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Constraining hadronic superfluidity with neutron star precession.
1Department of Physics, Montana State University, Bozeman, Montana 59717, USA.
Physical Review Letters
|October 4, 2003
Summary
The standard model of neutron star cores, featuring coexisting neutron and proton superfluids, contradicts pulsar observations. This suggests either no superfluid coexistence or a type I superconducting core, impacting cooling and glitch theories.
Area of Science:
- Astrophysics
- Nuclear Physics
- Condensed Matter Physics
Background:
- Neutron stars are dense remnants of supernovae.
- Their cores are theorized to contain neutron and proton superfluids.
- Protons may form a Type II superconductor, influencing stellar behavior.
Purpose of the Study:
- To reconcile theoretical models of neutron star cores with observational data.
- To investigate the superconducting state of protons within neutron stars.
- To understand the implications for observable phenomena like pulsar precession.
Main Methods:
- Analysis of observational data from long-period (approx. 1 year) precession in isolated pulsars.
- Comparison of observational constraints with theoretical models of neutron star core composition and superconductivity.
- Theoretical modeling of superfluid and superconducting states in extreme densities.
Main Results:
- The standard model of a Type II superconducting proton component is inconsistent with observed pulsar precession periods.
- The observed precession suggests a deviation from the standard model's assumptions.
- This inconsistency challenges the assumed structure of neutron star cores.
Conclusions:
- The coexistence of neutron and proton superfluids in the standard configuration may not occur in neutron star cores.
- Alternatively, the proton core might be a Type I superconductor, not Type II.
- These findings necessitate revisions to theories of neutron star cooling and spin-down (glitches).