what theoretical physics can we learn from lisa gravitational wave … · 2017. 6. 1. ·...
TRANSCRIPT
Nicolas Yunes eXtreme Gravity Institute Montana State University
LISA Telecon May, 2017
What Theoretical Physics can we learn from LISA Gravitational Wave Observations ?
Yunes
eXtreme Matter meets eXtreme Gravity
2
Yunes
Plan of Attack
3
How well will we do?
What are we testing?
What are the open problems?
Yunes
What are we testing?
4
Gravitational Wave Generation
Gravitational Wave Propagation
Scalar/Vector Field Activation
Extra-Dimensional Leakage
Time-Variation of G
Gravitational Parity Violation
Gravitational Lorentz Violation
Modified Dispersion Relations
Cosmological Screening
Time-Variation of G
Modified Kinematics
Gravitational Lorentz Violation
Parity Violation
Lorentz Violation
SEP Violation
Spacetime Dimensionality Speed of Gravity
Mass of Graviton
Lorentz Violation
SEP Violation
Constrain Deviations of GR Pillars
Yunes
What well will we do?
5
[Chamberlain & Yunes, submitted]
10−27
10−26
10−25
10−24
10−23
10−22
aLIG
O
Voy.
A+
CE
ET-D
N2A
1
N2A
2
N2A
5
Ground-based
Space-based
Current Bound
Con
strainton
mg[eV/c
2]
Instrument
NSNSlBHNSlBHBHBHBH
GW150914
EMRIIMRIIMBHSMBH
Massive Graviton
[Barausse, Yunes, Chamberlain, PRL ’16]
Dipole Radiation
Yunes
What are the open problems?
6
Theory Data Analysis
New & Interesting Physical Mechanisms?
Cosmological Modified Theories?
Spin Precession in Modified Gravity?
Efficient data analysis w/high D parameter space? Reduced order methods for Modified gravity?
Mergers in Modified Gravity?
Pipelines for combined GW+EM studies of modified gravity?
EMRIs and resonances in Modified Gravity?
Pipelines for stacking tests of gravity ? (including e.g. coherent stacking and ringdown tests)
Modified Gravity
GR Modeling
Collaborative structure for theorists and data analysts? Just releasing analysis “code” will not work
Community
Support for both data analysis development and theory development is needed.
Yunes 7
Back Up Slides
Yunes 8
Intro Stuff
Yunes
What Physics Regime do GWs Probe?
9
Field Strength
Curvature Strength
GWs probe eXtreme Gravity
Extreme Gravity Tests
Weak Field Tests
[Will, Liv. Rev., 2005, Psaltis, Liv. Rev., 2008, Baker, et al, Siemens & Yunes, Liv. Rev. 2013, Yunes, et al PRD 2016]
Yunes
The Parameterized post-Einsteinian Framework
10
[Yunes & Pretorius, PRD 2009]
h(f) = hGR(f) (1 + ↵fa) ei�fb
[MSU: Cornish et al PRD 84 (’11), Sampson et al PRD 87 (’13), Sampson, et al PRD 88 (’13), Sampson et al PRD 89 (’14), Nikhef: Del Pozzo et al PRD 83 (’11), Li et al PRD 85 (’12), Agathos et al PRD 89 (’14), Del Pozzo et al CQG (’14).]
Yunes 11
Current Ligo Bounds
Yunes
GR Consistency Implies Constraints on Modified
12
Scalar Dipole Radiation
Anomalous Acceleration
Parity Violation
Lorentz Violation
Stronger GravityWeaker Gravity
[Yunes, Yagi, Pretorius, PRD ‘16]
Yunes
Theory Implications of Published GW Observations
13
[Yunes, Yagi, Pretorius, PRD ‘16]
Yunes
GR Consistency Implies Constraints on Modified
14
E2 = (pc)2 + A(pc)↵⇣vgc
⌘2= 1 + (↵� 1)AE↵�2
Massive Graviton
Doubly Special Relativity
SME, Horava-Lifshitz, Extra-Dimensions
Multifractal Spacetime
Superluminal
Subluminal
[Yunes, Yagi, Pretorius, PRD ‘16]
…. —> SME (5.5PN, 7PN)
Yunes
More on Robustness of Constraints
15
Constraint on ppE amplitude as a function of PN order at which the modification first enters (assuming BD functional structure)
Constraints are always robust, provided the modifications to the GW generation enter below 2.5PN order (ie. provided there is enough “information” in the
inspiral part of the waveform)
Yunes
But what about the higher PN order terms?
16
Case Study: Scalar-Tensor (Brans Dicke) theory
Caveat: These constraints are “conservative.” We could do better if we knew how the merger was modified and we included this in the analysis.
Yunes 17
Some Future Bounds (Including With Lisa)
Yunes
Future ppE Constraints on GR
18
[Chamberlain & Yunes, to appear soon]
bin. pul. bin. pul.
ground-basedspace-based
Yunes
Future Constraints on Violations of SEP
19
Extractable Physics:
Maximize Extraction:
Open Questions:
Non-Schw BHs (yes-hair theorem in EdGB)
NSs have scalar charge (scalar-tensor)
Low-mass BH or NS (long-inspiral) GWs
Merger? Hybrid IMR waveforms?
Compact Object binaries inspiral faster due to dipole radiation
[Chamberlain & Yunes, to appear soon]
10−8
10−7
10−6
10−5
10−4
10−3
10−2
aLIG
O
Voy.
A+
CE
ET-D
N2A
1
N2A
2
N2A
5
Ground-based
Space-based
A0620-00 LMXB
ConstraintonδE
Instrument
NSNSlBHNSlBHBHBHBH
GW150914
EMRIIMRIIMBHSMBH
� = � 3
224⌘2/5�E
Binary with tiny mass ratio
Yunes
Future Constraints on Gravitational Lorentz
20
Extractable Physics:
Maximize Extraction:
Non-Spinning BH is not SchwarzschildNSs have sensitivity-dependent GR deviationsCompact Object binaries inspiral faster due to dipole radiation
SMBHs or EMRIs do best
Open Questions:BH sensitivities and Inspiral BH waveforms? Merger? Hybrid IMR waveforms?
[Chamberlain & Yunes, to appear soon]
� =3
128nasty(c+, c�)
Yunes
Future Constraints on the Variation of Newton’s G
21
Maximize Extraction:
Open Questions:
Generation of GWs?
Merger? Hybrid IMR waveforms?
Binary system at widest separation possible (lowest frequency)
[Chamberlain & Yunes, to appear soon]
� = � 25
65526
G
GMz
Binary with largest chirp mass