Variations in the spin period of the radio-quiet pulsar 1E 1207.4-5209

Vyacheslav E. Zavlin, George G. Pavlov, Divas Sanwal

Research output: Contribution to journalArticle

37 Citations (Scopus)

Abstract

The X-ray source 1E 1207.4-5209 is a compact central object in the G296.5+10.0 supernova remnant. Its spin period of 424 ms, discovered with Chandra, suggests that it is a neutron star. The X-ray spectrum of this radio-quiet pulsar shows at least two absorption lines, the first spectral features discovered in radiation from an isolated neutron star. Here we report the results of timing analyses of Chandra and XMM-Newton observations of this source showing a nonmonotonous behavior of its period. We discuss three hypotheses that might explain the observational result. The first assumes that 1E 1207.4-5209 is a glitching pulsar, with frequency jumps of Δf ≳ 5 μHz occurring every 1-2 yr. The second hypothesis explains the deviations from a steady spin-down as being due to accretion (with the accretion rate varying from ∼1013 to ≳1016 g s-1) from a disk possibly formed from ejecta produced in the supernova explosion. Finally, the period variations might be explained by assuming the pulsar is in a wide binary system with a long period Porb ∼ 0.2-6 yr and a low-mass companion M2 < 0.3 M.

Original languageEnglish (US)
Pages (from-to)444-451
Number of pages8
JournalAstrophysical Journal
Volume606
Issue number1 I
DOIs
StatePublished - May 1 2004

Fingerprint

pulsars
accretion
radio
neutron stars
ejecta
explosion
supernova remnants
XMM-Newton telescope
newton
supernovae
explosions
x rays
time measurement
deviation
radiation
rate

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Zavlin, Vyacheslav E. ; Pavlov, George G. ; Sanwal, Divas. / Variations in the spin period of the radio-quiet pulsar 1E 1207.4-5209. In: Astrophysical Journal. 2004 ; Vol. 606, No. 1 I. pp. 444-451.
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Variations in the spin period of the radio-quiet pulsar 1E 1207.4-5209. / Zavlin, Vyacheslav E.; Pavlov, George G.; Sanwal, Divas.

In: Astrophysical Journal, Vol. 606, No. 1 I, 01.05.2004, p. 444-451.

Research output: Contribution to journalArticle

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AB - The X-ray source 1E 1207.4-5209 is a compact central object in the G296.5+10.0 supernova remnant. Its spin period of 424 ms, discovered with Chandra, suggests that it is a neutron star. The X-ray spectrum of this radio-quiet pulsar shows at least two absorption lines, the first spectral features discovered in radiation from an isolated neutron star. Here we report the results of timing analyses of Chandra and XMM-Newton observations of this source showing a nonmonotonous behavior of its period. We discuss three hypotheses that might explain the observational result. The first assumes that 1E 1207.4-5209 is a glitching pulsar, with frequency jumps of Δf ≳ 5 μHz occurring every 1-2 yr. The second hypothesis explains the deviations from a steady spin-down as being due to accretion (with the accretion rate varying from ∼1013 to ≳1016 g s-1) from a disk possibly formed from ejecta produced in the supernova explosion. Finally, the period variations might be explained by assuming the pulsar is in a wide binary system with a long period Porb ∼ 0.2-6 yr and a low-mass companion M2 < 0.3 M⊙.

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