Pulsar Workshop , NAOC1

Timing irregularities Timing noise: random fluctuation in pulse frequency with δν/ν ＜ Glitch: pulse frequency suddenly increases with ＜ Δν/ν ＜ Pulsar Workshop , NAOC2

(Lyne et al. 2000)

Glitches in the Crab pulsar ● Small glitch/3yr ● Decay rapidly ● Permanent increase in slowdown rate after the glitch Pulsar Workshop , NAOC4 PSR B Epoch ν 0 = (3) s -1 ν 1 = (7)x s -2 ν 2 = (4)x s -3 ν 3 =-6.0x s -4 DM= 56.77(2) cm -3 pc

Glitch Parameters: Q=0.8(4) Short fits of the Crab glitch Glitches in the Crab pulsar

two glitches in PSR B (Crab pulsar)

Glitches in the Vela Pulsar Pulsar Workshop , NAOC ， Oct ， UT MJD ~ Q~0.4 Linear increase of vdot

Pulsar Workshop , NAOC8 Change of of the Vela Pulsar

Other glitches Frequent glitching pulsars Various glitch recovery Slow glitch Tiny glitches Unseen glitches Pulsar Workshop , NAOC9

频繁跃变的脉冲星 Frequent glitching pulsars PSR B （ The Crab pulsar ） PSR B0833 － 45 （ The Vela pulsar ） PSR J0537 － 6910 PSR B1338 － 62 PSR B1737 － 30 PSR B1800 － 21 PSR B1046 － Pulsar Workshop , NAOC10

频繁跃变的脉冲星 — PSR B 的 8 个跃变 W. Z. Zou,N. Wang, R. N. Manchester,et al 2008, MNRAS, 384, 1063 J. P. Yuan, N. Wang, R. N. Manchester, Z. Y. Liu, 2009, MNRAS 20 年一共探测到 22 个周期跃变 ，相对变化幅度范围在 增加 最大跃变为： PSRs J0537−6910, B0833−45, B1046−58 and B1800−21 的跃变 幅度变化较大，及 B1737 － 30 PSRs B1338−62, B1757−24 and B1758−23 跃变幅度较均一

Various glitch recovery 多种形式的周期跃变恢复过程 J. P. Yuan, N. Wang, R. N. Manchester, Z. Y. Liu ，拟投稿 MNRAS Vela like permanent change in frequency derivative: PSRs B1046 － 58, B1610 － 50, B1706 － 44 (10 3 —10 4 yr) Others no permanent change: PSRs B1338 － 62, J1617 － 5055, B1737 － 30, J1708 － 4009, B1757 － 24 ， J

Slow glitch 慢跃变 Zou, W. Z.; Wang, N.; Wang, H. X. et al. 2004, MNRAS, 354, 811 J. P. Yuan, N. Wang, R. N. Manchester, Z. Y. Liu, 2009, MNRAS

Tiny glitches 微跃变 PSRs B , B , B , J1705−3423, B1815−14, B , B 和 B J. P. Yuan, N. Wang, R. N. Manchester, Z. Y. Liu ，已投稿 MNRAS

Unseen glitches

Glitch Model: ◇ Amplitude in ΔP and agree with our observation ◇ In agreement with the Crab pulsar glitch: ◇ Correlation in sign Fractional decayQ = △ ν d / △ ν g Size △ ν/ν=10 -6 time constant τ d =400 d

Significant cubic terms with opposite signs are present in the pre- and post-glitch data, suggesting a sign change in at the time of the glitch. Detected one glitch in PSR J Other pulsars

Pulsar Workshop , NAOC18 The jump in at MJD has the reversed sign of before and after the glitch. There was little or no change in at the time of the glitch.

Pulsar Workshop , NAOC19 Statistics

Pulsar Workshop , NAOC20 Statistics

Pulsar Workshop , NAOC21

Pulsar Workshop , NAOC22 Statistics The glitch activity is proportional to spin- down rate

Pulsar Workshop , NAOC23 Statistics

Pulsar Workshop , NAOC24 Statistics

Pulsar Workshop , NAOC25 Statistics

Pulsar Workshop , NAOC26 Statistics 199 glitches in 63 pulsars, Mostly occur in young pulsars.

跃变的产生： 基于中子星的解释 中子星的大气，超热等离子体 外壳层， 200 米深 ，核子 + 电子 内壳层，晶体结构 1km, 核子 + 电子 + 中子滴 外核， 原子粒子流 内核，固态亚原子粒子？

极端物理条件下的固态物理 当 Δν/ν=10 -8 ： ΔR=-0.1mm 星 震星 震 由于偶极辐射损失 能量，脉冲星的自转并 不是常数，它们是逐渐 减慢的。能量被注入到 超新星遗迹。然而 …… 28 跃变的产生： 基于中子星的解释 Starquake model: change in ellipticity

Two component models- crust and superfluid: sudden unpinning of superfluid vortices, release the angular momentum to the crust Pulsar Workshop , NAOC 跃变的产生： 基于中子星的解释 Try to solve different type of pulsar glitches: Crab like Vela like Old pulsars Slow glitch pulsars

Pulsar Workshop , NAOC30 Timing Noise Continuous Restless Small scale Red Long term Quasi-periodic

Timing Noise ——data from Urumqi

Activity parameter Pulsar Workshop , NAOC32 If t=10 8, we have Δ 8. Fit to many pulsars we have: Phase noise ∝ t 1/2 Frequency noise ∝ t 3/2 Frequency-derivative (slowdown) noise ∝ t 5/2

残差与周期和周期导数 Pulsar Workshop , NAOC33