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Huaike Guo 1 University of Oklahoma Oct. 12, 2019 Huaike Guo, Jing Shu, Yue Zhao, Phys. Rev. D 99, 023001 Huaike Guo, Kuver Sinha, Chen Sun, JCAP 1909,032 (2019)
Huaike Guo
1
University of Oklahoma
Oct. 12, 2019
Huaike Guo, Jing Shu, Yue Zhao, Phys. Rev. D 99, 023001Huaike Guo, Kuver Sinha, Chen Sun, JCAP 1909,032 (2019)
• 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
3
• (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
4
Huaike Guo, Kuver Sinha, Chen Sun, arXiv:1904.078715
Huaike Guo, Kuver Sinha, Chen Sun, Joshua Swaim, Daniel Vagie, in preparation6
109
SMBHIMBH105102110-18
SBH
PBH
7ECOs
109
SMBHIMBH105102110-18
SBH
PBH
8ECOs
• background free from ordinary COs
• large number density
http://archive.ncsa.illinois.edu/Cyberia/Cosmos/RotationsReckon.html
9
•m/M << 1 (e.g.,10/106)10
SMBH
Extreme Mass Ratio Inspiral (EMRI)
11Moore, Cole and Berry, Class. Quantum Grav. 32 (2015) 015014
• 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.
12
detectorrmax
Matched-filtering
EMRI
Noise
SNR = 20
13
Huaike Guo, Kuver Sinha, Chen Sun, JCAP 1909,032 (2019)14
15
ISCO
Huaike Guo, Kuver Sinha, Chen Sun, JCAP 1909,032 (2019)
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5-years observation time
ISCO
Huaike Guo, Kuver Sinha, Chen Sun, JCAP 1909,032 (2019)
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5-years observation time
ISCO
Huaike Guo, Kuver Sinha, Chen Sun, JCAP 1909,032 (2019)
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Image credit: ESA/C
ISCO
Huaike Guo, Kuver Sinha, Chen Sun, JCAP 1909,032 (2019)
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Image credit: ESA/C
ISCO
Huaike Guo, Kuver Sinha, Chen Sun, JCAP 1909,032 (2019)
20Huaike Guo, Kuver Sinha, Chen Sun, JCAP 1909,032 (2019)
Huaike.Guo, Kuver Sinha, Chen Sun, in preparation
assume a mass ratio of 10^5
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Huaike.Guo, Kuver Sinha, Chen Sun, in preparation
assume a mass ratio of 10^5
22
Huaike.Guo, Kuver Sinha, Chen Sun, in preparation
assume a mass ratio of 10^5
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Huaike.Guo, Kuver Sinha, Chen Sun, in preparation
200 hours
• Nearest NS: ~76 - 306 pc
• Nearest WD: ~3pc
• Nearest SBH: ~1kpc
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•Luminous ECO?
•Collision with other stars
•Tidal Disruption Events(more promising)
Image credit: ESA/C 25
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• EMRI is a powerful way of probing ECOs
• Future space-based GW detectors might discover sub-solar mass ECOs.
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