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

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

Jul 07, 2023 222 likes •579 views

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

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Huaike Guo

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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)

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  • Neutron Stars
  • White Dwarfs
  • Black Holes
  • Primordial Black Holes
  • Boson Stars
  • Quark Stars
  • ...

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Ordinary Exotic

  • Neutron Stars
  • White Dwarfs
  • Black Holes

?

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

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  • (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

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

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

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

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SMBH IMBH

105 102 1 10-18

SBH PBH

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ECOs

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SMBH IMBH

105 102 1 10-18

SBH PBH

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ECOs

  • background free from ordinary COs
  • large number density
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Credit: http://archive.ncsa.illinois.edu/Cyberia/Cosmos/RotationsReckon.html

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  • m/M << 1 (e.g.,10/106)

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SMBH

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Extreme Mass Ratio Inspiral (EMRI)

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Moore, Cole and Berry, Class. Quantum Grav. 32 (2015) 015014 MAGIS/AION

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  • Binaries (BH-BH, BH-NS, NS-NS)
  • Stochastic Gravitational Waves(inflation, phase transition)
  • Continuous Waves (spinning neutron stars)
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  • 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.

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detector

rmax

Matched-filtering EMRI Noise

SNR = 20

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

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

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ISCO

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

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5-years observation time

ISCO

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

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5-years observation time

ISCO

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

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Image credit: ESA/C ISCO

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

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Image credit: ESA/C ISCO

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

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

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Huaike.Guo, Jing Shu, Yue Zhao, Phys. Rev. D 99, 023001

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assume one detection in 5 years

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LISA DECIGO Taiji Tianqin

Wikipedia

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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

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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

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  • 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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  • ~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...)