1 Kazuhiro Yamamoto Institute for Cosmic Ray Research (ICRR) the University of Tokyo KAGRA face to face meeting University of Toyama, Toyama, Japan 3 August 2013 Effect of MOMENTUM deposited by EXOTIC particles on interferometeric gravitational wave detectors

2 0. Abstract Gravitational wave detectors can detect everything. Can they detect exotic particles ? Exotic particle : It is not found in experiment although theorist predicts.

3 Contents 1.Introduction 2.Momentum deposition 3.KAGRA 4.Improvement 5.Exotic particle search 6.Summary

44 1. Introduction 444 Gravitational wave detector (interferometer and resonator) : Ultra high sensitive sensor Many noise sources : Quantum noise, Thermal noise, Seismic motion, Noise from laser source, Circuit noise, Electric and Magnetic fields,.... Cosmic rays ? Resonator First paper : B.L. Baron and R. Hofstadter (Nobel prize 1961), Physical Review Letters 23 (1969) 184. Interferometer First paper : A. Giazotto, Phys. Lett. A 128 (1988) 241.

55 1. Introduction Not noise, but signal !Exotic particle search Exotic particle search using resonator G. Liu and B. Barish, Physical Review Letters 61 (1988) 271. P. Astone et al., Physical Review D 47 (1993) How about interferometer ? (calculation) K. Yamamoto et al., Physical Review D 78 (2008) Interferometer is inferior to resonator as particle detector. (a)Signal to Noise ratio (S/N) is smaller than that of resonator. (b)Cross section is also smaller.

1. Introduction 6 Nevertheless, interferometer as exotic particle detector is considered. Q. How do cosmic ray (or exotic) particles generate noise (or signal) in gravitational wave detector ? A. Energy deposition of particles makes elastic vibration of resonator or mirror of interferometer.

Process of cosmic-ray excitation (Energy deposition) (i) Passage of cosmic ray particle in mirror or resonator (ii) Energy deposition (iii) Temperature gradient (iv) Thermal stress (v) Elastic vibration of mirror or resonator Mirror or resonator Cosmic ray particle

Process of cosmic-ray excitation (Energy deposition) (i) Passage of cosmic ray particle in mirror or resonator (ii) Energy deposition (iii) Temperature gradient (iv) Thermal stress (v) Elastic vibration of mirror or resonator Mirror or resonator

Process of cosmic-ray excitation (Energy deposition) (i) Passage of cosmic ray particle in mirror or resonator (ii) Energy deposition (iii) Temperature gradient (iv) Thermal stress (v) Elastic vibration of mirror or resonator Hot Mirror or resonator

Process of cosmic-ray excitation (Energy deposition) (i) Passage of cosmic ray particle in mirror or resonator (ii) Energy deposition (iii) Temperature gradient (iv) Thermal stress (v) Elastic vibration of mirror or resonator Mirror or resonator

Process of cosmic-ray excitation (Energy deposition) (i) Passage of cosmic ray particle in mirror or resonator (ii) Energy deposition (iii) Temperature gradient (iv) Thermal stress (v) Elastic vibration of mirror or resonator Mirror or resonator

12 If we take only energy deposition into account, interferometer is inferior as particle detector. K. Yamamoto et al., Physical Review D 78 (2008) According to A. Giazotto, Phys. Lett. A 128 (1988) 241, energy deposition implies momentum deposition. When particles give a suspended mirror in interferometer momentum, pendulum motion can be excited. Nobody considered the effect of momentum deposition by exotic particle on interferoemter. 1. Introduction

13 2. Momentum deposition In the case of cosmic ray... pendulum motion excited by momentum deposition is smaller than the elasctic motion of mirror by energy deposition. Energy deposition Thermal stress : Decay time is about 1000 sec. Step response Momentum deposition Momentum transfer in a moment Impulse response

14 2. Momentum deposition Speed of cosmic ray particles is almost same as that of light ! If exotic particles moves more slowly ? Momentum deposition (speed is the same as that of light (c)) Energy deposition Momentum deposition (slower, speed is v)

15 2. Momentum deposition If speed of exotic particle is the same as that of light... momentum (p) is proportional to energy (E). If exotic particles run slowly... energy is almost constant (mc 2 ) even if momentum changes drastically. Thus, dp/dE is larger when v is smaller than c.

16 2. Momentum deposition How much is c/v typically ? If exotic particles are trapped in gravitational potential of Earth, averaged speed is about 10 km/sec (Virial theorem). Thus, c/v is about 3*10 4. Note : dE/dl (enery deposition per unit length) depends on energy. l is the length of particle track in a mirror.

KAGRA (or 2 nd generation) interferometer as exotic particle detector We must find the pendulum motion by exotic particles. Matched filter is useful. Signal to Noise ratio (S/N) is as follows. This is similar to S/N of resonators KAGRA

18 Improvement of interferometer as exotic particle detector 18 Displacement (not strain) noise must be small. Long baseline is not necessary. Lighter mirror is better. Since we must observe excited pendulum motion, noise below 100 Hz must be smaller. (a) Seismic noise must be small. (b) Pendulum will be cooled to reduce thermal noise. (c) Light power will be small to reduce radiation pressure noise. 4. Improvement

19 Improvement of interferometer as exotic particle detector 19 How about CLIO ? Signal to Noise ratio (S/N) of CLIO is only half of that of KAGRA ! Note : Limit sensitivity at cryogenic temperature is assumed. 4. Improvement

20 Improvement of interferometer as exotic particle detector 20 For example... Mirror : 100 times smaller than KAGRA mirror Size is on the order of 1 mm (mass is 30 mg). Baseline : table top Laser power : 0.25 W No Fabry-Perot cavity (shot noise : m/rtHz) Tempearture of mirror : 20 K Excellent seimic vibration system : smaller than m/rtHz above 10 Hz Signal to Noise ratio is 10 times larger than that of KAGRA and resonators. 4. Improvement

21 Mass of target particle 5. Exotic particle search If particle is too light, it must stop in a mirror. Lower limit of mass of target particle KAGRA : 4.5 *10 9 GeV Table top interfetomer : 1.8*10 6 GeV Proton : 1 GeV, Top quark : 170 GeV, Higgs (like) particle : 125 GeV

22 5. Exotic particle search Lower limit of mass of target particle KAGRA : 4.5 *10 9 GeV Table top interfetomer : 1.8*10 6 GeV What kinds of exotic particles are targeted ? Magnetic monopole C. Bernard et al., Nuclear Physics B 242(1984)93. Nuclearite E. Witten, Physical Review D 30(1984)272. A. De Ru´jula and S. L. Glashow, Nature 312(1984)734. Mirror dust particle R. Foot and S. Mitra, Physical Review D 68(2003)071901(R).

23 5. Exotic particle search How often can we observe ? Lower limit of mass of target particle KAGRA : >4.5 *10 9 GeV Table top interfetomer : >1.8*10 6 GeV Average (or critical) density of Universe 5*10 3 eV/cm 3 If Universe is dominated by exotic particle, we can observe an exotic particle every two months (KAGRA) or every eight months (Table top interferometer) in the best case.

24 6. Summary Momentum deposition of exotic particle can excite mirror pendulum motion. When this particle moves more slowly than light, the exctitation could be large. Signal to Noise ratio of KAGRA as exotic particle detector is comparable with that of resonators. Signal to Noise ration of Table top interferometer with tens mg mirrors is 10 times larger than that of KAGRA.

25 6. Summary Only extremely heavy particles (larger than 10 6 GeV) can be target. We observe an exotic particle every a few or several months in the best case if Universe is dominated by these exotic particles.

26 If you are interested with this topic, here are details in Japanese ! bin/private/DocDB/ShowDocument? docid=1112 It is written in

27 Thank you for your attention !

Improvement of interferometer as exotic particle detector 4. Improvement