Some of GW sources and physics potentials - Interests in 500 ~ kHz - - PowerPoint PPT Presentation

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Apr 13, 2023 133 likes •285 views

Some of GW sources and physics potentials - Interests in 500 ~ kHz GW- Yousuke Itoh ( ) KAGRA Gravitational Wave Data Analysis International cooperation section Research Center for the Early Universe, Graduate School of Science,

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Some of GW sources and physics potentials

Interests in 500 ~ kHz GW-

3rd KAGRA International Workshop@Academia Sinica, 2017/05/21-22

Yousuke Itoh (伊藤洋介)

KAGRA Gravitational Wave Data Analysis International cooperation section Research Center for the Early Universe, Graduate School of Science, the University of Tokyo [“RESCEU” for short]

SLIDE 2

Interesting topics

Nuclear physics

– EOS & hyperon puzzle: tidal disruption/deformability, mass-radius – site of r-process elements generation: SGRB/SNe?

Astrophysics

– origins & evolution scenario(s) of SMBH [eLISA/PTA] – existence & formation of SMBH binaries (Last 1 parsec problem) [PTA] – existence & formation scenario(s) of IMBHs – verification binaries: “the calibration sources” or test of GR [eLISA] – Massive Black Hole Binary as a smoking gun of Pop III – r-process sites – short GRB: NS/NS or NS/BH? – Supernovae mechanism: neutrino, rotation – Supernovae: what will be left? BH or NS? – pulsar glitch – oscillations of compact stars à compactness, density, … – pulsar precession: Is it possible? (too low frequency … ?)

SLIDE 3

Interesting topics (cont’d)

test of GR

– velocity of GW – polarizations of GW – Kerr-ness: QNM, quadrupole moment

Exotic objects

– exotic compact objects: QNM, tidal deformability – Higher “mountain on” quark stars: (continuous wave) – echo by firewall??? – extra dimensions???

Cosmology

– Inflation (CMB B-mode, direct detection by Ultimate- DECIGO?) – Large scale structure with different method other than EM – gravitational lensing of gravitational wave – Primordial BH – cosmic strings – phase transition

SLIDE 4

O(100-1000) events/yr in the next decade.

Report from the DAWN-II Workshop, Atlanta, GA, July 7-8, 2016

SLIDE 5

Interesting topics at 500-kHz (1)

Nuclear physics: EOS

– site of r-process elements generation: SGRB/SNe?

Astrophysics

– r-process sites – short GRB: NS/NS or NS/BH? – Supernovae mechanism(s): neutrino, rotation,SASI,.. – Supernovae: what will be left? BH or NS? – pulsar glitch – FRB, …

SLIDE 6

Detection prospects & r-elements abundance if NS binary origin

Rosswog et al. (2017) CQG 34 104001

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Localization

LSC-V (2016) PRX 6, 041015

galaxy density: 0.02 L10 /Mpc3 (Kopparapu et. al. ApJ. 2008)

The number of galaxies in an observable volume (horizon distance 200Mpc) in 5 square degrees is O(10000).

sGRB 10-7 events/Mpc3/yr or 3 if NS/NS, 160 events/yr if NS/BH for

aLIGO (D. Yonetoku, et al. ApJ. 789 (2014) 65)

SLIDE 8

100 1 10 1 100 0.1 10 time resolution (s) FOV (sq. deg.)

HSC SDSS

CCD

Pan-STARR Decam

22 20 25 23

iPTF

circle size: limiting magnitude

Follow-up: time resolution & FOV

Tomoe-Gozen

CMOS

17 Assume 0.01Msun.

Mag. (red-opt/IR)

22mag@200Mpc to 24mag (10 days after)

M. Tanaka (2016) Adv.

Astron

SLIDE 9

EOS can be determined by how NS/NS are tidally disrupted?

Takami, Rezzolla & Baiotti, PRL 113, 091104 (2014)

NS/NS: merge at higher frequencies (kHz), HMNS f-mode ~ 2-4 kHz.

SLIDE 10

LV-UL distributions of ε & h0

LSC-V ApJ 839:12 (2017)

Higher the frequency, more stringent the limit

n epsilon is. [But msec PSR are old and

probably more spherical?]

Known PSR search results

n ”mountain heights”

ℎ ∝ 𝜁𝑔&

SLIDE 11

Interesting topics at 500-kHz (2)

test of GR
Deviation(s) in waveform from GR predictions
spin-quadrupole moment relation
Black-Hole spectroscopy
Exotic objects
QNM, tidal deformability, higher stellar mountain

…

SLIDE 12

Tidal deformability and exotic objects

Differences in tidal deformability among

normal objects (NS,BH) and exotic objects (Boson stars, Quark stars …)

Kerr-ness [Spin-Quadrupole relation]

For all those proposals, it is nicer to have a better sensitivity in higher frequency.

Quadrupole moment appears at 5 PN order in PN expansions

SLIDE 13

Test of GR

LSC-VC PHYSICAL REVIEW X 6, 041015 (2016)

N. Yunes, K. Yagi, & F. Pretorius

PHYSICAL REVIEW D 94, 084002 (2016)

Strong gravity -> Higher PN order -> Better to have a better sensitivity in higher frequency?

SLIDE 14

BH Spectroscopy

Berti, Cardoso, & Will, PHYSICAL REVIEW D 73, 064030 (2006)

Frequency of l=m=3 mode is higher than l=m=2 mode by ~ 1.5 times. If l=m=3 mode amplitude is 0(10%) of l=m=2 mode, need [Q330Sn(f220)/(Q220Sn(f330))]1/2 ~ 8. Too much à Better expect stacking or gold event

SLIDE 15

Summary today

First detection made by LIGO, more to come

– Expect High ER: ~ 1 event/day in 202x (O5)

Higher frequency is (also) interesting, e.g.,