GRAVITATIONAL WAVES The Child of General Relativity.

Slides:



Advertisements
Similar presentations
by Robert Nemiroff Michigan Technological University
Advertisements

The sound of the Universe: The search for Gravitational Waves Giovanni Santostasi, Ph. D. Baton Rouge Community College, Baton Rouge, LA.
Chapter 18: Relativity and Black Holes
15.1Tenets of General Relativity 15.2Tests of General Relativity 15.3Gravitational Waves 15.4Black Holes General Relativity CHAPTER 15 General Relativity.
Extragalactic Astronomy & Cosmology First-Half Review [4246] Physics 316.
Neutron Stars and Black Holes
Jonathan Gair Graduate Seminar, St.Catharine’s College, 28 th November 2005 The Black Hole Symphony – listening to the Universe with gravitational waves.
1 Science Opportunities for Australia Advanced LIGO Barry Barish Director, LIGO Canberra, Australia 16-Sept-03 LIGO-G M.
Jonathan Gair Extragalactic Group Seminar, IoA, 21 st November 2005 Gravitational Wave Detection – current status & future prospects.
Spacetime: just when you thought it was it throws you a.
Edmund Bertschinger MIT Department of Physics and Kavli Institute for Astrophysics and Space Research General Relativity and Applications 2. Dynamics of.
Semester Physics 1901 (Advanced) A/Prof Geraint F. Lewis Rm 560, A29
2/9/2006Welcome to LIGO1 Welcome to LIGO!. 2/9/2006Welcome to LIGO2 LIGO: A detector that measures very tiny displacements How tiny?
General Relativity Physics Honours 2005 Dr Geraint F. Lewis Rm 557, A29
Gravitational waves LIGO (Laser Interferometer Gravitational-Wave Observatory ) in Louisiana. A laser beam is.
Entanglement of cats |   =  |  +  |  Teleportation: making an exact replica of an arbitrary quantum state (while destroying the original...)
1 Observing the Most Violent Events in the Universe Virgo Barry Barish Director, LIGO Virgo Inauguration 23-July-03 Cascina 2003.
Gravitational-waves: Sources and detection
LIGO -- Studying the Fabric of the Universe LIGO-GOxxxx Barry C. Barish National Science Board LIGO Livingston, LA 4-Feb-04.
What are Gravity Waves?. According to Einstein's theory of gravity, an accelerating mass causes the fabric of space-time to ripple like a pond disturbed.
Gravitational Waves. Prediction General Relativity – 1915 Gravity is not the pulling force envisioned by Kepler or Newton Space warps around massive objects.
25 Facts about Parkes, Pulsars and
The Search for a Stochastic Background of Gravitational Radiation Part I Rosa M. Luna, D. Auzmus, M. Casquette, C.W. Torres, M.C. Diaz, J.D. Romano, and.
Brennan Ireland Rochester Institute of Technology Astrophysical Sciences and Technology December 5, 2013 LIGO: Laser Interferometer Gravitational-wave.
Chapter 34 Electromagnetic Waves. Currents produce B Change in E produces B Currents produce B Change in E produces B Change in B produces an E charges.
Chapter 9 Electromagnetic Waves. 9.2 ELECTROMAGNETIC WAVES.
1 LISA Science and Concept Robin T. Stebbins. 2 May 13, 2003 LISA Overview The Laser Interferometer Space Antenna (LISA) is a joint ESA- NASA mission.
GridLab, Eger, 31 Mar-1 Apr Potential Gravitational Applications of Grid B.S. Sathyaprakash GridLab conference, 31.
What are GW’s ?? Fluctuation in the curvature of space time, propagating outward form the source at the speed of light Predicted by Einstein’s GTR Gravitational.
Paik-1 Search for Gravitational Waves Ho Jung Paik University of Maryland and Seoul National University January 12, 2006 Seoul, Korea KIAS-SNU Physics.
M H Maps of space Space: N & E or M & H Electromagnetism: E & B or E & B.
Gravitational Waves (& Gravitons ?)
Gravitational Wave Arezu Dehghafnar Physics Department SUT.
LIGO-G Black holes, Einstein, and space-time ripples Peter R. Saulson Syracuse University.
Einstein’s elusive waves
NS 1300 Dr. Hoge.  Can we slow light down?  Can we make things invisible?  Is it possible to travel faster than the speed of light?  Is faster than.
Copyright © 2010 Pearson Education, Inc. Neutron Stars and Black Holes Unit 9.
Black Holes Escape velocity Event horizon Black hole parameters Falling into a black hole.
LIGO-G D Enhanced LIGO Kate Dooley University of Florida On behalf of the LIGO Scientific Collaboration SESAPS Nov. 1, 2008.
1 Chapter 3 Electromagnetic Theory, Photons and Light September 5,8 Electromagnetic waves 3.1 Basic laws of electromagnetic theory Lights are electromagnetic.
 Newtonian relativity  Michelson-Morley Experiment  Einstein ’ s principle of relativity  Special relativity  Lorentz transformation  Relativistic.
Fundamental Principles of General Relativity  general principle: laws of physics must be the same for all observers (accelerated or not)  general covariance:
Black Holes - Observation How do you see something you can’t see ?????
18/04/2004New Windows on the Universe Jan Kuijpers Part 1: Gravitation & relativityPart 1: Gravitation & relativity J.A. Peacock, Cosmological Physics,
Principle of Equivalence: Einstein 1907 Box stationary in gravity field Box falling freely Box accelerates in empty space Box moves through space at constant.
Physics 1202: Lecture 18 Today’s Agenda Announcements: –Lectures posted on: –HW assignments, etc.
8 June 2004Summer School on Gravitational Wave Astronomy 1 Gravitational Wave Detection #1: Gravity waves and test masses Peter Saulson Syracuse University.
Gravitational Waves ASTR 3010 Lecture 24.
Gravitational Wave Astronomy Gregory Harry Massachusetts Institute of Technology April 25, 2006 Hobart and William Smith Colleges G R.
High energy Astrophysics Mat Page Mullard Space Science Lab, UCL 13. Gravitational waves.
Gravitational Waves.
DECIGO – Japanese Space Gravitational Wave Detector International Workshop on GPS Meteorology January 17, Tsukuba Center for Institutes Seiji Kawamura*
LIGO-G D LIGO Laboratory1 Stoyan Nikolov LIGO-G D The LIGO project’s quest for gravitational waves Presenting LIGO to the students of.
Gravitational Wave Observatories By: Matthew Fournier.
General Relativity and Cosmology The End of Absolute Space Cosmological Principle Black Holes CBMR and Big Bang.
LIGO G M Intro to LIGO Seismic Isolation Pre-bid meeting Gary Sanders LIGO/Caltech Stanford, April 29, 2003.
Gravitational waves Gideon Koekoek January 9 th 2008 Research done at Nikhef.
LOGO Gravitational Waves I.S.Jang Introduction Contents ii. Waves in general relativity iii. Gravitational wave detectors.
Gravitational Waves Earth expands and contracts by the diameter of an atomic nucleus: cm A world-shaking discovery.
Brief summaries on general relativity (II) Gungwon Kang (KISTI) July 26, 2015 at Int’l Summer School on NR & GW, KAIST in Korea.
The search for those elusive gravitational waves
Current and future ground-based gravitational-wave detectors
The Search for Gravitational Waves with Advanced LIGO
Gravitational Waves: On the Brink of a New Astronomy
2017 Nobel Prize in Physics: Discovery of Gravitational Waves
Black holes, neutron stars and binary star systems
GW150914: The first direct detection of gravitational waves
A world-shaking discovery
The First Ever Detection of Gravity Waves
Gideon Koekoek January 10th 2007
Presentation transcript:

GRAVITATIONAL WAVES The Child of General Relativity

A NECESSARY CHANGE Concepts after Einstein :- Time is not absolute There is no ether frame Notion of spacetime Concepts before Einstein :- There is a preferred reference frame ether Time is absolute 3 dimensional universe

SPACETIME Spacetime (also space–time, space time or spacetime continuum) is any mathematicalmodel that combines space and time into a single Interwoven continuum. Wikipedia  Event as a point in four dimension.  Space and time intervals of one coordinate system gets intermixed to give those intervals in another coordinate system.  Transformations in special relativity can be interpreted as rotation of coordinate system (realised by Minkowski).

'CROOKED' AND 'STRAIGHT'  Space was thought to be 'flat' or 'Euclidean'  In GR Einstein showed that spacetime gets curved in presence of mass.  Gravitation was interpreted as a consequence of curved spacetime.  Well, it was not a mere 'interpretation', it was a new physics. This model of gravitation gives different predictions than Newton's model.  Experiments confirmed that Einstein was correct.

GRAVITATIONAL WAVES Gravitational waves are ripples in the curvature of spacetime that propagate as a wave, travelling outward from the source. Wikipedia Emerge as solution of Einstein's field equations in linear approximation. There are both similarities and dissimilarities with EM waves.

ORIGIN OF GW Curvature of spacetime depends on the mass per unit volume at any region. When mass moves the curvature changes. The changes of curvature due to accelerating object propagates at speed of light. This is called gravitational wave.  Similar origin of EM waves.  Both travel at the speed of light (in vacuum)

SOURCES OF GW  Two objects orbiting each other in a quasi-Keplerian planar orbit (basically, as a planet would orbit the Sun) will radiate.  A spinning non-axisymmetric planetoid — say with a large bump or dimple on the equator — will radiate.  A supernova will radiate except in the unlikely event that the explosion is perfectly symmetric.  An isolated non-spinning solid object moving at a constant velocity will not radiate. This can be regarded as a consequence of the principle of conservation of linear momentum.  A spinning disk will not radiate. This can be regarded as a consequence of the principle of conservation of angular momentum. However, it will show gravitomagnetic effects.  A spherically pulsating spherical star (non-zero monopole moment or mass, but zero quadrupole moment) will not radiate, in agreement with Birkhoff's theorem. Wikipedia Accelerating mass provided its motion is not spherically or cylindrically symmetric

SOME PROPERTIES o Gravitation is very weak compared to electromagnetic forces. So gravitational wave is hard to detect. o Gravitational waves comes in two types of polarizations: plus polarization and X polarization

SOME PROPERTIES It causes oscillating motion of bodies perpendicular to its direction of motion Motion of beads placed perpendicular to plus polarized wave Motion of beads placed perpendicular to cross polarized wave

DIFFERENCES WITH EM WAVES  Mathematically, EM waves arises as solution of Maxwell's equations without any approximation. But GW arises as solution in linear approximation.  GW are not absorbed by intervening medium. They can travel through matter of any composition or density.  Photons are themselves neutral. But gravitons themselves are massive. Mass is cause of gravitation. So the nonlinearity of field equations.

IMPORTANCE  One of the triumphs of general relativity  It will complete Big-Bang model “Other than finding life on other planets or directly detecting dark matter, I can’t think of any other plausible near-term astrophysical discovery more important than this one for improving our understanding of the universe,” Caltech theoretical physicist Sean Carroll

GRAVITATIONAL WAVE DETECTION

GRAVITATIONAL WAVES Emitted by a massive object, or group of objects, whose shape or orientation changes rapidly with time Changes the geometry of space in a time-varying way Strength and polarization depend on direction relative to source Can be a linear combination of polarization components “Plus” polarization “Cross” polarizationCircular polarization

GW DETECTION I – INDIRECT Binary pulsars Observe binary systems with optical & radio telescopes. See changes in orbit due to loss of energy to GWs. Best test of GR to date – J (Hulse/Taylor Nobel Prize 1993), J Pulsar timing GWs propagating across line of sight from a pulsar to an observer change light travel time. See this time shift in pulse timing.

GW DETECTION II – RESONANT BARS A large cylinder of metal resonates when bathed in gravitational waves of the right frequency. Detectors must be suspended to give seismic isolation. Cryogenic cooling reduces thermal noise. First ever GW detector was a resonant aluminium bar. Today there are several increasingly sophisticated experiments in operation – ALLEGRO (US), AURIGA (Italy), EXPLORER (CERN), NAUTILUS (Italy), NIOBE (Australia), GRAIL (Netherlands)

GW DETECTION III – INTERFEROMETERS Interferometers exploit quadrupole nature of GWs – send laser beams in perpendicular directions and combine them on return to construct interference patterns.

LASER INTERFEROMETERS Measure difference in arm lengths to a fraction of a wavelength Responds to one polarization component Antenna Pattern of a Laser Interferometer Directional sensitivity depends on polarization of waves “  ” polarization RMS sensitivity

GROUND BASED INTERFEROMETERS Several ground based interferometers are now operating or are being built – LIGO – US project. Two 4km and one 2km detector. GEO – British/German project. One 600m detector. VIRGO – Italian/French project. One 3km detector. TAMA – Japanese project. One 300m detector. AIGO – Australian project. One 80m detector.

SPACE BASED INTERFEROMETERS A space based interferometer, LISA, is planned Joint NASA/ESA mission. Will consist of three satellites in a heliocentric, earth-trailing orbit. Longer baseline (5 million km) gives sensitivity to lower frequency gravitational waves. Launch date is LISA will be a true GW telescope – confusion between multiple sources dominates over instrumental noise throughout much of the spectrum.

INTERFEROMETERS - SOURCES

DIFFICULTIES IN GW DETECTION Gravitational waves are very weak and weakly interacting. Events are faint, typically an order of magnitude below the noise. Detection will be by matched filtering using a bank of templates. Overlap of template with data pulls signal out of the noise. +

“GW DETECTIONS” TO DATE - BARS In the late 60s/early 70s, Joseph Weber claimed to have made coincident detections in two detectors, 1000km apart. The claim was never verified and is regarded skeptically. In 2002, the EXPLORER and NAUTILUS teams announced an excess of events towards the galactic centre. – These results are highly controversial, even though no claim of a “detection” was actually made – The statistics used in analysing the data are extremely suspect

THANK YOU