Huaike Guo University of Oklahoma August 8, 2019 Searching for new - PowerPoint PPT Presentation

Huaike Guo University of Oklahoma August 8, 2019 Searching for new physics - Leaving no stone unturned! Huaike Guo, Jing Shu, Yue Zhao, Phys. Rev. D 99, 023001 Huaike Guo, Kuver Sinha, Chen Sun, arXiv:1904.07871(JCAP) 1

Ordinary Exotic • Neutron Stars • Neutron Stars • White Dwarfs • White Dwarfs • Black Holes • Black Holes • Primordial Black Holes • Boson Stars • Quark Stars ? • ... 2

see talks of Stefano Profumo Sam McDermott Carr, et al PRD,94,083504

• (Mini)Boson Star(self-interactions or not) Particle Physics • Solitonic Boson Star(specific potential) • Oscillaton(real scalar field) • Proca Star(massive vector) • Axion Stars(dense or dilute) ECO

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

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

Dense Axion Stars Braaten, Mohapatra and Zhang, PRL 117,121801 Not so dense? See Visinelli, Baum, Redondo, Freese, Wilczek, PLB 777(2018),64

10 2 10 -18 1 10 5 10 9 SBH SMBH IMBH PBH ECOs 8

• background free from ordinary COs • large number density 10 2 10 -18 1 10 5 10 9 SBH SMBH IMBH PBH ECOs 9

Credit: http://archive.ncsa.illinois.edu/Cyberia/Cosmos/RotationsReckon.html 10

SMBH • m/M << 1 (e.g.,10/10 6 ) 11

Extreme Mass Ratio Inspiral (EMRI) MAGIS/AION 12 Moore, Cole and Berry, Class. Quantum Grav. 32 (2015) 015014

• 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

EMRI r max detector SNR = 20 Matched-filtering Noise 15

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

ISCO 17 Huaike Guo, Kuver Sinha, Chen Sun, arXiv:1904.07871

5-years observation time ISCO 18 Huaike Guo, Kuver Sinha, Chen Sun, arXiv:1904.07871

5-years observation time ISCO 19 Huaike Guo, Kuver Sinha, Chen Sun, arXiv:1904.07871

ISCO Image credit: ESA/C 20 Huaike Guo, Kuver Sinha, Chen Sun, arXiv:1904.07871

ISCO Image credit: ESA/C 21 Huaike Guo, Kuver Sinha, Chen Sun, arXiv:1904.07871

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

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

assume one detection in 5 years 24 Huaike.Guo, Jing Shu, Yue Zhao, Phys. Rev. D 99, 023001

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DECIGO LISA Tianqin Taiji Wikipedia 26

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

• Luminous ECO? • Collision with other stars • Tidal Disruption Events(more promising) Image credit: ESA/C 31

• 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. 32

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• ~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...) 34