1997/09/25 by A. N. Parmar, T. Oosterbroek, Parmar, A. N. +11 · 1 citation
Engineering · Physics and Astronomy · #Astrophysical Phenomena and Observations #Astrophysics (astro-ph) #Astrophysics and Cosmic Phenomena #FOS: Physical sciences #Particle Accelerators and Free-Electron Lasers #Pulsars and Gravitational Waves Research #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/9709248
6 pages. Accepted for publication in A&A
arxiv created 1997/09/25 · openalex publication_date 1997/09/25 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
The 7 s X-ray pulsar 1E2259+586 and the supernova remnant (SNR) G109.1-1.0\n(CTB 109) were observed by BeppoSAX in 1996 November. The pulse period of\n6.978914 +/- 0.000006 s implies that the source continues its near constant\nspin-down trend. The 0.5-10 keV pulse shape is characterized by a double peaked\nprofile, with the amplitude of the second peak ~50% of that of the main peak.\nThe pulse profile does not exhibit any strong energy dependence. We confirm the\nASCA discovery of an additional low-energy spectral component from 1E2259+586.\nThis can best be modeled as a 0.44 keV blackbody, but we cannot exclude that\nsome, or all, of this emission arises from the part of the SNR that lies within\nthe pulsar's extraction region.\n The spectrum of G109.1-1.0 is well fit with a non-equilibrium ionization\nplasma model with a best-fit temperature of 0.95 keV. The derived mass for the\nX-ray emitting plasma (~15-20 solar masses) and its near cosmic abundances\nimply that the X-ray emission comes mainly from mildly enriched, swept-up\ncircumstellar material. The spectrum is strongly out of equilibrium with an\nionization age of only 3000 yr. This age is in good agreement with that derived\nfrom hydrodynamic simulations of the SNR using the above X-ray temperature.\n