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Glitches; Link between Typical radio pulsars and Anomalous X-ray Pulsars

Glitches; Link between Typical radio pulsars and Anomalous X-ray Pulsars Jinrong Lin & Shuangnan Zhang, 2003, in preparation Physics department & Center for Astrophysics in Tsinghua University. Contents. Brief introduction to the timing feature of AXP

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Glitches; Link between Typical radio pulsars and Anomalous X-ray Pulsars

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  1. Glitches; Link between Typical radio pulsars and Anomalous X-ray Pulsars Jinrong Lin & Shuangnan Zhang, 2003, in preparation Physics department & Center for Astrophysics in Tsinghua University

  2. Contents • Brief introduction to the timing feature of AXP • Pulsar glitches and the post-glitch recovery • The fate of PSR B1757-24 (a future candidate of Anomalous X-ray Pulsar). • Conclusions and discussion

  3. What is AXP (Anomalous X-ray Pulsar)

  4. glitches

  5. Post-glitch recovery for Vela and Crab

  6. Average ratio of permanent changes to slowdown rate For Vela 0.00092 For Crab 0.00009

  7. Spin-down rate in the accretion model

  8. Fate of pulsars in accretion model (P. Chatterjee et al. 2000)

  9. Chandra detection is consistent with standard magnetospheric emission (Kaspi et al. 2001)

  10. Estimation of the age of PSR B1757-24 or similar pulsars

  11. Glitch pulsars and their associated SNRs

  12. “young” pulsars and their missing SNRs

  13. Timing feature of AXPs

  14. Fate of PSR B1757-24when it is 290000 yrs old;

  15. Conclusions and discussion • New model bases on observation; glitches • We should carefully estimate the pulsars’ ages • the fate of a pulsar depends on its post-glitch recovery type. • The population of AXPs given by our model is reasonable.

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