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 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

What is AXP (Anomalous X-ray Pulsar) Mereghetti et al., 2002

glitches

23

69

10 to10

10 to10

P

P

P

P

Theoretical models for pulsar glitches; star quake and vortex creep

Post-glitch recovery for Vela and Crab

Detected glitch parameters for Crab

Average ratio of permanent changes to slowdown rate

For Vela 0.00092

For Crab 0.00009

propeller

eq

eq mBPP

mB

P

7/315

7/612

Mc

7/215

7/412

8M

3/28c

7.4

RR when happenspropeller

106.4R

:radius ericmagnetosph

cm107.1R

:radius corotationKeplerian

Spin-down rate in the accretion model

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

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

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

Glitch pulsars and their associated SNRs

“young” pulsars and their missing SNRs

Spin-down rate in the accretion model

Timing feature of AXPs

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

Glitches in AXP?

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.