Bepposax Observations of the Young Pulsar in the Kes 75 Supernova Remnant (Articolo in rivista)

Type
Label
  • Bepposax Observations of the Young Pulsar in the Kes 75 Supernova Remnant (Articolo in rivista) (literal)
Anno
  • 2002-01-01T00:00:00+01:00 (literal)
Alternative label
  • Mereghetti S., Bandiera R., Bocchino F., Israel G.L. (2002)
    Bepposax Observations of the Young Pulsar in the Kes 75 Supernova Remnant
    (literal)
Http://www.cnr.it/ontology/cnr/pubblicazioni.owl#autori
  • Mereghetti S., Bandiera R., Bocchino F., Israel G.L. (literal)
Pagina inizio
  • 873 (literal)
Pagina fine
  • 878 (literal)
Http://www.cnr.it/ontology/cnr/pubblicazioni.owl#numeroVolume
  • 574 (literal)
Note
  • ISI Web of Science (WOS) (literal)
Http://www.cnr.it/ontology/cnr/pubblicazioni.owl#affiliazioni
  • AA(Istituto di Astrofisica Spaziale e Fisica Cosmica, Sezione di Milano ``G. Occhialini,'' via Bassini 15, I-20133 Milan, Italy; sandro@ifctr.mi.cnr.it), AB(Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, I-50125 Florence, Italy; bandiera@arcetri.astro.it), AC(Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, I-90134 Palermo, Italy; bocchino@astropa.unipa.it), AD(Osservatorio Astronomico di Roma, via Frascati 33, I-00040 Monteporzio Catone, Italy; gianluca@mporzio.astro.it) (literal)
Titolo
  • Bepposax Observations of the Young Pulsar in the Kes 75 Supernova Remnant (literal)
Abstract
  • We present the results of BeppoSAX observations of the young X-ray pulsar PSR J1846-0258, recently discovered at the center of the composite supernova remnant Kes 75. The pulsar (plus nebula) spectrum can be fitted by an absorbed power law with photon index ±ph=2.16+/-0.15, NH=(4.7+/-0.8)×1022 cm-2, and unabsorbed flux ~3.9×10-11 ergs cm-2 s-1 (2-10 keV). By joining two observations taken at an interval of 2 weeks, we have been able to obtain a precise measurement of the spin period (P=324.818968+/-0.000006 ms). This value, when combined with previous measurements, cannot be fitted by a smooth frequency evolution with a canonical braking index n=3. With the hypothesis of no glitches and/or significant timing noise, the braking index would be n=1.86+/-0.08, and assuming a short initial period, the pulsar age would be ~1700 yr, closer to that of the supernova remnant than the simple estimate Ä=P/2P&d2;=723 yr. Other likely possibilities involve the presence of glitches and lead to a wide range of acceptable ages. For example, we obtain n in the range 1.8-2.5 if a glitch occurred near MJD 51500, while for a glitch between 1993 October and 1999 March, we can only get a lower limit of n>1.89. (literal)
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