Vortex creep heating in neutron star cooling with direct Urca processes in heavy neutron stars
arXiv:2511.13263
Abstract
Old, thermally bright neutron stars imply internal heating at late times. Among candidate mechanisms, vortex creep heating (VCH) provides a robust link between spin-down and frictional dissipation in the pinned inner-crust superfluid, yet its interplay with fast DUrca cooling in massive stars remains insufficiently explored. We (i) implement VCH in our cooling code and validate it; (ii) identify the physically consistent domain where the steady-state form applies; (iii) quantify how regulate observable VCH signatures under DUrca cooling; and (iv) introduce a 3D representation that resolves degeneracies hidden in standard 2D projections. Cooling is computed with BSk24 and APR EoS, standard pairing gaps, and iron/carbon envelopes. VCH is modeled with erg s, and a quantum-creep coverage fraction diagnoses when steady-state heating is valid. We survey G and -- ms for and , and compare with a curated set of ordinary pulsars with measured . Results: (1) Our implementation reproduces published VCH bands. (2) The validity boundary follows magnetic-dipole spin-down, confirming consistency with . (3) DUrca+VCH maintains K for G up to ms. (4) The 3D representation shows that sources appearing coincident in occupy distinct -layers, removing degeneracies. VCH can substantially reshape late-time thermal states when spin-down power remains high; its observability depends chiefly on rather than on mass alone. We provide a practical validity map for and advocate treating as a co-equal axis in cooling analyses. (Shortened due to the arXiv words limit.)
20 pages, 14 figures, 1 table