quark matter transition and test the robustness of the compact star mass twin phenomenon against the appearance of pasta phases modeled in this way.

8 pages, 9 figures, 2 tables, revised version accepted for publication in Eur. Phys. J. A

References in corpus (22)

• Shapiro delay measurement of a two solar mass neutron star
• A Massive Pulsar in a Compact Relativistic Binary
• Relativistic Shapiro delay measurements of an extremely massive millisecond pulsar
• Gravitational-wave constraints on the neutron-star-matter Equation of State
• Constraints on a phenomenologically parameterized neutron-star equation of state
• Using gravitational-wave observations and quasi-universal relations to constrain the maximum mass of neutron stars
• Neutron-star radius constraints from GW170817 and future detections
• A new quark-hadron hybrid equation of state for astrophysics - I. High-mass twin compact stars
• Implications from GW170817 and I-Love-Q relations for relativistic hybrid stars
• Disordered nuclear pasta, magnetic field decay, and crust cooling in neutron stars
• Third family of compact stars within a nonlocal chiral quark model equation of state
• Phases of dense matter in compact stars
• Hybrid equation of state with pasta phases and third family of compact stars
• Quark deconfinement transition in hyperonic matter
• Robustness of third family solutions for hybrid stars against mixed phase effects
• Binary and ternary ionic compounds in the outer crust of a cold nonaccreting neutron star
• Two novel approaches to the hadron-quark mixed phase in compact stars
• Neutron star mass limit at $2M_{\odot }$ supports the existence of a CEP
• Astrophysical aspects of general relativistic mass twin stars
• The QCD Phase Structure at High Baryon Density
• Model of the Phase Transition Mimicking the Pasta Phase in Cold and Dense Quark-Hadron Matter
• Astrophysical Constraints on Strong Modified Gravity

Cited by in corpus (12)

• The slope, the hill, the drop, and the swoosh: Learning about the nuclear matter equation of state from the binary Love relations
• Systematic study on the quark-hadron mixed phase in compact stars
• Two novel approaches to the hadron-quark mixed phase in compact stars
• Neutron stars with crossover to color superconducting quark matter
• Mixed phase transition from hypernuclear matter to deconfined quark matter fulfilling mass-radius constraints of neutron stars
• A bag model of matter condensed by the strong interaction
• Probing hadron-quark phase transition in twin stars using $f$-modes
• Studying VLOCV twin compact stars with binary mergers
• Isospin effect on quark matter instabilities
• Properties of the Object HESS J1731-347 as a Twin Compact Star
• Density functional approach to quark matter with confinement and color superconductivity
• Dense Baryonic Matter and Applications of QCD Phase Diagram Dualities