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Strange star

A strange star, also called a strange quark star,[1]: 352  is a hypothetical compact astronomical object, a quark star made of strange quark matter.[2][3][4]

Strange stars might exist without regard to the Bodmer–Witten assumption of stability at near-zero temperatures and pressures, as strange quark matter might form and remain stable at the core of neutron stars, in the same way as ordinary quark matter could.[5] Such strange stars will naturally have a crust layer of neutron matter. The depth of the crust layer will depend on the physical conditions and circumstances of the entire star and on the properties of strange quark matter in general.[6] Stars partially made up of quark matter (including strange quark matter) are also referred to as hybrid stars.[7][8][9][10]

The collapse of the crust layer of strange stars is one of the proposed causes of fast radio bursts.[7][8][9][10]

Theoretical description

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Neutron stars are formed when the collapse of a star occurs with such intense force that gravity forces subatomic particles such as protons and electrons to merge into neutrally charged neutron particles, releasing a shower of neutrinos. If the resultant neutral core is able to maintain form and not collapse into a black hole, the result is an incredibly dense celestial body composed entirely of neutral uncharged particles.

Protons and neutrons are composed of three quarks: a proton by two up quarks and one down quark, a neutron by two down quarks and one up quark. It is hypothesized that within neutron stars, the conditions are so extreme that a process known as deconfinement occurs: where subatomic particles dissolve and leave their constituent quarks behind as free particles. The temperature and pressure would then force these quarks to be squeezed together to such an extent that they would form a hypothetical phase of matter known as quark matter. If this occurs, the neutron star becomes a "quark star". If the pressure is great enough, the quarks could be affected even further and transform into strange quarks, which would then interact with the other "non-strange" quarks to form strange matter. If this occurs, the quark star would then become a strange star.

Characteristics

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Early work on strange quark matter suggested that it would be a homogeneous liquid, but other models propose[11] a heterogeneous alternative with positively charged "strange quark nuggets" embedded in a negatively charged electron gas.[1] This structure decreases the stars' external electric field and density variation from previous theoretical expectations, with the result that such stars appear nearly indistinguishable from ordinary neutron stars.

Other theoretical work contends that:

A sharp interface between quark matter and the vacuum would have very different properties from the surface of a neutron star.[12]

Addressing key parameters like surface tension and electrical forces that were neglected in the original study, the results show that as long as the surface tension is below a low critical value, the large strangelets are indeed unstable to fragmentation and strange stars naturally come with complex strangelet crusts, analogous to those of neutron stars.[12]

Crust collapse

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For a strange star's crust to collapse, it must accrete matter from its environment in some form.

The release of even small amounts of its matter causes a cascading effect on the star's crust.[13] This is thought to result in a massive release of magnetic energy as well as electron and positron pairs in the initial phases of the collapsing stage. This release of high energy particles and magnetic energy in such a short period of time causes the newly released electron/positron pairs to be directed towards the poles of the strange star due to the increased magnetic energy created by the initial secretion of the strange star's matter. Once these electron/positron pairs are directed to the star's poles, they are then ejected at relativistic velocities, which is proposed to be one of the causes of fast radio bursts.

Primordial strange stars

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Theoretical investigations have revealed that quark stars might not only be produced from neutron stars and powerful supernovae, they could also be created in the early cosmic phase separations following the Big Bang.[14]

If these primordial quark stars can transform into strange quark matter before the external temperature and pressure conditions of the early universe renders them unstable, they might become stable, if the Bodmer–Witten assumption holds true. Such primordial strange stars could survive to this day.[14]

Observability

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Strange dwarfs, unlike neutron stars with strange cores, are postulated to be different from white dwarfs. A database of white dwarfs has been analyzed. Knowledge of the mass and surface gravity of a star allows calculation of its radius. A team that compared 40,000 white dwarfs to the mass–radius relation for white dwarfs discovered that most of them followed that relation. Eight exceptions were much smaller in size and matched predictions for a strange dwarf.[15]

See also

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References

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  1. ^ a b Page, Dany; Reddy, Sanjay (2006-11-01). "Dense Matter in Compact Stars: Theoretical Developments and Observational Constraints". Annual Review of Nuclear and Particle Science. 56 (1): 327–374. arXiv:astro-ph/0608360. doi:10.1146/annurev.nucl.56.080805.140600. ISSN 0163-8998.
  2. ^ Alcock, Charles; Farhi, Edward; Olinto, Angela (1986). "Strange stars". Astrophys. J. 310: 261–272. Bibcode:1986ApJ...310..261A. doi:10.1086/164679. Archived from the original on 2019-04-02. Retrieved 2018-11-16.
  3. ^ P., Haensel; R., Schaeffer; J.L., Zdunik (1986). "Strange quark stars". Astronomy and Astrophysics. 160. Archived from the original on 2022-03-22. Retrieved 2018-11-16.
  4. ^ Weber, Fridolin; et al. (1994). Strange-matter Stars. Proceedings: Strangeness and Quark Matter. World Scientific. Bibcode:1994sqm..symp....1W.
  5. ^ Stuart L. Shapiro; Saul A. Teukolsky (20 November 2008). Black Holes, White Dwarfs, and Neutron Stars: The Physics of Compact Objects. John Wiley & Sons. pp. 2ff. ISBN 978-3-527-61767-8. Archived from the original on 3 August 2020. Retrieved 16 April 2018.
  6. ^ Kodama Takeshi; Chung Kai Cheong; Duarte Sergio Jose Barbosa (1 March 1990). Relativistic Aspects Of Nuclear Physics - Rio De Janeiro International Workshop. #N/A. pp. 241–. ISBN 978-981-4611-69-5. Archived from the original on 19 August 2020. Retrieved 16 April 2018.
  7. ^ a b Alford, Mark G.; Han, Sophia; Prakash, Madappa (2013). "Generic conditions for stable hybrid stars". Physical Review D. 88 (8): 083013. arXiv:1302.4732. Bibcode:2013PhRvD..88h3013A. doi:10.1103/PhysRevD.88.083013. S2CID 118570745.
  8. ^ a b Goyal, Ashok (2004). "Hybrid stars". Pramana. 62 (3): 753–756. arXiv:hep-ph/0303180. Bibcode:2004Prama..62..753G. doi:10.1007/BF02705363. S2CID 16582500.
  9. ^ a b Benić, Sanjin; Blaschke, David; Alvarez-Castillo, David E; Fischer, Tobias; Typel, Stefan (2015). "A new quark-hadron hybrid equation of state for astrophysics". Astronomy & Astrophysics. 577: A40. arXiv:1411.2856. Bibcode:2015A&A...577A..40B. doi:10.1051/0004-6361/201425318. S2CID 55228960.
  10. ^ a b Alvarez-Castillo, D; Benic, S; Blaschke, D; Han, Sophia; Typel, S (2016). "Neutron star mass limit at 2 M⊙ supports the existence of a CEP". The European Physical Journal A. 52 (8): 232. arXiv:1608.02425. Bibcode:2016EPJA...52..232A. doi:10.1140/epja/i2016-16232-9. S2CID 119207674.
  11. ^ Jaikumar, P.; Reddy, S.; Steiner, A. W. (2006). "Strange star surface: A crust with nuggets". Physical Review Letters. 96 (4): 041101. arXiv:nucl-th/0507055. Bibcode:2006PhRvL..96d1101J. doi:10.1103/PhysRevLett.96.041101. PMID 16486800. S2CID 7884769.
  12. ^ a b Alford, Mark G.; Rajagopal, Krishna; Reddy, Sanjay; Steiner, Andrew W. (2006). "Stability of strange star crusts and strangelets". Physical Review D. 73 (11): 114016. arXiv:hep-ph/0604134. Bibcode:2006PhRvD..73k4016A. doi:10.1103/PhysRevD.73.114016. S2CID 35951483.
  13. ^ Chamel, Nicolas; Haensel, Pawel (2008). "Physics of Neutron Star Crusts". Living Reviews in Relativity. 11 (1): 10. arXiv:0812.3955. Bibcode:2008LRR....11...10C. doi:10.12942/lrr-2008-10. ISSN 1433-8351. PMC 5255077. PMID 28163609.
  14. ^ a b Witten, Edward (1984). "Cosmic separation of phases". Physical Review D. 30 (2): 272–285. Bibcode:1984PhRvD..30..272W. doi:10.1103/PhysRevD.30.272.
  15. ^ Kurban, Abdusattar; Huang, Yong-Feng; Geng, Jin-Jun; Zong, Hong-Shi (May 27, 2022). "Searching for strange quark matter objects among white dwarfs". Physics Letters B. 832: 137204. arXiv:2012.05748. Bibcode:2022PhLB..83237204K. doi:10.1016/j.physletb.2022.137204. S2CID 228083632.

Further reading

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