Detecting Strangeon Nuggets with Acoustic Messenger Reporter

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Explore the groundbreaking research on detecting Strangeon Nuggets through acoustic methods, shedding light on their unique properties and potential implications in dark matter studies. This study delves into the motivations, introduction to Strangeon Nuggets, acoustic detection techniques, and intrinsic characteristics, providing insights into this fascinating area of astrophysics.

  • Strangeon Nuggets
  • Acoustic Detection
  • Dark Matter
  • Astrophysics
  • Research
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  1. Detecting Strangeon Nuggets with Acoustic Messenger Reporter: Haoyang Qi Mentor: Renxin Xu 2024 07 15 FPS13

  2. Contents Motivations Introduction to Strangeon Nuggets (StN) Acoustic detection of StN pass-through event in normal matter Discussions and conclusions 2

  3. Motivations 3

  4. Developing of idea Neutron star (Landau 1932) Quark star (Witten 1984 as a representative) Strangeon star (Xu 2003) 4

  5. Motivations of this work Implication in: dark matter, for its low hadronic charge-mass ratio pulsar, as a probable equation of state and acoustic detection, as a new messenger 5

  6. Introduction to Strangeon Nuggets (StN) 6

  7. Strangeonization ?F= 2? ?1/3(3/4?)1/3 480 MeV/? for ? = 0.25 fm 3 Strange quark ?0 95 MeV/?2, perturbation QCD energy scale ? 1 GeV Three-flavor symmetry Xu, R., Lai, X., & Xia, C. (2021). Astron. Nachr., 342(1-2), 320-325. Yuan, W. In prep. 7

  8. Intrinsic characteristics ?StN~ 4.2 1014g/cm3(for ? = 0.25 fm 3at ? = 0) Baryon number ?~1030(Critical baryon number ?? 109) Mass ?StN~ 1.7 106g 1/3 = 1.6 10 3cm 1/3 1/3 3?StN 4??StN ? ?StN Radius ?0= 1030 1014g/cm3 Hadronic charge-mass ratio ??=?? ?= 10 7~10 4 Farhi, E., & Jaffe, R. L. (1984). PRD, 30(11), 2379-2390. 8

  9. Other characteristics ? = 220 km/s or 0.1? (for dark matter or merger remnant) Number density ? = 3.2 10 31cm 3(Single component, ?DM= 0.3 GeV/cm3) 1 ? ? Event rate: ?? = 7.04 10 24s 1cm 2 1030 220 km/s 2= 1.28 1018cm2, event rate is ~280 / yr) (Consider ?? 9

  10. Magnetic field of StN Wave function of identical particles without spin-orbit coupling 1,2?1,?2,?1,?2 = ?1,2?1,?2?1(?1)?2(?2) S=1 ?1?2is exchange symmetric ?1,2?1,?2 is exchange anti-symmetric when?1= ?2, ?1,2= 0 ?emget lower Transfer from one spin direction to another kinetic energy of electron ?kget higher 10

  11. Spontaneous magnetization of electron spin magnetic moment 1 3 2? ?2 ?em=1 3 ?? 2 ? ? (???)2+??2 2 ? ? 4??0??,??= ??, ?k= 2 4? ? ?em= ?k(Multi-body interaction and ? 1potential: ? > 1) 1 3 ?em 8? 0.064??em ? ??= ? ?? 10 MeV/? for ??=10 5 ? ?? 480 MeV/? 4? 3 ?? ?? ? After spin reverse, blue means only one spin is filled Fermi ball of electrons, gray means two spins are filled 11

  12. Magnetic field of StN ?? ?????=4??? 2 ? ????= 0.38??em ??? ?? 4? 3?? 3 ?? ????? 4? 3?0 ?? ?StN = 2.0 1011G ? ?0= ??0 10 5 1014g/cm3 3 Take ?0= 1012G as (Surface dipole magnetic field of the StN, strangeon star may have extra magnetic field from collective movement of electrons) 12

  13. Acoustic detection of StN pass-through event in normal matter 13

  14. Incident and ionize 1/3 1/3, normal matter can ? ?StN ?0= 1.6 10 3cm be considered as continuous medium 1030 1014g/cm3 ?2 2??(For SiO2, ??= 7 106erg/(g K)) Aerodynamic heating ? = 1 2 ?? ? ? = 7 107K , enough to ionize 7 106erg/(g K)) 220 km/s (OVIII OIX ? = 871.4 eV = 1.011 107K) Ionization zone may be small (discuss later) 14

  15. Magnetopause of StN 1 6 ?03 ?m 6 2?0 ????2=2?2 2?0 ?0????2 1 6 ?0, ? = ?0 3,? = 1 ?m= 1 3 1 ? ?0 ?med 1 g/cm3 ?StN ? 3 ?m= 0.316 cm 1030 1 3 1014g/cm3 1 3 1012G 220 km/s 1 ?m ?0= 196 ?0 ?med 1 g/cm3 ? 6 1012G 220 km/s ?0 ?? VanDevender, J. P., VanDevender, A. P., Sloan, T., et al. (2017). Sci. Rep., 7(1), 8758. 15

  16. Cross section and penetration depth 2 3 1 2 ? ?0 ?med 1 g/cm3 ?StN ? 3 3 ?m= ??m2= 0.320 cm2 1030 1014g/cm3 1012G 220 km/s 2 3 1 2 ?m ?StN= 1.92 10 7cm2/g ?m= ?m????2= d?k ?0 ? ?med 1 g/cm3 ?StN ? 3 3 1030 1014g/cm3 1012G 220 km/s d?,? = 1 2 ?k=1 ? ? 2?StN?2= 4.1 1020erg 1030 220 km/s 2 3 1 3 2 2 3 2 3 ? ?StN ?0 ?med 1 g/cm3 3 (?0 220 ? = 7.88 106cm 1012G ?? 220 ) 1030 1014g/cm3 16

  17. Penetration depth Passing through earth atmosphere: ? 1020 17

  18. Penetration depth 18

  19. Characteristics of acoustic signal Sound pressure and energy: ?2 ?med?? 2??d? ?shock= d?sound 1 4= 0.336 ms 5 4 1014g/cm3 ?? ?shock= 1.822?m ?? ?? ????m 1 1 1 4 1 ?StN ?med 1 g/cm3 ? ? ?0 ?? ? 4 8 4 1030 1012G 1 km 1 km/s Mach shockwave 100 ? ?shock StN trajectory ? ?? Maher, R. (2006). 2006 IEEE 12th D. S. P. Workshop & 4th IEEE S. P. E. Workshop, 257 261. 19

  20. Characteristics of acoustic signal Attenuation: geometric, scattering, and absorption (exponential decay for the last item) Absorption: viscosity, thermal conduction, and relaxation 2?med??3 [4? In pure crystal medium and pure water: 1 ?2 ?? 1 1 ?? d?sound= d?sound 0? ??, ? = + ? 3+ ? ?? 2] 1+?2?? ?> ? (? 103Hz) Sea water or real rock: not pure and uniform medium 20

  21. Characteristics of acoustic signal Take ? 1 ms, ??= 1.5 km/s Experiments in real water: ? 9.01 103cm, d?sound= ?d??? ?noise 1 erg/cm3,? = 1.1 10 6 Critical detectable distance: 2?? ?med?? ? 9.01 103cm= 2 ??m? ?noise ? VanDevender, J. P., VanDevender, A. P., Sloan, T., et al. (2017). Sci. Rep., 7(1), 8758. 21

  22. Acoustic critical detectable distance ? 0.0901 km) =????med?? ? = 3.66 1010km ? exp( 10 6 2???2 ? 2 3 4 3 5 3 1012G 1014g/cm3 2 ? ?0 ? ?med 1 g/cm3 ?? 1030 1 erg/cm3 ?? 1.5 km/s ?StN 1 ms ? 220 km/s Attention there are another characteristic length: 0.0901 km rather than 3.66 1010km 22

  23. Acoustic critical detectable distance 23

  24. Discussions and conclusions 24

  25. Cosmic dusts If there is atmosphere: burnt 2 ?k=1 ? ? 2?dust?2= 4.1 1020erg ?dust= ??0 1030 220 km/s 2????2,? = 1 (ram pressure) 2 3 ( 2 3 g/cm3) 2 ? ?dust ? ?med 1 g/cm3 ?dust= 3.9 1018dyn 3 1030 220 km/s 1 3 2 3 1 ?k ? ?dust 3 g/cm3 ?med 1 g/cm3 ?dust= ?dust= 106 cm 1030 25

  26. Energy losing efficiency and accumulation in celestial bodies Ionize energy loss (~0.01 time of influence of plasma ram pressure) 1 2 1 2 ?0 1 2 ? 1 ? ?med 1 cm3 ?atom 20?u ?D= 1.26 10 7cm 2 g 107K 1 3 ?Landau ?0 ?0 = 9.48 1012G 1 3? 1 1 2 ??_atom ?=? ?0 ?0 ?atom ?Bohr = 7.52 6 1012G 1 3? 1 2 3 ??_StN ?=? ?0 ?0 ?atom ?Bohr = 3.50 3 1012G 26

  27. Conclusions Strangeon nugget have a strong dipole magnetic field ~1012G because of spontaneous magnetization of electron spin magnetic moment. Stangeon nugget impact event may can be detected by microphone array in several km distance to the trajectory and can be distinguished from cosmic dust impact event. The radius of magnetosphere of StN passing through medium may be smaller, make StN harder to detect and will not to be trap by celestial bodies in every event. Thanks! 27

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