Huaike Guo

1

University of Oklahoma

August 8, 2019

Searching for new physics - Leaving no stone unturned!

Huaike Guo, Jing Shu, Yue Zhao, Phys. Rev. D 99, 023001Huaike Guo, Kuver Sinha, Chen Sun, arXiv:1904.07871(JCAP)

• Neutron Stars

• White Dwarfs

• Black Holes

• Primordial Black Holes

• Boson Stars

• Quark Stars

• ...

2

Ordinary Exotic

• Neutron Stars

• White Dwarfs

• Black Holes

?

Carr, et al PRD,94,083504

see talks ofStefano ProfumoSam McDermott

• (Mini)Boson Star(self-interactions or not)

• Solitonic Boson Star(specific potential)

• Oscillaton(real scalar field)

• Proca Star(massive vector)

• Axion Stars(dense or dilute) ECO

Particle Physics

Huaike Guo, Kuver Sinha, Chen Sun, arXiv:1904.07871

Huaike Guo, Kuver Sinha, Chen Sun, Joshua Swaim, Daniel Vagie, in preparation

Braaten, Mohapatra and Zhang, PRL 117,121801

Dense Axion Stars

Not so dense? See Visinelli, Baum, Redondo, Freese, Wilczek, PLB 777(2018),64

109

SMBHIMBH105102110-18

SBH

PBH

8ECOs

109

SMBHIMBH105102110-18

SBH

PBH

9ECOs

• background free from ordinary COs

• large number density

Credit: http://archive.ncsa.illinois.edu/Cyberia/Cosmos/RotationsReckon.html

10

•m/M << 1 (e.g.,10/106)11

SMBH

Extreme Mass Ratio Inspiral (EMRI)

12Moore, Cole and Berry, Class. Quantum Grav. 32 (2015) 015014

MAGIS/AION

• Binaries (BH-BH, BH-NS, NS-NS)

•Stochastic Gravitational Waves(inflation, phase transition)

•Continuous Waves (spinning neutron stars)

• Signal is long-lasting, large SNR even for sub-solar mass ECO

• Parameters can be determined very precisely. (e.g.,10-5)

•For much sub-solar mass PBH, once detected, we know it is not Stellar BH.

14

detectorrmax

Matched-filtering

EMRI

Noise

SNR = 20

15

Huaike Guo, Kuver Sinha, Chen Sun, arXiv:1904.0787116

Huaike Guo, Kuver Sinha, Chen Sun, arXiv:1904.0787117

ISCO

Huaike Guo, Kuver Sinha, Chen Sun, arXiv:1904.0787118

5-years observation time

ISCO

Huaike Guo, Kuver Sinha, Chen Sun, arXiv:1904.0787119

5-years observation time

ISCO

Huaike Guo, Kuver Sinha, Chen Sun, arXiv:1904.0787120

Image credit: ESA/C

ISCO

Huaike Guo, Kuver Sinha, Chen Sun, arXiv:1904.0787121

Image credit: ESA/C

ISCO

Huaike Guo, Kuver Sinha, Chen Sun, arXiv:1904.0787122

Huaike Guo, Kuver Sinha, Chen Sun, arXiv:1904.0787123

Huaike.Guo, Jing Shu, Yue Zhao, Phys. Rev. D 99, 02300124

assume one detection in 5 years

25

26

LISA

DECIGO

TaijiTianqin

Wikipedia

Huaike.Guo, Kuver Sinha, Chen Sun, in preparation

assume a mass ratio of 10^5

Huaike.Guo, Kuver Sinha, Chen Sun, in preparation

assume a mass ratio of 10^5

Huaike.Guo, Kuver Sinha, Chen Sun, in preparation

assume a mass ratio of 10^5

Huaike.Guo, Kuver Sinha, Chen Sun, in preparation

200 hours

• Nearest NS: ~76 - 306 pc

• Nearest WD: ~3pc

• Nearest SBH: ~1kpc

•Luminous ECO?

•Collision with other stars

•Tidal Disruption Events(more promising)

Image credit: ESA/C 31

32

• EMRI is a powerful way of probing ECOs

• Future space-based GW detectors might discover sub-solar mass ECOs.

• Some mini-EMRI might hide in LIGO data.

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34

• ~pc region around the SMBH (radius of influence)

• DM Halo profile (cuspy, cored or spiky)

• Stellar dynamics near the SMBH(2-body relaxation, resonant relaxation, mass segregation...)