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.
33
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...)