pulsar timing residuals induced by non-evolving single gw sources
DESCRIPTION
Pulsar timing residuals induced by non-evolving single GW sources. 童明雷 中国科学院国家授时中心. Outline. Introduction of pulsar timing The general solution of GWs from a supermassive black hole binary The time properties of timing residuals due to a single GW - PowerPoint PPT PresentationTRANSCRIPT
童明雷
中国科学院国家授时中心
23/4/21
1
Pulsar timing residuals induced by non-evolving
single GW sources
Outline
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Introduction of pulsar timingThe general solution of GWs from a supermassive black hole binary
The time properties of timing residuals due to a single GW
The effects of all the related parameters on the timing residuals
TOA (measured using the observatory clock) Residual
Pulsar timing
Fold Fold
Model
p2
SSB / EsRclkobs fDttt
clktDRsE
Observatory clock to TTDM delay ( D=DM/(2.41×10-16)s )Roemer delayShapiro delayEinstein delayParallex delay
Other delay terms including atmospheric delay, Shklovskii effect, relativistic second-order Doppler shift, GWs, etc.
Time transformationTime transformation
P
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Application of pulsar timingEstablish pulsar time standard similar
to atomic time scale Direct detection of GWs Improve knowledge of Solar system
properties, e.g. masses and orbits of outer planets and asteroids.
Application to spacecraft navigation based on pulsar timing
Outline
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Introduction of pulsar timingThe general solution of GWs from a supermassive black hole binary
The time properties of timing residuals due to a single GW
The effects of all the related parameters on the timing residuals
GW sources
Continuous sources: inspiral of binary compact stars, the rotating isolated neutron stars, and the neutron stars in the x-ray binary star systems.
Instantaneous sources: supernovae and coalescing binary systems
Stochastic background sources:Numbers of compact binary stars (inspiral and
merge)Relic GW from inflationCosmic strings
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In vacuum
the solution is the superposition of plane waves:
GWs only have two polarizations
h+ h×
The solution of GWs in Vacuum
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In vacuum
the solution is the superposition of plane waves:
GWs only have two polarizations
h+ h×
The solution of GWs in Vacuum
What is a non-evolving black hole binary?
Elliptical orbit of a binary system
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The kinematic solution
The period of the orbit
The differential equation for the Keplerian motion
The GW solution from a compact star binary
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In the linearized Einstein theory of GWs, the metric purterbations with TT gauge
The quadrupole moment for a binary system is
The coordinate system
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The solution of GWs
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13 Wahlquist, GRG, 1987
The cace of e=0
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Lee K J et al, MNRAS, 2011
Outline
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Introduction of pulsar timingThe general solution of GWs from a supermassive black hole binary
The time properties of timing residuals due to a single GW
The effects of all the related parameters on the timing residuals
Single GW sources
Earth
Pulsar
GW source
n
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The general cases of e≠0
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The setting of some parameters
Taking J0437-4715 as
an example
pn ,0,0,0
pcDp 157
1510H
sP 910 120
e=0
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e=0.3
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e=0.6
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120
e=0.8
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RMS residuals
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e=0
e=0.3
e=0.6
e=0.8
nsR 3.27
nsR 4.22
nsR 2.11
nsR 2.5
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Outline
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Introduction of pulsar timingThe general solution of GWs from a supermassive black hole binary
The time properties of timing residuals due to a single GW
The effects of all the related parameters on the timing residuals
The effect of
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The effect of Dp
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The effects of
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,
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3.0' eHH
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Thank you!