2009/04/30 by Raka Dona Ray Mandal, Sushan Konar, Mira Dey +1 · 3 citations
Earth and Planetary Sciences · Physics and Astronomy · #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Binary pulsar #Geophysics and Gravity Measurements #Glitch #Magnitude (astronomy) #Millisecond pulsar #Neutron star #Optics #Physics #Pulsar #Pulsar planet #Pulsars and Gravitational Waves Research #Stars #astro-ph.SR
paper · pdf · doi:10.1111/j.1365-2966.2009.15314.x
published in Monthly Notices of the Royal Astronomical Society 399(2), 822-826 (Oxford University Press) · 5 pages, 5 figures, uses LaTeX2e(mn2e.cls) and astrobib(mn2e.bst): text substantially modified, to be published in MNRAS
arxiv created 2009/06/26 · openalex publication_date 2009/08/20 · arxiv updated 2015/05/13 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
The single glitch observed in PSR B1821−24, a millisecond pulsar in M28, is unusual on two counts. First, the magnitude of this glitch is at least an order of magnitude smaller (Δν/ν∼ 10−11) than the smallest glitch observed to date. Secondly, all other glitching pulsars have strong magnetic fields with B≳ 1011 G and are young, whereas PSR B1821−24 is an old recycled pulsar with a field strength of 2.25 × 109 G. We have earlier suggested that some of the recycled pulsars could actually be strange quark stars. In this work, we argue that the crustal properties of such a strange pulsar are just right to give rise to a glitch of this magnitude, explaining the scarcity of larger glitches in millisecond pulsars.