脉冲星时间噪声和周期跃变

23/4/19 Pulsar Workshop - 2009, NAOC 1

Timing irregularities

• Timing noise: random fluctuation in pulse frequency with δν/ν ＜ 10-9

• Glitch: pulse frequency suddenly increases with 10-9 ＜ Δν/ν ＜ 10-6


(Lyne et al. 2000)

0( ) ( ) dtp p dt t t e

0( ) ( ) dtp dt t e

Glitches in the Crab pulsar

● Small glitch/3yr● Decay rapidly● Permanent increase in slowdown rate after the glitch


PSR B0531+21 Epoch 51562.7279 ν0=29.845547780(3) s-1 ν1=-3.7457341(7)x10-10 s-2 ν2= 1.0161006(4)x10-20 s-3 ν3=-6.0x10-31 s-4 DM= 56.77(2) cm-3 pc

Glitch Parameters:

Q=0.8(4)

810)8(4.2/

310)2(5/

d4

410)9(28.1/ p

Short fits of the Crab glitch

Glitches in the Crab pulsar

• two glitches in PSR B0531+21 (Crab pulsar)

Glitches in the Vela Pulsar


1996 ， Oct ， UT13.394MJD ~ 50369.394Q~0.4

62.15(2) 10 900 dd

Linear increase of vdot


Change of of the Vela Pulsar

Other glitches

• Frequent glitching pulsars• Various glitch recovery• Slow glitch• Tiny glitches• Unseen glitches


频繁跃变的脉冲星Frequent glitching pulsars

• PSR B0531+21 （ The Crab pulsar ） • PSR B0833 － 45 （ The Vela pulsar ）• PSR J0537 － 6910• PSR B1338 － 62• PSR B1737 － 30• PSR B1800 － 21• PSR B1046 － 58


频繁跃变的脉冲星— PSR B1737-30 的 8 个跃变

W. Z. Zou,N. Wang, R. N. Manchester,et al 2008, MNRAS, 384, 1063J. 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

9 610 2 10

61.85 10

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 (103—104yr)

• Others no permanent change: PSRs B1338 － 62, J1617 －5055, B1737 － 30, J1708 － 4009, B1757 － 24 ， J2021+3651

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 11 910 10

PSRs B0144+59, B0402+61, B0525+21, J1705−3423, B1815−14, B1900+06, B1907+10 和 B2224+65

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

ttQtt pdg )]/exp(1(1[)()( 0

pdd tt )/exp()(

Fractional decayQ = △νd/ △νg

Size △ν/ν=10-6

time constant τd=400 d

P

0P 0pP

•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 J1835-1106

Other pulsars


The jump in at MJD 52220 has the reversed sign of before and after the glitch. There was little or no change in at the time of the glitch.


Statistics


Statistics

Statistics



Statistics

The glitch activity is

proportional to spin-

down rate

1 gg

g

At


Statistics


Statistics


Statistics


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

直径2

0

公

里

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

2I R

I R

当 Δν/ν=10-8 ： ΔR=-0.1mm

星震由于偶极辐射损由于偶极辐射损

失能量，脉冲星的自转失能量，脉冲星的自转

并不是常数，它们是逐并不是常数，它们是逐

渐减慢的。能量被注入渐减慢的。能量被注入

到超新星遗迹。然到超新星遗迹。然

而而…………

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

23/4/19 29Pulsar Workshop - 2009, 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


Timing Noise

Continuous Restless Small scale

Red Long term Quasi-periodic

Timing Noise——data from Urumqi

Activity parameter


3( ) log6

t t

If t=108, we have Δ8.Fit to many pulsars we have:

8 6.6 0.6 log( )P

• Phase noise ∝ t1/2

• Frequency noise ∝ t3/2

• Frequency-derivative (slowdown) noise ∝ t5/2

Random walk in , and

残差与周期和周期导数


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脉冲星时间噪声和周期跃变