English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Context: When a rotating neutron star loses angular momentum, the reductionin the centrifugal force makes it contract. This perturbs each fluid element,raising the local pressure and originating deviations from beta equilibriumthat enhance the neutrino emissivity and produce thermal energy. This mechanismis named rotochemical heating and has previously been studied for neutron starsof nonsuperfluid matter, finding that they reach a quasi-steady configurationin which the rate at which the spin-down modifies the equilibriumconcentrations is the same at which neutrino reactions restore the equilibrium.Aims: We describe the thermal effects of Cooper pairing with spatially uniformenergy gaps of neutrons \Delta_n and protons \Delta_p on the rotochemicalheating in millisecond pulsars (MSPs) when only modified Urca reactions areallowed. By this, we may determine the amplitude of the superfluid energy gapsfor the neutron and protons needed to produce different thermal evolution ofMSPs. Results: We find that the chemical imbalances in the star grow up to thethreshold value \Delta_{thr}= min(\Delta_n+ 3\Delta_p, 3\Delta_n+\Delta_p),which is higher than the quasi-steady state achieved in absence ofsuperfluidity. Therefore, the superfluid MSPs will take longer to reach thequasi-steady state than their nonsuperfluid counterparts, and they will have ahigher a luminosity in this state, given by L_\gamma ~ (1-4)10^{32}\Delta_{thr}/MeV \dot{P}_{-20}/P_{ms}^3 erg s^-1. We can explain the UVemission of the PSR J0437-4715 for 0.05 MeV<\Delta_{thr}<0.45 MeV.

Rotochemical heating in millisecond pulsars: modified Urca reactions with uniform Cooper pairing gaps