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Area of Science:

  • Astrophysics
  • Nuclear Physics
  • Condensed Matter Physics

Background:

  • Neutron stars are extreme astrophysical objects with superfluid cores.
  • R-mode oscillations are a key phenomenon in rapidly rotating neutron stars.
  • Neutron superfluidity influences the dynamics and observable properties of neutron stars.

Purpose of the Study:

  • To constrain the parameters of neutron superfluidity in neutron star cores.
  • To investigate the effect of resonance stabilization on r-mode instability.
  • To utilize observations of rapidly rotating neutron stars to test theoretical models.

Main Methods:

  • Calculating finite-temperature r-mode spectra for realistic rotating superfluid neutron star models.
  • Accounting for muons and neutron-proton entrainment in stellar interiors.
  • Analyzing avoided crossings between normal and superfluid r modes.

Main Results:

  • Identified avoided crossings between normal and superfluid r modes at specific temperatures and spin frequencies.
  • Found strong dissipation and suppression of r-mode instability near avoided crossings.
  • Demonstrated the sensitivity of avoided crossing positions to neutron superfluidity models.

Conclusions:

  • The study successfully constrains neutron superfluidity parameters using r-mode resonance stabilization.
  • Observations of rapidly rotating neutron stars provide crucial data for these constraints.
  • This work advances our understanding of the physics within neutron star cores.