Post-Newtonian Mechanics of the Earth-Moon System · Earth-Moon System 2Department of Physics and...

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Post-Newtonian Mechanics of the Earth-Moon System 2 Department of Physics and Astronomy University of Missouri-Columbia, USA Journées 2010, 20-22 September 2010 Yi Xie 1,2 , Sergei Kopeikin 2 1 Astronomy Department Nanjing University, China

Transcript of Post-Newtonian Mechanics of the Earth-Moon System · Earth-Moon System 2Department of Physics and...

Page 1: Post-Newtonian Mechanics of the Earth-Moon System · Earth-Moon System 2Department of Physics and Astronomy University of Missouri-Columbia, USA Journées 2010, 20-22 September 2010

Post-Newtonian Mechanics of the Earth-Moon System

2Department of Physics and Astronomy

University of Missouri-Columbia, USA

Journées 2010, 20-22 September 2010

Yi Xie1,2, Sergei Kopeikin2

1Astronomy Department

Nanjing University, China

Page 2: Post-Newtonian Mechanics of the Earth-Moon System · Earth-Moon System 2Department of Physics and Astronomy University of Missouri-Columbia, USA Journées 2010, 20-22 September 2010

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Outline

Motivations

Post-Newtonian reference frames

Post-Newtonian mechanics

Outlook

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Motivations

Distinguish physics from coordinates

Comprehensive and self-consistent theory of PN Equations of Motion

Current and future high-precision experiments

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MotivationsDistinguish physics from coordinates

Curved spacetime:

Coordinates

Physics

Strongly coupledDifficult to disentangle

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ai=aiNewton

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c2∑j≠i

vi× vj×GMj

rij3 rji⋯

Extrinsic gravitomagnetic effects:

PPN-EIH:

t '=t− 1

c 4∑B

B

GMB

rB

rB⋅vB

x '=x−1c 2∑

B

B

GMB

rB

rB

∑j≠i

22−j

c2 vi× vj×GMj

rij3 rji

gravitomagnetic force:

depends on the choice of coordinates .j

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MotivationsComprehensive theory of PN EoMEinstein-Infeld-Hoffman: N-point particleBarker & O'Connell: spin (point particle)Brumberg-Kopeikin: N-body (Newtonian multipoles+spins)Damour-Soffel-Xu: N-body (PN multipoles+spins in GR)Kopeikin & Vlasov: N-body (PN multipole+spins in STT)Racine & Flanagan: extend BK+DSX (flux integral method)Xie & Kopeikin: Earth-Moon reference frames (offprints available)

Our goals:

PN EoM with multipoles expressed explicitly with coordinates and velocities of bodies

MBaB=F (xC, vC; IC<L>, SC

<L>;γ,β)

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Motivations

Current and future high-precision experiments:Lunar Laser Ranging

relativisitic parameters selenophysics: liquid core?

Pulsar timingGravitational wave astronomy:

Earth-Moon system as a detector of GWs

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EMBSSB

GRF

SRF

Ĝμν(Σ,Y)

gμν(t,x)

Gμν(T,X )

ĝμν(u,w)

PN Reference Frames

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PN Reference FramesA global frame

Solar System Barycentric Frame orbital motions

N local frames

eg. Geocentric Frame internal motions of matter, time evolution of multipoles

Some local frames for subsystems

eg. the Earth-Moon Barycentric Frame relative motions for LLR

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e=0.00549

Why local frames? Multipole moments

S

Ev

M

Lorentzcontraction~2 m (Lunar Orbit)

S

E

M

Einsteincontraction

~4 m (Lunar Orbit)

Earth+Moon as acomposite body

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e=0.00549

Why to use the local frame for subsystems?

Hierarchical systems: extension of IAU2000 resolutions

Universe -> superclusters -> clusters -> groups

-> galaxies -> stellar clusters -> stellar systems

-> planetary systems

Lunar mass is not negligible: M/E~1/80

The Geocentric Frame can not cover the Moon.

LLR is a local frame experiment

EMB frame helps to understand the gauge freedom

of equations of motion.

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Momentum centered

I=0

A coincides with B (a constraint

on dipole)

dI/du=0I=Pu+I0

Page 13: Post-Newtonian Mechanics of the Earth-Moon System · Earth-Moon System 2Department of Physics and Astronomy University of Missouri-Columbia, USA Journées 2010, 20-22 September 2010

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PN Mechanics

PN orbital motion (external problem)

the body B's motion in the SSB frame

PN relative motion (internal problem)

Moon with respect to Earth in the EMB frame

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PN orbital motion Conservation of dipole moment: d2I/du2=0

Matching procedure: coordinate transformation, the law of motion of the origin of the local frame

... ...

The PPN translational equations of motion of extended bodies in the global frame

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2-body interactions: RBC 3-body interactions: RBCRBD, RBCRCD

spin effects

B

CD

PN orbital motion

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Definition of Mass (Blanchet-Damour)

1. a single particle: rest mass

2. a single body: rest mass + internal energy

3. a body in N-body system: rest mass + internal energy + external effects

rest mass internal energy external effects

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MB≠IB inertial mass ≠ gravitational mass violation of Strong EquivalencePrinciple in Scalar-Tensor theory

Violation of Strong Equivalence Principle

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PN relative Motion

PN orbital motion of Moon in EMB

PN orbital motion of Earth in EMB

Moon-Earth in the EMB frame

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Outlook: SelenophysicsFluid coremore convincing evidences, radius

Elastic propertiesLove numbers

Spin-orbit coupling

Harmonics in the multi-layer Moon

Dissipation and convection

Free libration modes

Topography and mascons

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Outlook: Fundamental PhysicsStronger limitationsnonlinear parameter , dark energy, scalar fieldsβ

New relativistic effectsrelativistic precession of lunar orbit w.r.t. ICRFrelativistic quadrupole moment of the Earthtidal gravitomagnetic effectsviolation of SEP

Stochastic GW background

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Thank you!