DOCSLIB.ORG

Einstein and Thermal Noise

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Einstein and Thermal Noise Einstein’s Dual Legacy: Thermal Noise and Gravitational Waves Gregory Harry LIGO Laboratory Massachusetts Institute of Technology University of Mississippi Department of Physics and Astronomy February 5, 2008 LIGO-G080023-00-R 1 Outline Show how understanding two of Einstein’s great ideas will allow for the birth of gravitational astronomy… • Two of Einstein’s Great Ideas – Brownian Motion – Gravitational Waves • Gravitational Wave Detection – Detection Methods – Astronomical Sources • Sensitivity and Detectability – Thermal Noise Limitations – Future Ideas and Detectors 2 Einstein and Thermal Noise Einstein’s first challenge to LIGO: “I did not believe that it was possible to study Brownian motion with such a precision.” -Letter from Albert Einstein to Jean Perrin (1909) • Einstein’s Brownian motion paper “On the motion of small particles suspended in liquids at rest required by the molecular-kinetic theory of heat”, Annalen der Physik 17 (1905) 549. – Most cited of all Einstein’s papers • Linked fluctuations to fluid viscosity • Confirmed statistical physics models – Atoms as basic units of matter – Kinetic theory of heat • Also contributed to the theory of lasers (Einstein’s A and B coefficients) 3 Thermal Noise Fluctuations from heat bath • Mechanical ⇒ Brownian motion • Electrical ⇒ Johnson noise • Optical ⇒ Thermorefraction • Others Brownian Motion in Fluid Related to energy loss in system – Viscosity for particle in fluid – Resistance in Johnson noise – Internal friction for mechanical systems Sv Callen and Welton’s Fluctuation- Dissipation Theorem 4 Fluctuation-Dissipation Theorem • Nyquist (1920s) proposed general relationship between energy loss and thermal noise • Callen and Welton (1950s) proved Fluctuation- Dissipation Theorem • Path for energy loss also a path for thermal excitation • Thermal equilibrium required Fluctuation s • Thermal bath can be Dissipatio same system n 5 Gravitational Waves Einstein’s second challenge to LIGO: “Do Gravitational Waves Exist?”-Title of paper submitted to (and rejected by) Physical Review by Einstein and Rosen (1936) • Einstein’s General Theory of Relativity Gμν= 8π Tμν – Analogous to Maxwell’s equations – Has wave solution • Oscillations in space-time • Propagate at c 1975 1985 1995 • Two polarizations: X and + Indirect Detection (1990s) • Binary Pulsar System 1913+16 • Nobel Prize 1993 Joseph Taylor and Russel Hulse 6 Gravitational Waves Comparison with Electromagnetic Waves • Quadrupolar – Influences design of detectors – Dipole (E&M) forbidden by momentum conservation Electromagnetic Wave • Much Weaker 5 2 L ~ G/c L internal G/c5 ≈ 2.5 10 -35 1/W • Strain rather than force h = ΔL / L ≈ 10 -21 Gravitational Wave 7 Detection of Gravitational Waves Interferometers • Light goes down two perpendicular arms – Similar to Michelson- Morley • Mirrors are free to move – Gravity or other forces • Returning light recombines – Constructively: equal arm length – Destructively: different arm lengths • Gravitational wave Interference of Light – Stretch one arm, shrink other 8 Laser Interferometer Gravitational-wave Observatory (LIGO) End Test Mirror Whole Interferometer Enclosed in Vacuum Input Test 4 km Fabry-Perot cavities Mirror Recycling 100 W Mirror Laser/MC 6 W 13 kW LIGO Livingston LIGO Hanford 0.2 W • Two sites in the US – Livingston, LA – Hanford, WA • Arms 4 km long (2 km for 2nd • SensitiveHanford) to strains around h=10-21 • ΔL = h L ≈ 10-18 m: subnuclear • Entire beam path in vacuum LIGO Vacuum Chambers 9 Generations of LIGO Initial, Enhanced, and Advanced Initial LIGO • Reached design sensitivity – Neutron star inspiral: 15 Mpc • Steel wire suspensions • Standard coatings on silica 10 Hz 100 Hz 1000 Hz Enhanced LIGO Advanced LIGO • Improvements to Initial • Major upgrade LIGO – Neutron star inspiral: 170 Mpc – Neutron star inspiral: 30 Mpc • Silica ribbon suspensions • Steel wire suspensions • Improved coatings on silica • Standard coatings on silica • Funding 4/08: Online 2013 • Begin taking data 2009 10 Initial LIGO Sensitivity LIGO Sensitivity in Time Initial LIGO Noise • Sensitivity improves over time • Data taken at most sensitivities – Technical checks – Upper limits on sources 10 Hz 100 Hz 1000 Hz • Design sensitivity - 2005 Science Data Run (S5) • Full year of coincidence between three interferometers • Two years of calendar time S5 Coincidence • Finished November 2007 11 World Network of Detectors GEO 600 in LIGO Germany Proposed LCGT in Japan Virgo 3 km in Italy Gingin site in Australia 12 Astronomical Sources Short Duration Long Duration Modeled Compact Body Inspirals Periodic Sources Unmodeled Bursts Stochastic Background 13 Astrophysical Results Inspirals Numerical Model of Inspiral Gamma Ray Bursts • GRB070201 – Galaxy M31 (750 kPc away) – NO inspiral or short transients – NOT binary neutron star inspiral – arXiv:0711.1163, ApJ • Over 200 GRBs during S5 – Analysis underway High density objects – ~10% short GRBs ⇒ likely to be in mutual orbit inspirals –Black holes – Long GRBs could be supernova –Neutron stars –White dwarfs 14 Astrophysical Results Bursts Gamma Ray Repeaters • Catastrophic events • Hyperflare in SGR 1806-20 – 10s of solar masses – Magnetar ~ 6 - 15 kPc away – Supernova etc – NO signals found at normal • Sources not mode frequencies modeled – Not during S5 – No theoretical model – Only Hanford 4 km detector – Non-optimal search – Phys Rev D 76 (2007) 062003. • Hyperflare in SGR 1900+14 – During S5 – Analysis underway Artists Conception of Hyperflare 15 Astrophysical Results Periodic • Rapidly rotating Crab Pulsar compact body • Position, frequency & spin – Pulsar down rate known – Low mass X-ray binary • NO signal seen • Needs asymmetry – Spin down NOT from gravitational waves – Sphere not • Limits on 78 other pulsars quadrupolar – Phys Rev D 76 (2007) 042001. Sensitivity to Pulsars Artists Conception of Accretion 16 Einstein @ Home http://einstein.phys.uwm.edu/ • Based on SETI@Home • Searching for unknown pulsars • Operating systems: – Windows – Mac – OSX – Linux • More computing power • Low cost 17 Astrophysical Results Stochastic Cosmic Microwave Background Big Bang • Similar to cosmic microwave background • Probe closer to beginning • Tests of inflation, quantum gravity, etc. Cosmological Nearby Sources Background • Unresolved background • NO correlated signal seen of burst type sources • Similar to theoretical limit • Distant supernova, -6 mergers, accretions, etc. – ΩGW < 9 10 (preliminary) – Assumes frequency independent spectrum 18 Noise in Inteferometric Indirect Laser NoiseDetectors – Direct Laser Noise – Radiation Pressure Shot Noise Suspension Thermal Noise Seismic Noise 10 Hz 100 Hz 1000 Hz Coating Thermal Noise Coating Thermal Noise -Brownian – Thermo-optic 19 Shaping Laser Noise Dual Recycling High Frequency Narrowband Dual Recycling Laser Thermal -22 • Laser noise can be shaped 10 Noises Laser Noise Noises – Mirror reflectivity and 1/2 -23 10 positions h(f) /Hz h(f) – Laser power -24 10 • Laser noise can optimized 10 Hz 100 Hz -25 Thermal Noises for different sources 10 2 3 10 10 100 Hz Frequency (Hz)1000 Hz • High frequency narrowband Laser Noise – Known pulsars • Low frequency – Stochastic background Thermal Noises • Mid frequency broadband 10 Hz 100 Hz – Inspirals and bursts Low Frequency Optimized 20 Thermal Noise and Sensitivity Wideband: Inspirals and Bursts • Coating thermal noises limit sensitivity • Improved coatings in Advanced LIGO – Titania doped Tantala/Silica Thermal Noises – Increased laser spot size 10 Hz 100 Hz 1000 Hz – Optimize design to reduce Wideband Advanced LIGO Sensitivity thermal noise – Sensitivity greatly improved • Inspiral range increased Generation Neutron Star 10 M BH – Neutron star binaries o Enhanced LIGO 30 Mpc 180 Mpc – Black hole binaries Advanced LIGO 170 Mpc 980 Mpc • Burst sensitivity also improved Next Generation 300 Mpc 1600 Mpc Depends on noise 21 Thermal Noise and Sensitivity High Frequency Narrowband: Pulsars Low Mass X-ray Binaries • Narrowband Advanced LIGO • Coating thermal noise-limited – Brownian Thermal Noises – Thermo-optic • Gravitational waves depend on 150 Hz 500 Hz ellipticity (ε) Narrowband Advanced LIGO Sensitivity High Frequency Pulsars Generation Crab ε Sco X-1 ε • Crab Pulsars and others (59.9 Hz) (620 Hz) • Coating thermal noise- Enhanced LIGO 7 10-6 1 10-7 limited Advanced LIGO 7 10-7 1 10-8 • Laser, suspension thermal, Next Generation 2 10-7 7 10-9 & seismic noises play roles 22 Thermal Noise and Sensitivity Low Frequency : Stochastic Stochastic Sensitivity • Only at low frequency – Frequency scale: c / D ~ 100 Hz Thermal Noises • Limited by thermal noise 10 Hz 100 Hz – Suspension at lowest Low Frequency Advanced LIGO Sensitivity frequencies – Coating at higher frequencies Stochastic Signal LIGO Suspension Stochastic • Depends on model Generation Background – Many ideas Enhanced LIGO Steel Wire 6 10-7 – Unknown in practice Advanced LIGO Silica Ribbon 1 10-9 • Frequency dependence Next Generation Sapphire Ribbon 3 10-10 – Also unknown 23 Next Generation Research 2 2 2 Sx(f) = kB Td Ycoatφ/ (π f w Ysub ) -23 (From 2007 Ops Proposal) 10 Coating Brownian • New coating materials – φ, Thermal Coating TO Suspension Thermal Ycoat Noises Newtonian Seismic • Reduce coating thickness - Quantum Noise d – Cavity reflectors – Corner reflectors Strain SensitivityStrain [1/rt(Hz)] • Change geometry - w Laser – Mesa beams and other Noise-24 shapes 10 1 2 3 10 10 10 • Reduce temperature - T 10 Hz 100Frequency Hz Hz] 1000 Hz – Cryogenics – Japanese 2nd generation Laser • New substrates
Load more

Recommended publications
  • General Relativistic Gravity in Core Collapse SN: Meeting the Model Needs
    General Relativistic Gravity in Core Collapse SN: Meeting the Model Needs Lee Samuel Finn Center for Gravitational Wave Physics Meeting the model needs • Importance of GR for SN physics? • Most likely quantitative, not qualitative, except for questions of black hole formation (when, how, mass spectrum)? • Gravitational waves as a diagnostic of supernova physics • General relativistic collapse dynamics makes qualitative difference in wave character Outline • Gravitational wave detection & detector status • Detector sensitivity • Gravitational waves as supernova physics diagnostic LIGO Status • United States effort funded by the National Science Foundation • Two sites • Hanford, Washington & Livingston, Louisiana • Construction from 1994 – 2000 • Commissioning from 2000 – 2004 • Interleaved with science runs from Sep’02 • First science results gr-qc/0308050, 0308069, 0312056, 0312088 Detecting Gravitational Waves: Interferometry t – Global Detector Network LIGO miniGRAIL GEO Auriga CEGO TAMA/ LCGT ALLEGRO Schenberg Nautilus Virgo Explorer AIGO Astronomical Sources: NS/NS Binaries Now: N ~1 MWEG • G,NS over 1 week Target: N ~ 600 • G,NS MWEG over 1 year Adv. LIGO: N ~ • G,NS 6x106 MWEG over 1 year Astronomical Sources: Rapidly Rotating NSs range Pulsar 10-2-10-1 B1951+32, J1913+1011, B0531+21 10-3-10-2 -4 -3 B1821-24, B0021-72D, J1910-5959D, 10 -10 B1516+02A, J1748-2446C, J1910-5959B J1939+2134, B0021-72C, B0021-72F, B0021-72L, B0021-72G, B0021-72M, 10-5-10-4 B0021-72N, B1820-30A, J0711-6830, J1730-2304, J1721-2457, J1629-6902, J1910-5959E,
    [Show full text]
  • Determination of the Neutron Star Mass-Radii Relation Using Narrow
    Determination of the neutron star mass-radii relation using narrow-band gravitational wave detector C.H. Lenzi1∗, M. Malheiro1, R. M. Marinho1, C. Providˆencia2 and G. F. Marranghello3∗ 1Departamento de F´ısica, Instituto Tecnol´ogico de Aerona´utica, S˜ao Jos´edos Campos/SP, Brazil 2Centro de F´ısica Te´orica, Departamento de F´ısica, Universidade de Coimbra, Coimbra, Portugal 3Universidade Federal do Pampa, Bag´e/RS, Brazil Abstract The direct detection of gravitational waves will provide valuable astrophysical information about many celestial objects. The most promising sources of gravitational waves are neutron stars and black holes. These objects emit waves in a very wide spectrum of frequencies determined by their quasi-normal modes oscillations. In this work we are concerned with the information we can ex- tract from f and pI -modes when a candidate leaves its signature in the resonant mass detectors ALLEGRO, EXPLORER, NAUTILUS, MiniGrail and SCHENBERG. Using the empirical equa- tions, that relate the gravitational wave frequency and damping time with the mass and radii of the source, we have calculated the radii of the stars for a given interval of masses M in the range of frequencies that include the bandwidth of all resonant mass detectors. With these values we obtain diagrams of mass-radii for different frequencies that allowed to determine the better candi- dates to future detection taking in account the compactness of the source. Finally, to determine arXiv:0810.4848v4 [gr-qc] 21 Jan 2009 which are the models of compact stars that emit gravitational waves in the frequency band of the mass resonant detectors, we compare the mass-radii diagrams obtained by different neutron stars sequences from several relativistic hadronic equations of state (GM1, GM3, TM1, NL3) and quark matter equations of state (NJL, MTI bag model).
    [Show full text]
  • Taming the Quantum Noisehow Quantum Metrology Can Expand the Reach of Gravitational-Wave Observatories
    Taming the quantum noise How quantum metrology can expand the reach of gravitational-wave observatories Dissertation zur Erlangung des Doktorgrades an der Fakultat¨ fur¨ Mathematik, Informatik und Naturwissenschaen Fachbereich Physik der Universitat¨ Hamburg vorgelegt von Mikhail Korobko Hamburg 2020 Gutachter/innen der Dissertation: Prof. Dr. Ludwig Mathey Prof. Dr. Roman Schnabel Zusammensetzung der Prufungskommission:¨ Prof. Dr. Peter Schmelcher Prof. Dr. Ludwig Mathey Prof. Dr. Henning Moritz Prof. Dr. Oliver Gerberding Prof. Dr. Roman Schnabel Vorsitzende/r der Prufungskommission:¨ Prof. Dr. Peter Schmelcher Datum der Disputation: 12.06.2020 Vorsitzender Fach-Promotionsausschusses PHYSIK: Prof. Dr. Gunter¨ Hans Walter Sigl Leiter des Fachbereichs PHYSIK: Prof. Dr. Wolfgang Hansen Dekan der Fakultat¨ MIN: Prof. Dr. Heinrich Graener List of Figures 2.1 Effect of a gravitational wave on a ring of free-falling masses, posi- tioned orthogonally to the propagation direction of the GW. 16 2.2 Michelson interferometer as gravitational-wave detector. 17 2.3 The sensitivity of the detector as a function of the position of the source on the sky for circularly polarized GWs. 18 2.4 Noise contributions to the total design sensitivity of Advanced LIGO in terms of sensitivity to gravitational-wave strain ℎ C . 21 ( ) 2.5 Sensitivity of the GW detector enhanced with squeezed light. 28 3.1 Effect of squeezing on quantum noise in the electromagnetic field for coherent field, phase squeezed state and amplitude squeezed state. 46 3.2 Schematic of a homodyne detector. 52 3.3 Sensing the motion of a mirror with light. 55 3.4 Comparison of effects of variational readout and frequency-dependent squeezing on quantum noise in GW detectors.
    [Show full text]
  • Ripples in the Fabric of Space-Time
    Papers and Proceedings of the Royal Society of Tasmania, Volume 150(1), 2016 9 RIPPLES IN THE FABRIC OF SPACE-TIME by Jörg Frauendiener (with three text-figures and four plates) Frauendiener, J. 2016 (31:viii): Ripples in the fabric of space-time. Papers and Proceedings of the Royal Society of Tasmania 150(1): 9–14. https://doi.org/10.26749/rstpp.150.1.9 ISSN 0080-4703. Department of Mathematics and Statistics, University of Otago, P.O. Box 56, Dunedin 9054, New Zealand. Email: [email protected] Einstein’s general theory of relativity is one of the finest achievements of the human mind. It has fundamentally changed the way we think about space and time, and how these in turn interact with matter. Based on this theory Einstein made several predictions, many of which have been verified experimentally. Among the most elusive phenomena that he predicted are gravitational waves, ripples in the fabric of space-time. They are disturbances in the space-time continuum which propagate with the speed of light. This contribution describes some of their properties, their sources and how it is intended to detect them. Key Words: general relativity, gravitational waves, space-time, black holes, gravitational physics, Einstein’s theory of gravitation. mass are equivalent. This is the (weak) principle of equivalence. INTRODUCTION It is the foundation on which the general theory of relativity is built upon. It is therefore essential that it is continuously One hundred years ago, on 25 November 1915, Albert checked experimentally with as many different and more Einstein presented to the Prussian Academy of Sciences accurate experiments as possible.
    [Show full text]
  • Gravitational Waves∗
    Vol. 38 (2007) ACTA PHYSICA POLONICA B No 12 GRAVITATIONAL WAVES ∗ Kostas D. Kokkotas Theoretical Astrophysics, University of Tübingen Auf der Morgenstelle 10, 72076 Tübingen, Germany and Department of Physics, Aristotle University of Thessaloniki Thessaloniki 54124, Greece [email protected] (Received October 23, 2007) Gravitational waves are propagating fluctuations of gravitational fields, that is, “ripples” in space-time, generated mainly by moving massive bodies. These distortions of space-time travel with the speed of light. Every body in the path of such a wave feels a tidal gravitational force that acts per- pendicular to the wave’s direction of propagation; these forces change the distance between points, and the size of the changes is proportional to the distance between these points thus gravitational waves can be detected by devices which measure the induced length changes. The frequencies and the amplitudes of the waves are related to the motion of the masses involved. Thus, the analysis of gravitational waveforms allows us to learn about their source and, if there are more than two detectors involved in observation, to estimate the distance and position of their source on the sky. PACS numbers: 04.30.Db, 04.30.Nk 1. Introduction Einstein first postulated the existence of gravitational waves in 1916 as a consequence of his theory of General Relativity, but no direct detection of such waves has been made yet. The best evidence thus far for their existence is due to the work of 1993 Nobel laureates Joseph Taylor and Russell Hulse. They observed, in 1974, two neutron stars orbiting faster and faster around each other, exactly what would be expected if the binary neutron star was losing energy in the form of emitted gravitational waves.
    [Show full text]
  • The Future of Gravitational Wave Astronomy a Global Plan
    THE GRAVITATIONAL WAVE INTERNATIONAL COMMITTEE ROADMAP The future of gravitational wave astronomy GWIC A global plan Title page: Numerical simulation of merging black holes The search for gravitational waves requires detailed knowledge of the expected signals. Scientists of the Albert Einstein Institute's numerical relativity group simulate collisions of black holes and neutron stars on supercomputers using sophisticated codes developed at the institute. These simulations provide insights into the possible structure of gravitational wave signals. Gravitational waves are so weak that these computations significantly increase the proba- bility of identifying gravitational waves in the data acquired by the detectors. Numerical simulation: C. Reisswig, L. Rezzolla (Max Planck Institute for Gravitational Physics (Albert Einstein Institute)) Scientific visualisation: M. Koppitz (Zuse Institute Berlin) GWIC THE GRAVITATIONAL WAVE INTERNATIONAL COMMITTEE ROADMAP The future of gravitational wave astronomy June 2010 Updates will be announced on the GWIC webpage: https://gwic.ligo.org/ 3 CONTENT Executive Summary Introduction 8 Science goals 9 Ground-based, higher-frequency detectors 11 Space-based and lower-frequency detectors 12 Theory, data analysis and astrophysical model building 15 Outreach and interaction with other fields 17 Technology development 17 Priorities 18 1. Introduction 21 2. Introduction to gravitational wave science 23 2.1 Introduction 23 2.2 What are gravitational waves? 23 2.2.1 Gravitational radiation 23 2.2.2 Polarization 24 2.2.3 Expected amplitudes from typical sources 24 2.3 The use of gravitational waves to test general relativity 26 and other physics topics: relevance for fundamental physics 2.4 Doing astrophysics/astronomy/cosmology 27 with gravitational waves 2.4.1 Relativistic astrophysics 27 2.4.2 Cosmology 28 2.5 General background reading relevant to this chapter 28 3.
    [Show full text]
  • Testing General Relativity and Gravitational Physics
    Testing General Relativity and Gravitational Physics June 28, 2019 Suwen Wang At Shanghai Jiaotong University Brief Introduction of Relativity • Special Relativity 1570年《西游记》： 孙悟空一个跟头十万八千里 天上一日，地上一年 D 5.4107 m Time Dilation: t 0.180125287sec dt d 2 v 1 d c 365 c 299792458m / sec dt General Relativity – A theory of gravity Einstein’s Field Equation (1916) 1 R g R 8GT 2 Testing of general relativity falls into two main categories: Predictions from the theory Testing the assumptions of the theory Testing methods involve astronomical observations and physics experiments Due to the weakness of gravitational interaction, the experimental test requires extreme precision. Planet Orbit Precession Perihelion Precession of Mercury (1943) Newton: 5557.62 +/- 0.20 sec/century Observation: 5600.73 +/- 0.41 sec/century Other Perihelion Precession Measurements Planet Gen. Relativity Observed a (sec/century) (sec/century) Mercury 43.03 43.11 MG Venus 8.6 8.4 6 rad/rev Earth 3.8 5.0 (1 e2 )a Icarus 10.3 9.8 Starlight Deflection Arthur Eddington with solar eclipse expedition (1919) 380 stars measured after Eddington Radio signal interferometric measurements yielded more accurate results Modern results agree with GR -4 within 1x10 (VLBI results) 1.7512” 4MG q = c2 R Shapiro Time-delay More Mariner 6 Delay Time delay measured by bouncing radio signals off of: • Mercury • Venus Earth • Mariner 6 spacecraft Less Delay • Mariner 7 spacecraft • Transponder on Mars (0.5%) • Cassini spacecraft (10 ppm) sec) Delay ( Delay Gravitational Redshift
    [Show full text]
  • Towards Detection of Gravitational Waves 1.5 A1B1G1 A3B3G1 1 TAMA A4B1G2 ] Burst –20 0.5 Search
    Towards Detection of Gravitational Waves 1.5 A1B1G1 A3B3G1 1 TAMA A4B1G2 ] Burst –20 0.5 Search 0 –0.5 Barry C. Barish Amplitude [x 10 –1 Gravitational waveforms from stellar–core collapse Caltech (10kpc from the earth) –1.5 0 1020304050 Time [msec] GR-17 20-July-04 Towards Detection of Gravitational Waves From Bars Bars with Increased Bandwidth Spheres From Interferometers Advanced Interferometers Next Generation (QND) Detectors From 6 Mpc (NN inspiral) 200 Mpc and then beyond From Upper Limits Searches Detections From Generic Searches Searches using Specified Waveforms From Single Detectors Global Networks 20-July-04 GR-17 - Barish 2 Resonant Bar MiniGrail Auriga, Italy The Netherlands Detectors Allegro USA Schenberg Brazil Nautilus, italy Explorer Switzerland Niobe 20-July-04 GR-17 - Barish Australia 3 Network of Resonant Bars Allegro Explorer Auriga Nautilus Niobe IGEC Network 20-July-04 GR-17 - Barish 4 International Gravitational Event Collaboration (IGEC) ALLEGRO,AURIGA,EXPLORER, NAUTILUS, and NIOBE 1997-2000. The search for burst waves at resonant frequency ~ 900 Hz. The detectors nearly parallel to maximize coincident sensitivity. Candidate events at SNR > 3-5 (~ background events 100/day) Data exchanged: peak amplitude, time of event and uncertainties. Threshold equivalent to ~0.1 M⊙ converted into a gravitational wave millisecond burst at a distance of 10 kpc. The accidental coincidence rate over 1 sec interval (e.g. bandwidth of 1 Hz) was ~ few/week two-fold and ~few/century three-fold. Time resolution not sufficient to resolve incident wave direction, no directional search has been applied. No evidence for grav wave bursts was found.
    [Show full text]
  • Study of Optomechanical Parametric Instabilities in the Advanced Virgo Detector David Cohen
    Study of optomechanical parametric instabilities in the Advanced Virgo detector David Cohen To cite this version: David Cohen. Study of optomechanical parametric instabilities in the Advanced Virgo detector. As- trophysics [astro-ph]. Université Paris-Saclay, 2021. English. NNT : 2021UPASP031. tel-03259687 HAL Id: tel-03259687 https://tel.archives-ouvertes.fr/tel-03259687 Submitted on 14 Jun 2021 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Study of optomechanical parametric instabilities in the Advanced Virgo detector Étude des instabilités paramétriques optomécaniques pour le détecteur Advanced Virgo Thèse de doctorat de l'université Paris-Saclay École doctorale n° 576, Particules, Hadrons, Énergie, Noyau, Instrumentation, Imagerie, Cosmos et Simulation (PHENIICS) Spécialité de doctorat: Astroparticules et Cosmologie Unité de recherche : Université Paris-Saclay, CNRS, IJCLab, 91405, Orsay, France Référent : Thèse présentée et soutenue à Paris-Saclay, le 29/03/2021, par David COHEN Composition du Jury t Sophie HENROT-VERSILLÉ Présidente Directrice
    [Show full text]
  • Redalyc.GRAVITATIONAL WAVE DETECTION: WHAT IS
    Revista Mexicana de Astronomía y Astrofísica ISSN: 0185-1101 [email protected] Instituto de Astronomía México Aguiar, O. D.; Graviton Collaboration GRAVITATIONAL WAVE DETECTION: WHAT IS NEW Revista Mexicana de Astronomía y Astrofísica, vol. 40, 2011, pp. 299-304 Instituto de Astronomía Distrito Federal, México Available in: http://www.redalyc.org/articulo.oa?id=57121297168 How to cite Complete issue Scientific Information System More information about this article Network of Scientific Journals from Latin America, the Caribbean, Spain and Portugal Journal's homepage in redalyc.org Non-profit academic project, developed under the open access initiative RevMexAA (Serie de Conferencias), 40, 299–304 (2011) GRAVITATIONAL WAVE DETECTION: WHAT IS NEW O. D. Aguiar1 for the Graviton Collaboration RESUMEN La b´usqueda de la detecci´on de ondas gravitacionales ha sido uno de los desaf´ıos tecnol´ogicos m´as dif´ıciles a los que se han enfrentado jam´as los f´ısicos experimentales y los ingenieros. A pesar de los resultados nulos obtenidos hasta la fecha despu´esde cuatro a˜nos de b´usqueda, la comunidad involucrada en ´esta ´area ha ido creciendo. Una de las principales razones de esto es que la primera detecci´on de ondas gravitacionales y la observaci´on regular de ellas son de las metas m´as importantes para el comienzo de este milenio. Ellas probar´an uno de los fundamentos de la f´ısica, la teor´ıa de la relatividad general de Einstein y abrir´auna nueva ventana para la observaci´on del universo, lo cual, seguramente causar´auna revoluci´on en nuestra comprensi´on de la f´ısica y la astrof´ısica.
    [Show full text]
  • I (I)" B -;; 2: Change the Opening Statement of This Section
    Detectors _ 217 216 _ Astrophysical Techniques Exerc ise 1.14 natural deposits. This is a fu nction of the half-life of the product and the neutrino fllLx in th e recent past, assuming that a state of eqUlltbnum has If Davis' ch lo rille-37 neutrino detector were allowed to reach equilibrium, bee n reached. Poss ibl e candidate elements are tabulated below. what would be the total number of atoms to be expected? (Hint: see Exercise 1.1 2, and note th at 2:: : 1 G)"= 0.693). Product Energy Threshold Half· life (Years) (MeV) Element React ion 3 x 10 0.046 1.6 GRAVITATIONAL RADIATION Thallium ' 2.6 x 106 8.96 1.6"1 Introduc ti on Molybdenum + /Ie - + II + e- 2. 1 X lOS 0.490 When the first edition of this book was written 25 years ago, this section Bromine + IIf - e- 8 X 10" 2.36 Potassium + /Ie + e- began "This section differs from the prev ious o nes beca use none of the techniques th at are di scussed have yet indisput3bly detected gravitational rad iation." That is still the case. It is possibl e that the upgrades to some of the cu rrent interferometric gravity wave detectors (see Secti on 1.6.2) will Exercise 1.1 2 be se nsitive enough to make the first detections by 2010 to 2012. It has Show that if an element and its rad ioactive reaction product are in an also been stated that a third-generat ion interferometric gravity wave equilibrium state with a steady flux of neutrinos.
    [Show full text]
  • Gravitational Wave Detection - Forefront Or Backwater of Astronomy?
    P a g e | 1 Gravitational Wave Detection - forefront or backwater of astronomy? A dissertation for the UCL evening certificate in astronomy (2nd year) A J Rumsey, May 2009 P a g e | 2 Contents: 1. Introduction and preamble 2.The development of the idea 3. Evidence for the existence of gravitational waves 4.Gravitational wave detectors a.Resonant mass detectors b.Laser interferometers c. Space antenna 5.Detectable sources and events P a g e | 3 6.Conclusions 1. Introduction and preamble The race is on to be the first to detect a gravitational wave. Considerable resources around the globe have been channelled into cutting-edge gravitational wave detection research and associated technological development in the last two decades. Scientists clearly believe that they are on the verge of making some exciting historical discoveries and the prizes will be substantial if they are right. Not only is personal kudos there for the winners, but also the immense scientific satisfaction of substantiating, yet again, the substance of the theories of one of the world’s foremost genii – Albert Einstein. His general theory of relativity, which has towered over all of science through the 20th century and into the 21st conceivably stands or falls depending on the outcome. The very existence of gravitational waves remained theoretical until quite recently, but finding the P a g e | 4 astronomical basis of the indirect evidence for their existence was enough to earn two astronomers a Nobel Prize. Interestingly, it seems as if the Nobel Prize panel were not quite convinced enough of those conclusions and cleverly hedged their bets by awarding the prize for finding a new type of Pulsar - not for proving the existence of gravitational waves and speed of propagation (although those very conclusions were drawn by the recipients).
    [Show full text]