Updated phase coherent timing solution of the isolated neutron star RX J0720.4-3125 using recent XMM-Newton and Chandra observations

M. M. Hohle*, F. Haberl, J. Vink, R. Turolla, S. Zane, C. P. de Vries, M. Méndez

*Corresponding author for this work

Research output: Contribution to journalArticleAcademicpeer-review

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Abstract

Aims. Since the last phase coherent timing solution of the nearby radio-quiet isolated neutron star RX J0720.4-3125 six new XMM-Newton and three Chandra observations were carried out. The phase coherent timing solutions from previous authors were performed without restricting to a fixed energy band. However, we recently showed that the phase residuals are energy dependent, and thus phase coherent solutions must be computed referring always to the same energy band.

Methods. We updated the phase coherent timing solution for RX J0720.4-3125 by including the recent XMM-Newton EPIC-pn, MOS1, MOS2 and Chandra ACIS data in the energy range 400-1000 eV. Altogether these observations cover a time span of almost 10 yrs. A further timing solution was obtained including the ROSAT pointed data. In this case, observations cover a time span of approximate to 16 yrs. To illustrate the timing differences between the soft band (120-400 eV) and the hard band (400-1000 eV) a timing solution for the soft band is also presented and the results are verified using a Z(n)(2) test.

Results. In contrast to previous work, we obtain almost identical solutions whether or not we include the ROSAT or Chandra data. Thanks to the restriction to the hard band, the data points from EPIC-pn are in better agreement with those from MOS1, MOS2 and Chandra than in previous works. In general the phase residuals are still large and vary with time. In particular, the latest XMM-Newton and Chandra data show that the phase residuals have attained relatively large and negative values. Using this and previous timing solutions, the residuals indicate a cyclic behaviour with a period approximate to 7-9 yrs if the variations follow a sinusoid, or twice this value in case the residuals are modulated by an abs(sine) probably approaching a new minimum around MJD = 55 240 days (February 2010). As an alternative interpretation, the phase residuals can be fitted with a glitch that occured around MJD = 53 000 days.

Original languageEnglish
Article number11
Number of pages13
JournalAstronomy & astrophysics
Volume521
DOIs
Publication statusPublished - Oct-2010

Keywords

  • stars: individual: RX J0720.4-3125
  • stars: neutron
  • stars: magnetic field
  • X-rays: stars
  • PHOTON IMAGING CAMERA
  • X-RAY-EMISSION
  • RX-J0720.4-3125
  • CANDIDATE
  • PULSARS
  • J1856.5-3754
  • DISCOVERY
  • SURFACES
  • RADIO

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