1 / 25

Glitches; the Link Between the Typical Radio Pulsars and the Anomalous X-ray Pulsars

Glitches; the Link Between the Typical Radio Pulsars and the 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

cade
Télécharger la présentation

Glitches; the Link Between the Typical Radio Pulsars and the Anomalous X-ray Pulsars

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript


  1. Glitches; the Link Between the Typical Radio Pulsars and the 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 • Introduction to pulsar glitches and the post-glitch recovery • Explanations for the age problem of PSR B1757-24 • 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) Mereghetti et al., 2002

  4. glitches

  5. Theoretical models for pulsar glitches; star quake and vortex creep

  6. Post-glitch recovery for Vela and Crab

  7. Detected glitch parameters for Crab

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

  9. propeller

  10. Spin-down rate in the accretion model

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

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

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

  14. Glitch pulsars and their associated SNRs

  15. “young” pulsars and their missing SNRs

  16. Spin-down rate in the accretion model

  17. Timing feature of AXPs

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

  19. Glitches in AXP?

  20. 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.

More Related