1998/08/11 by M. Jahan-Miri, Jahan-Miri, M.
Earth and Planetary Sciences · Physics and Astronomy · #Astrophysics (astro-ph) #FOS: Physical sciences #Geological and Geophysical Studies #Geophysics and Gravity Measurements #Pulsars and Gravitational Waves Research #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/9808100
7 pages, 1 figure, submitted to ApJ, only one part of the earlier version, largely revised
openalex publication_date 1998/08/11 · arxiv created 1999/11/11 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
The observed large rates of spinning down after glitches in some radio pulsars has been previously explained in terms of a long-term spin-up behaviour of a superfluid part of the crust of neutron stars. We argue that the suggested mechanism is not viable; being inconsistent with the basic requirements for a superfluid spin-up, in addition to its quantitative disagreement with the data. One may therefore conclude, for the first time, that the presence and the pinned nature of neutron superfluid in the core of neutron stars is evidenced by the existing observational data.