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Quark star

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Title: Quark star  
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Subject: Neutron star, Exotic star, Q star, Stellar black hole, White dwarf
Collection: Degenerate Stars, Exotic Matter, Hypothetical Stars, Quark Stars, Star Types, Unsolved Problems in Physics
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Quark star

A quark star is a hypothetical type of compact exotic star composed of quark matter. These are ultra-dense phases of degenerate matter theorized to form inside particularly massive neutron stars.

The existence of quark stars has not been confirmed theoretically or astronomically. The equation of state of quark matter is uncertain, as is the transition point between neutron-degenerate matter and quark matter. Theoretical uncertainties have precluded making predictions from first principles. Experimentally, the behaviour of quark matter is currently being actively studied with particle colliders, although this can only produce hot quark-gluon plasma blobs the size of an atomic nucleus, which decay immediately after formation. There are no known artificial methods to produce or store cold quark matter as it would be found in quark stars.


  • Creation 1
    • Stability and strange quark matter 1.1
    • Strange stars 1.2
  • Characteristics 2
    • Strange stars 2.1
  • Other theorized quark formations 3
  • Observed overdense neutron stars 4
  • See also 5
  • References 6
  • External links 7


It is theorized that when the neutron-degenerate matter, which makes up neutron stars, is put under sufficient pressure from the star's own gravity or the initial supernova creating it, the individual neutrons break down into their constituent quarks (up quarks and down quarks), forming what is known as quark matter. This conversion might be confined to the neutron star's center or it might transform the entire star, depending on the physical circumstances.[1] Such a star is known as a quark star.

Stability and strange quark matter

Ordinary quark matter consisting of up and down quarks (also referred to as u and d quarks) has a very high Fermi energy compared to ordinary atomic matter and is only stable under extreme temperatures and/or pressures. This suggests that only quark stars comprising neutron stars with a quark matter core will be stable, while quark stars consisting entirely of ordinary quark matter will be highly unstable and dissolve spontaneously.[2][3]

It has been shown that the high Fermi energy making ordinary quark matter unstable at low temperatures and pressures can be lowered substantially by the transformation of a sufficient number of u and d quarks into strange quarks, as strange quarks are, relatively speaking, a very heavy type of quark particle.[2] This kind of quark matter is known specifically as strange quark matter and it is speculated and subject to current scientific investigation whether it might in fact be stable under the conditions of interstellar space (i.e. near zero external pressure and temperature). If this is the case (known as the Bodmer–Witten assumption), quark stars made entirely of quark matter would be stable if they quickly transform into strange quark matter.[4]

Strange stars

Quark stars made of strange quark matter are known as strange stars, and they form a subgroup under the quark star category.[4]

Strange stars might exist without regard of 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.[1] Such strange stars will naturally have a crust layer of neutron star material. 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. Stars partially made up of quark matter (including strange quark matter) are also referred to as hybrid stars.[5][6]

Theoretical investigations have revealed that quark stars might not only be produced from neutron stars and powerful supernovas, but they could also be created in the early cosmic phase separations following the Big Bang.[2] If these primordial quark stars transform into strange quark matter before the external temperature and pressure conditions of the early Universe makes them unstable, they might turn out stable, if the Bodmer–Witten assumption holds true. Such primordial strange stars could survive to this day.[2]


If the conversion of neutron-degenerate matter to (strange) quark matter is total, a quark star can to some extent be imagined as a single gigantic hadron. But this "hadron" will be bound by gravity, rather than the strong force that binds ordinary hadrons.

Strange stars

Recent theoretical research has found mechanisms by which quark stars with "strange quark nuggets" may decrease the objects' electric fields and densities from previous theoretical expectations, causing such stars to appear very much like — nearly indistinguishable from — ordinary neutron stars. This suggests that many, or even all, known neutron stars might in fact be strange stars. However, the investigating team of Prashanth Jaikumar, Sanjay Reddy, and Andrew W. Steiner made some fundamental assumptions, that led to uncertainties in their results large enough that the case is not finally settled. More research, both observational and theoretical, remains to be done on strange stars in the future.[7]

Other theoretical work[8] contends that, "A sharp interface between quark matter and the vacuum would have very different properties from the surface of a neutron star"; and, 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.

Other theorized quark formations

  • Jaffe 1977, suggested a four-quark state with strangeness (qsqs).
  • Jaffe 1977 suggested the H dibaryon, a six-quark state with equal numbers of up-, down-, and strange quarks (represented as uuddss or udsuds).
  • Bound multi-quark systems with heavy quarks (QQqq).
  • In 1987, a pentaquark state was first proposed with a charm anti-quark (qqqsc).
  • Pentaquark state with an antistrange quark and four light quarks consisting of up- and down-quarks only (qqqqs).
  • Light pentaquarks are grouped within an antidecuplet, the lightest candidate, Ө+.
    • This can also be described by the diquark model of Jaffe and Wilczek (QCD).
  • Ө++ and antiparticle Ө−−.
  • Doubly strange pentaquark (ssddu), member of the light pentaquark antidecuplet.
  • Charmed pentaquark Өc(3100) (uuddc) state was detected by the H1 collaboration.[9]
  • Tetra quark particles might form inside neutron stars and under other extreme conditions. In 2008, 2013 and 2014 the tetra quark particle of Z(4430), was discovered and investigated in laboratories on Earth.[10]

Observed overdense neutron stars

Statistically, the probability of a neutron star being a quark star is low, so in the Milky Way there would only be a small population of quark stars. If it is correct however, that overdense neutron stars can turn into quark stars, that makes the possible number of quark stars higher than was originally thought, as we would be looking for the wrong type of star.

Quark stars and strange stars are entirely hypothetical as of 2011, but observations released by the Chandra X-ray Observatory on April 10, 2002 detected two candidates, designated RX J1856.5-3754 and 3C58, which had previously been thought to be neutron stars. Based on the known laws of physics, the former appeared much smaller and the latter much colder than it should be, suggesting that they are composed of material denser than neutron-degenerate matter. However, these observations are met with skepticism by researchers who say the results were not conclusive;[11] and since the late 2000s, the possibility that RX J1856 is a quark star has been excluded (see RX J1856.5-3754).

Another star, XTE J1739-285,[12] has been observed by a team led by Philip Kaaret of the University of Iowa and reported as a possible candidate.

In 2006, Y. L. Yue et al., from Peking University, suggested that PSR B0943+10 may in fact be a low-mass quark star.[13]

It was reported in 2008 that observations of supernovae SN2006gy, SN2005gj and SN2005ap also suggest the existence of quark stars.[14] It has been suggested that the collapsed core of supernova SN1987A may be a quark star.[15][16]

See also


  1. ^ a b Shapiro and Teukolsky: Black Holes, White Dwarfs and Neutron Stars: The Physics of Compact Objects, Wiley 2008
  2. ^ a b c d Witten, Edward (1984). "Cosmic separation of phases". Physical Review D 30 (2): 272–285.  
  3. ^ E. Farhi; R. L. Jaffe (1984). "Strange matter". Physical Review D 30: 2379.  
  4. ^ a b Fridolin Weber; et al. (1994). "Strange-matter Stars". Proceedings: Strangeness and Quark Matter. World Scientific. 
  5. ^ Mark G. Alford, Sophia Han and Madappa Prakash (2013). "Generic conditions for stable hybrid stars". Phys. Rev. D 88, 083013.  
  6. ^ Ashok Goyal (March 2014). "Hybrid stars" (PDF). Pramana - journal of physics, Vol. 62, No. 3 (Indian Academy of Sciences): 753–56. Retrieved 22 March 2014. 
  7. ^ Jaikumar, Prashanth; Reddy, Sanjay; Steiner, Andrew (2006). "Strange Star Surface: A Crust with Nuggets". Physical Review Letters 96 (4).  
  8. ^ Alford, Mark; Rajagopal, Krishna; Reddy, Sanjay; Steiner, Andrew (2006). "Stability of strange star crusts and strangelets". Physical Review D 73 (11).  
  9. ^ H1 Collaboration; Aktas, A.; Andreev, V.; Anthonis, T.; Asmone, A.; Babaev, A.; Backovic, S.; Bähr, J.; et al. (2004). "Evidence for a Narrow Anti-Charmed Baryon State of mass". Physics Letters B 588: 17–28.  
  10. ^ Brian Koberlein (April 10, 2014). "How CERN’s Discovery of Exotic Particles May Affect Astrophysics". Universe Today. Retrieved 14 April 2014. /
  11. ^ Truemper, J. E.; Burwitz, V.; Haberl, F.; Zavlin, V. E. (June 2004). "The puzzles of RX J1856.5-3754: neutron star or quark star?". Nuclear Physics B Proceedings Supplements 132: 560–565.  
  12. ^ Fastest spinning star may have exotic heart
  13. ^
  14. ^ Astronomy Now Online – Second Supernovae Point to Quark Stars
  15. ^ Chan; Cheng; Harko; Lau; Lin; Suen; Tian (2009). "Could the compact remnant of SN 1987A be a quark star?". Astrophysical Journal 695: 732–746.  
  16. ^ Quark star may hold secret to early universe New Scientist
  • Quark star on

External links

  • Jaffe, R. (1977). "Perhaps a Stable Dihyperon". Physical Review Letters 38 (5): 195–198.  
  • Neutron Star/Quark Star Interior (image to print)
  • Quark star glimmers, Nature, April 11, 2002.
  • Debate sparked on quark stars, CERN Courier 42, #5.
  • Wish Upon a Quark Star, Paul Beck, Popular Science, June 2002.
  • Drake; Marshall; Dreizler; Freeman; Fruscione; Juda; Kashyap; Nicastro; et al. (2002). "Is RX J185635-375 a Quark Star?". Astrophysical Journal 572 (2): 996–1001.  
  • Perhaps a 1,700-year-old quark star in SNR MSH 15-52
  • Curious About Astronomy: What process would bring about a quark star?
  • RX J185635-375: Candidate Quark Star, Astronomy Picture of the Day, April 14, 2002.
  • Quarks or Quirky Neutron Stars?, Mark K. Anderson, Wired News, April 19, 2002.
  • Strange Quark Stars, Ask an Astrophysicist, question submitted April 12, 2002.
  • Seeing "Strange" Stars,, February 8, 2006.
  • Quark Stars Could Produce Biggest Bang,, June 7, 2006.
  • Meissner Effect in Strange Quark Stars, Brian Niebergal, web page, University of Calgary.
  • Irina Sagert; Mirjam Wietoska; Jurgen Schaffner-Bielich (2006). "Strange Exotic States and Compact Stars". Journal of Physics G 32 (12): S241–S249.  
  • Quark Stars Involved in New Theory of Brightest Supernovae – The first-ever evidence of a neutron star collapsing into a quark star is announced,, 3 June 2008
  • Quark Stars, Alternate View Column AV-114, John G. Cramer, Published in the November-2002 issue of Analog Science Fiction & Fact Magazine
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