Theoretical Physics Implications of LIGOs Gravitational Wave - PowerPoint PPT Presentation

Theoretical Physics Implications of LIGO’s Gravitational Wave Observations Nicolas Yunes eXtreme Gravity Institute Montana State University Experimental Searches for Quantum Gravity Conference September 21st, 2016 Yunes, Yagi, Pretorius, arXiv 1608.06187, PRD (2016)

What is Montana? Montana Yunes 2

What is Montana? Now accepting Applications for our Physics PhD Program!! Yunes 3

What do I do? Theoretical Physics Analytical Relativity Experimental Gravitational Wave Relativity Astrophysics What can we learn from precision observations in extreme gravity environments? Yunes 4

Why is this important now? Yunes 5

Why is this important in the near future? GEO LHO KAGRA Ligo-India LLO Virgo/AdV eLISA Pathfinder Success! Yunes 6

Roadmap Extreme Gravity GW Tests Implications Yunes 7

What is eXtreme Gravity & Gravitational Waves? eXtreme where gravity is [RIT Group] Gravity: (a) very strong, (b) non-linear (c) dynamical Gravitational Wave-like perturbation Waves (GWs): of the grav. field. Generation Accelerating masses of GWs: (t-variation in multipoles) Propagation Light speed, weakly of GWs: interacting, 1/R decay. GW Spectrum: Kepler 3rd Law: , Yunes Example: Binary BH merger, Extreme Gravity GW Tests Implications Yunes 8

Gravitational Wave Spectrum Cosmic Strings SMBH Mergers Supernovae BH and NS Binaries Relic radiation Extreme Mass Ratio Supermassive BH Binaries Spinning NS Binary Mergers 10 -16 Hz 100 years hours milliseconds year days seconds 10 -16 Hz 10 -7 Hz 10 1 Hz 10 3 Hz 10 -9 Hz 10 -6 Hz 10 -4 Hz Pulsar timing Ground interferometers Inflation Probe Space detectors Yunes Extreme Gravity GW Tests Implications Yunes 9

How do we detect gravitational waves? Yunes Extreme Gravity GW Tests Implications Yunes 10

How do we detect gravitational waves? Yunes Extreme Gravity GW Tests Implications Yunes 11

How do we detect gravitational waves? Yunes Extreme Gravity GW Tests Implications Yunes 12

How do we extract signals from the noise? Modelling 1. Create template “filters” 2. Cross-correlate filters & data Data Analysis 3. Find filter that maximizes the cross-correlation. signal-to- [C. Hanna, PSU] data noise ratio (SNR) template param that Z ˜ characterize system s ( f )˜ h ( f, λ µ ) detector noise Yunes ρ 2 ∼ d f template (projection of (spectral noise S n ( f ) GW metric perturbation) density) Extreme Gravity GW Tests Implications Yunes 13

How do we build GW models? Yunes [Blanchet, LRR] Extreme Gravity GW Tests Implications Yunes 14

Roadmap Extreme Gravity GW Tests Implications Yunes 15

What Physics do GWs Probe? Curvature Strength Extreme Gravity Tests Weak Field Tests Field Strength GWs probe eXtreme Gravity [Will, Liv. Rev., 2005, Psaltis, Liv. Rev., 2008, Baker, et al, Siemens & Yunes, Liv. Rev. 2013, Yunes, et al PRD 2016] Extreme Gravity GW Tests Implications Yunes 16

Extreme Gravity versus Strong Gravity [Yunes, Yagi, Pretorius, PRD ’16] Extreme Gravity GW Tests Implications Yunes 17

How are GW Probes of Extreme Gravity Different? 1. Extreme Gravity: Sources : Compact Object Coalescence, SN, deformed NSs, etc. Processes : Generation & Propagation of metric perturbation 2. Clean: Absorption is negligible, lensing unimportant at low z, accretion disk and magnetic fields unimportant during inspiral. [Yunes, et al PRL (’11), Kocsis, et al PRD 84 (’11), Barausse, et al PRD 89 (’14)] 3. Localized: Point sources in spacetime Constraint Maps [Yunes & Pretorius, PRD 81 (’10)] Extreme Gravity GW Tests Implications Yunes 18

What can we learn from GWs? Generation Eg Case Study: Dipole Radiation Conservation laws disallow dipole ˙ E b = − L = − ( L GW + L θ ) radiation in GR, but not in mod gravity ⌘ 10 ⇣ v D ... ij E ... L GW ∼ I ij I ∼ Dipole radiation removes energy more c effectively than quadrupole radiation ⇣ v ⌘ 8 D D i E D i ¨ ¨ L θ ∼ ∼ c Dipole radiation forces binary to inspiral faster and GWs to chirp faster ◆ − 1 ✓ dE ✓ dE ◆ Ψ GW = ˙ GW Phase is sensitive fT 2 T 2 g = g d f dt to rate of inspiral ∼ ( π Mf ) − 5 / 3 + β θ ( π Mf ) − 7 / 3 Extreme Gravity GW Tests Implications Yunes 19

What can we learn from GWs? Propagation Eg Case Study: Massive Graviton Special Relativity tells us that for a propagating massive particle GWs emitted close to merger travel faster than those emitted in the early inspiral. GW Phase is sensitive to the GW frequency x GW travel time Massive graviton effect accumulates with distance travelled. [Will, PRD 1998, Will & Yunes, CQG 2004, Berti, Buonanno & Will, CQG 2005 Mirshekari, Yunes & Will, PRD 2012] Extreme Gravity GW Tests Implications Yunes 20

GW Tests of Principles, not Theories The parameterized post-Einsteinian Framework [Yunes & Pretorius, h GR ( f ) (1 + α f a ) e i β f b ˜ h ( f ) = ˜ PRD 2009] [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).] Extreme Gravity GW Tests Implications Yunes 21

Classification of Inferences Gravitational Gravitational Wave Generation Wave Propagation Scalar/Vector Field Activation Modified Dispersion Relations Gravitational Parity Violation Modified Kinematics Gravitational Lorentz Violation Gravitational Lorentz Violation Extra-Dimensional Leakage Cosmological Screening Test Fundament Time-Variation of G Time-Variation of G al Pillars of GR Spacetime Dimensionality Speed of Gravity Parity Violation Mass of Graviton Lorentz Violation Lorentz Violation SEP Violation SEP Violation Extreme Gravity GW Tests Implications Yunes 22

Roadmap Extreme Gravity GW Tests Implications Yunes 23

LIGO’s First Direct Detection of GWs GW151226 WAVES People LIGO GW150914 Black Holes Not What [New York Times, Front Page, 2016] [LIGO, PRL, ’16] Extreme Gravity GW Tests Implications Yunes 24

Properties of GW150914 m 1 = 35 . 7 +5 . 4 � 3 . 8 M � m 2 = 29 . 1 +3 . 8 � 4 . 4 M � | ~ 1 = 0 . 31 +0 . 48 S 1 | /m 2 − 0 . 28 | ~ 2 = 0 . 46 +0 . 48 S 2 | /m 2 − 0 . 42 m f = 61 . 8 +4 . 2 � 3 . 5 M � | ~ f = 0 . 67 +0 . 05 S f | /m 2 − 0 . 07 D L = 410 +160 − 180 Mpc z = 0 . 088 +0 . 031 − 0 . 038 [LIGO, PRL, ’16] Extreme Gravity GW Tests Implications Yunes 25

Consistency with GR [Littenberg & Cornish] 10 10 data data MAP waveform residual whitened amplitude whitened amplitude 5 5 0 0 -5 -5 -10 -10 -0.5 -0.5 -0.4 -0.4 -0.3 -0.3 -0.2 -0.2 -0.1 -0.1 0 0 0.1 0.1 t-t peak (s) t-t peak (s) SNR of Residual (data - best fit) is consistent with noise Extreme Gravity GW Tests Implications Yunes 26

GW Constraints on Modified Generation Weaker Gravity Stronger Gravity [Yunes, Yagi, Anomalous Parity Scalar Dipole Lorentz Pretorius, Acceleration Violation Radiation Violation PRD ‘16] Extreme Gravity GW Tests Implications Yunes 27

GW Constraints on Modified Propagation Superluminal E 2 = ( pc ) 2 + A ( pc ) α ⇣ v g ⌘ 2 = 1 + ( α − 1) A E α − 2 c Subluminal …. —> SME (5.5PN, 7PN) [Yunes, Yagi, Doubly Massive Multifractal SME, Horava-Lifshitz, Pretorius, Special Relativity Graviton Spacetime Extra-Dimensions PRD ‘16] Extreme Gravity GW Tests Implications Yunes 28

Theory Implications of GW observations [Yunes, Yagi, Pretorius, PRD ‘16] Extreme Gravity GW Tests Implications Yunes 29

Conclusions Gravitational Wave Tests Are Special Probes of Physics (extreme gravity, clean, localized, constraint maps) Model-Independent Framework To Search For Anomalies In The Data Allows For Constraints On Deviations (parameterized post-Einsteinian and Bayesian model selection) Gravitational Waves Are Already Telling Us About Theoretical Physics (Lorentz violation, graviton mass, dipole emission, higher curvature action, screening mechanisms, no-hair theorem) Modified Theories Must Pass A New High Bar Doveryai, no proveryai (They must be consistent with LIGO’s observations of BHs and GWs) Yunes 30

Thank You Yunes 31