Rapid cooling of neutron star in Cassiopeia A and r-mode damping in the core

Abstract

We proposed alternative explanation to the rapid cooling of neutron star in Cas A. It is suggested that the star is experiencing the recovery period following the r-mode heating process,assuming the star is differentially rotating. Like the neutron-superfluidity-triggering model, our model predicts the rapid cooling will continue for several decades. However, the behavior of the two models has slight differences, and they might be distinguished by observations in the near future.

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Cited by in corpus (18)

• Tests of the nuclear equation of state and superfluid and superconducting gaps using the Cassiopeia A neutron star
• Limit on the Axion Decay Constant from the Cooling Neutron Star in Cassiopeia A
• Central Compact Objects in Supernova Remnants
• New constraints on the cooling of the Central Compact Object in Cas A
• Cooling of Small and Massive Hyperonic Stars
• Diffusive nuclear burning in cooling simulations and application to new temperature data of the Cassiopeia A neutron star
• Superfluid phases of triplet pairing and rapid cooling of the neutron star in Cassiopeia A
• X-ray bounds on cooling, composition, and magnetic field of the Cassiopeia A neutron star and young central compact objects
• $R$-mode Stability of GW190814's Secondary Component as a Supermassive and Superfast Pulsar
• Model-independent constraints on superfluidity from the cooling neutron star in Cassiopeia A
• Impact of axions on the Cassiopea A neutron star cooling
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• Neutron star cooling within the equation of state with induced surface tension
• Neutron star cooling with a dynamic stellar structure
• Axion Emission from Proton Cooper Pairs in Neutron Stars