Probing Relativistic Gravity with the Double Pulsar
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1 Probing Relativistic Gravity with the Double Pulsar Marta Burgay INAF Osservatorio Astronomico di Cagliari
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3 The spin period of the original millisecond pulsar PSR B : P = ± sec In this pulsar, after few years of pulse timing, we can predict the time of arrival of pulses within 1 µs over 1 year!
4 Pulsars as clocks time Time residual time time
5
6 Pulsar Timing
7 Pulsar Timing: Binary pulsars 5 Keplerian-parameters: P orb, a p, e, ω, T 0 Mass function:
8 Testing GR with pulsars Extremely stable clocks TOA measurable and predictable with high accuracy Point-like massive source deforms spacetime delays in TOAs PK parameters measurable
9 Pulsar Timing: Post Keplerian parameters Periastron Precession - ω. Shapiro Delay r & s Grav. redshift & time dilation - γ Orbital decay P b.
10 Testing GR with Pulsars
11 What do we learn from PK parameters? Periastron precession Time dilation & gravitational redshift Shapiro delay (amplitude) Orbital period decay Shapiro delay (shape) GR tests!
12 Theories of Gravity: Tests Mass Function constraints NOT ALLOWED sin i = 1
13 Theories of Gravity: Tests
14 Theories of Gravity: Tests
15 Theories of Gravity: Tests
16 Theories of Gravity: Tests
17 Theories of Gravity: Tests
18 PSR B GR verified at 0.2% level
19 The discovery of PSR J Orbital period = 2.4 hr Orbital velocity 0.01 c Neutron Star companion Huge periastron advance (16.88 deg/yr) THE MOST RELATIVISTIC BINARY PULSAR EVER
20 Pulsations from the neutron star John Rowe Animation The first double pulsar ever known!
21 General Relativity with the Double Pulsar
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25 ! Theory independent
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30 June 2005 Kramer et al GR verified with 0.05% precision!
31 2009 GR verified with 0.02% precision!
32 Moment of Inertia Measurement precision increases with time Need 2PN order. At 2PN, spin-orbit coupling contribution to ω Related to the moment of inertia I, M, P EoS Total periastron advance at 2PN level:
33 7 mm per day! Coalescence in only 85 John Rowe Animation Short life time + Short Pb + Low Luminosity More DNS mergers than thought before
34 Method Use observed rotational and orbital parameters Consider separately the 3 coalescing DNS Simulate spatial and luminosity distribution of pulsars simulate N tot PSRs (same P s & P orb ) simulate major pulsar surveys and count pulsars observed (N obs )
35 N obs - N tot Correlation <N obs > = α N tot Calculate α for any model & DNS. Use the obtained value to calculate probability density function P(R)
36 Probability Density Function P(R) For every observed system i P i (R) = C i2 R exp(-c i R) where C i = α τ life f i combining the three P(R) i calculate P(R)
37 New estimate of R Thanks to the discovery of J R peak (revised) R peak (previous) ~ 5-7
38 Let s find them!
39 Thank you!
40 Constraining alternative theories. Kinematic. correction to P b very small (< 0.02%) we can measure GR P b to this precision (decreasing with T -2/5 ) we can do better than solar system tests to constrain alternative theories (scalar tensor)! Esposito-Farèse 2004
41 Constraining alternative theories.. - if Lorentz-invariance is violated a preferred frame would exist and the orbital orientation relative to it would change due to orbital precession - when W varies, orbital parameters should vary. Amplitudes for changing ω and e would be related.. (Wex & Kramer 2007)
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