2025/02/04 by Yujie Lian, P. C. C. Freire, Lian, Yujie +15 · 2 citations
Biochemistry, Genetics and Molecular Biology · #Cancer Genomics and Diagnostics #Cancer, Hypoxia, and Metabolism #FOS: Physical sciences #High Energy Astrophysical Phenomena (astro-ph.HE) #RNA modifications and cancer
paper · pdf · doi:10.48550/arxiv.2502.02042
openalex publication_date 2025/02/04 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
PSR B1310+18A is a 33-ms binary pulsar in a 256-day, low eccentricity orbit with a low-mass companion located in NGC 5024 (M53). In this Letter, we present the first phase-coherent timing solution for this pulsar (designated as M53A) derived from a 35-year timing baseline; this combines the archival Arecibo Observatory data with the recent observations from the Five-hundred-meter Aperture Spherical radio Telescope (FAST). We find that the spin period derivative of the pulsar is between 6.1 and 7.5 × 10-19 \rm s s-1, which implies a characteristic age between 0.70 and 0.85 Gyr. The timing solution also includes a precise position and proper motion for the pulsar, enabling the identification of the companion of M53A in Hubble Space Telescope data as a Helium white dwarf (He WD) with a mass of M\rm WD=0.39+0.05-0.07 \rm M\odot and a cooling age of 0.14+0.04-0.03 \rm Gyr, confirming that the system formed recently in the history of the GC. The system resembles, in its spin and orbital characteristics, similarly wide pulsar - He WD systems in the Galactic disk. We conclude by discussing the origin of slow pulsars in globular clusters, showing that none of the slow pulsars in low-density globular clusters are as young as the systems observed in the densest known globular clusters.