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Phase Transitions in Neutron Stars and Maximum Masses.

Heiselberg, Hjorth-Jensen

    The Astrophysical Journal
    |October 8, 1999
    PubMed
    Summary

    We used nuclear matter interactions to constrain the equation of state for neutron stars. If neutron star masses reach 2.3 solar masses, soft equations of state and strong phase transitions are ruled out.

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    Area of Science:

    • Nuclear Physics
    • Astrophysics
    • High-Energy Physics

    Background:

    • Neutron stars are remnants of supernovae, governed by extreme physics.
    • Understanding the equation of state (EoS) of nuclear matter is crucial for neutron star properties.
    • Phase transitions at high densities within neutron stars are theoretically predicted.

    Purpose of the Study:

    • To constrain the equation of state (EoS) of nuclear matter using realistic interactions.
    • To calculate the maximum masses of rotating neutron stars, incorporating phase transitions.
    • To test the impact of potential quark matter formation on neutron star structure.

    Main Methods:

    • Employed recent realistic effective interactions for nuclear matter.
    • Extrapolated to high densities, ensuring causality.
    • Included first- and second-order phase transitions, such as to quark matter.
    • Calculated maximum masses for rotating neutron stars.

    Main Results:

    • Constrained the equation of state (EoS) for dense nuclear matter.
    • Determined maximum mass limits for rotating neutron stars.
    • Showed that confirmed neutron star masses around 2.3 solar masses exclude soft EoS and strong phase transitions.

    Conclusions:

    • The equation of state of neutron stars is sensitive to high-density physics.
    • Observational constraints from neutron star masses can rule out specific EoS models.
    • Strong phase transitions in neutron star cores are unlikely if high masses are confirmed.

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