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2010 Glitch in Vela Pulsar
Sarah BuchnerSKA Bursary conference
Dec 2010
Observing Vela with XDM 2
Neutron Stars and Pulsars
Observing Vela with XDM 3
Pulsar Glitches
– Very good clock but …– Sudden increase in frequency
or “spin-up”– Frequency increases by few
parts per million– In energy terms
• earthquake of 17 on Richter scale
• surface of the earth moves by 15 m.
Observing Vela with XDM 4
Vela Pulsar
• PSR 0833-45• Vela supernova remnant• About 10 000 years old• P = 0.089 s = 11.2 Hz
Observing Vela with XDM 5
Vela Glitches
• Vela glitches
– Change in– Recovery contains exponential scales– 16 large glitches since 1969– Glitches every 1040 +- 326 days
69 1010
210
Observing Vela with XDM 6
Vela Glitches from HartRAO
• The Vela Pulsar is observed three or more times daily on most days from 1985-2008 using the HartRAO 26m antenna.
• Observations made at either S or L-band.
• Online glitch detection – if a glitch is detected then continuous observing begins to catch exponential recoveries.
• 10 large glitches observed
710
Observing Vela with XDM 7
Vela Glitches From HartRAO
Observing Vela with XDM 8
HartRAO bearing failure
• In October 2008 HartRAO 26m south polar bearing failed
• Started observing Vela with 15m XDM at HartRAO
Observing Vela with XDM 9
XDM observations
• 26m pulsar timer was single channel pulsar timer. Produced a folded profile for each 55s observation
• On XDM multi-channel iBob• Can access single pulse
data
Observing Vela with XDM 10
• Began observing Vela with XDM for 14.7 hours per day
• First prize: Catch a glitch “in the act”
• Second Prize: Parameterize the recovery
• Free gift: – Pulsar timing provides exacting test of
polarization and timing of XDM.– Soak test – continuous observing
Observing Vela with XDM 11
XDM and HartRAO
• Use XDM to observe continuously (15 hour per day)
• Use HartRAO 26m to make transit observations
Observing Vela with XDM 12
Waiting for Glitch
Observing Vela with XDM 13
Observing Vela
• 22 July 2010 26m was repaired and begun normal observing once again
• Observed Vela approximately once hourly
-160.000
-159.500
-159.000
-158.500
-158.000
-157.500
-157.000
-156.500
-156.000
-155.500
-155.000
45000 46000 47000 48000 49000 50000 51000 52000 53000 54000 55000
Observing Vela with XDM 14
10 days after 26m repaired…
Observing Vela with XDM 15
Glitch Parameters
• Glitch epoch– MJD 55408.802
• Vela was below horizon at the time
• Last pre-glitch observation– 1.9 hour before glitch
• First post-glitch observation– 7.4 hours after glitch
• Glitch size
91.1
Observing Vela with XDM 16
Issued ATel
Observing Vela with XDM 17
FERMI follow-up
• FERMI did not detect any increase of gamma-ray flux associated with the glitch
• FERMI timing detected the timing glitch – epoch not well constrained
Observing Vela with XDM 18
Constraining Glitch Epoch
• Regular observing allows glitch epoch to be constrained
• 2006 Glitch observed with 26m• Glitch occurred during a LIGO
science run• First direct search for grav
waves assoc with glitch• No grav wave seen
Observing Vela with XDM 19
Post-glitch Observations
Observing Vela with XDM 20
Determine nudot values
Observing Vela with XDM 21
XDM data
Observing Vela with XDM 22
Rotation Frequency
2010 Glitch
-5
0
5
10
15
20
25
55380 55400 55420 55440 55460 55480 55500 55520 55540
MJD
nu
* 1
E6 91.1
Observing Vela with XDM 23
Nu dot from XDM
Observing Vela with XDM 24
26 m data
Observing Vela with XDM 25
Spin-down
Observing Vela with XDM 26
The Standard Vela Glitch
3
1i
t
idgidet
Observing Vela with XDM 27
Transients for Glitches
5 d50 d5d5d
0.5d0.5d
50d50d
Observing Vela with XDM 28
Comparison with other Glitches
Observing Vela with XDM 29
Comparison
Observing Vela with XDM 30
Underlying Physics?
Observing Vela with XDM 31
Neutron Star
Observing Vela with XDM 32
Superfluid Rotation
• Core of neutron star is superfluid
• Rotates by means of array of quantised vortices
• For superfluid to slow down vortex lines must move outward
Observing Vela with XDM 33
Vortices in inner crust
• In inner crust vortices may pin to nuclei
• This region of superfluid is then unable to spin-down at same rate as crust
• Differential rotation develops
• At glitch vortices unpin and angular momentum is transferred from crustal superfluid to crust causing the spin-up
Observing Vela with XDM 34
Two-component model
intextcc NNI
)(I
N CSCint
)(I
NI CSCCC
)(I
I CSCSS
Observing Vela with XDM 35
Alpar Vortex Creep Model
• Coupling between superfluid and the crust is a function of the lag between the velocities
• At the time of the glitch – the crust spins up– The lag decreases– Hence the coupling
decreases– Superfluid “decouples”– Torque acting on smaller I
so spin-down increases– Recovery as region of
superfluid recouples
)(I
N CSCint
Observing Vela with XDM 36
Non-linear coupling
Observing Vela with XDM 37
Alpar Vortex Creep Model
Observing Vela with XDM 38
But …
• Not all glitches are the same
• HartRAO archive data – 1994 double glitch
Observing Vela with XDM 39
Overlaid Glitches with 1994
Observing Vela with XDM 40
• 1994 glitch does not show transients• Regions do not decouple?
– Yet lag between superfluid and crust must change
• Different mechanism?• Is the model correct?
Observing Vela with XDM 41
Pulse Shape Changes
• Recent paper by Weltevrede et al suggests glitch induced magnetospheric changes
• Look for pulse shape changes
• Look for increase of single pulses
Observing Vela with XDM 42
Conclusion
• Observing Vela with XDM• First prize: Catch a glitch “in the act”
– Vela was below horizon
• Second Prize: Parameterize the recovery– 14.7 hours of observing enabled 0.5d time scale to be
observed
• Free gift: – Pulsar timing provides exacting test of polarization and
timing of XDM.– Soak test – continuous observing
Observing Vela with XDM 43
Conclusion
• Work continues on modelling post-glitch recovery• Can recovery be modelled by 3 distinct
exponentials?• What is the physical reason for this?
Observing Vela with XDM 44
Thanks
KAT teamKAT teamHartRAO staffHartRAO staff
Observing Vela with XDM 45
Questions / Thoughts?
Observing Vela with XDM 46
Observing Vela with XDM 47
Questions
• How fast does the crust spin-up?
• What is the recovery?– Interior of neutron star
Observing Vela with XDM 48
Dedispersion and folding
DBE Dedisperse Fold Find TOA
BarycentreFind residuals
clock DM P
Std Profile
Pls position
Timestamp
Obs x,y,z
Observing Vela with XDM 49
Arrival Times (TOA)
53075.871601404853076.606809902953076.631509316253076.635258953453076.639008589753076.745305551253076.772805320553076.814437082853076.8440091993
Observing Vela with XDM 50
1st order - frequency
‘early’
‘late’
Observed - Predicted
Observing Vela with XDM 51
2nd order
Observing Vela with XDM 52
2nd order
Observing Vela with XDM 53
Residuals
32.04 us
Observing Vela with XDM 54
12 m @ Parkes
50.66 us
Hobbs et al, 20090907.4847
Observing Vela with XDM 55
Residuals
32.04 us
Observing Vela with XDM 56
XDM prototype at HartRAO
Kitty
Observing Vela with XDM 57
KAT-7
Observing Vela with XDM 58
KAT -> meerKAT
Observing Vela with XDM 59
meerKAT
Observing Vela with XDM 60
Observing Vela with XDM 61
Neutron Stars and Pulsars
Observing Vela with XDM 62
Observing Vela with XDM
Observing Vela with XDM 63
Waiting for Vela to glitch
Observing Vela with XDM 64
Storm clouds over HartRAO
Observing Vela with XDM 65
XDM Observations
• Observing Vela with XDM• First prize: Catch a glitch “in the act”
• Second Prize: Parameterize the recovery
• Free gift: – Pulsar timing provides exacting test of polarization and
timing of XDM.– Soak test – continous observing
Observing Vela with XDM 66
Determine Glitch Epoch