Editing Quark star

{{short description|Compact exotic star which forms matter consisting mostly of quarks}}
{{distinguish|Quasar|Q star}}
{{More citations needed|date=March 2024}}
A '''quark star''' is a hypothetical type of [[compact star|compact]], [[exotic star]], where extremely high core temperature and pressure have forced [[Nucleon|nuclear particles]] to form [[quark matter]], a continuous [[state of matter]] consisting of free [[quark]]s.<ref>{{cite news |last1=Sutter |first1=Paul |title=These Stars Are Like Nothing Else You’ll Ever See |url=https://www.popularmechanics.com/space/deep-space/a45456628/cosmologist-explains-weird-quark-stars/ |access-date=6 July 2024 |publisher=Popular Mechanics |date=5 October 2023}}</ref>

==Background==
{{Unreferenced section|date=March 2024}} 
Some [[star#Massive stars|massive stars]] collapse to form [[neutron stars]] at the end of their [[stellar life cycle|life cycle]], as has been both observed and explained theoretically. Under the extreme temperatures and pressures inside neutron stars, the neutrons are normally kept apart by a [[Neutron degeneracy|degeneracy pressure]], stabilizing the star and hindering further gravitational collapse.<ref>{{Cite web |last=Seife |first=Charles |title=Quark Stars Get Real |url=https://www.science.org/content/article/quark-stars-get-real |website=Science.org}}</ref> However, it is hypothesized that under even more extreme temperature and pressure, the degeneracy pressure of the neutrons is overcome, and the [[neutrons]] are forced to merge and dissolve into their constituent quarks, creating an ultra-dense [[Phase (matter)|phase]] of [[quark matter]] based on densely packed quarks. In this state, a new equilibrium is supposed to emerge, as a new degeneracy pressure between the quarks, as well as repulsive [[electromagnetic force]]s, will occur and hinder [[black hole|total gravitational collapse]].

If these ideas are correct, quark stars might occur, and be observable, somewhere in the universe. Such a scenario is seen as scientifically plausible, but has not been proven observationally or experimentally; the very extreme conditions needed for stabilizing quark matter cannot be created in any laboratory and has not been observed directly in nature. The stability of quark matter, and hence the existence of quark stars, is for these reasons among the [[List of unsolved problems in physics|unsolved problems in physics]].

If quark stars can form, then the most likely place to find quark star matter would be inside [[neutron star]]s that exceed the internal pressure needed for [[degenerate matter|quark degeneracy]] – the point at which [[neutron]]s break down into a form of dense quark matter. They could also form if a [[massive star]] [[core collapse supernova|collapses]] at the end of its life, provided that it is possible for a star to be large enough to collapse beyond a neutron star but not large enough to form a [[black hole]].

If they exist, quark stars would resemble and be easily mistaken for neutron stars: they would form in the death of a massive star in a [[Type II supernova]], be extremely dense and small, and possess a very high gravitational field. They would also lack some features of neutron stars, unless they also contained a shell of neutron matter, because free quarks are not expected to have properties matching degenerate neutron matter. For example, they might be radio-silent, or have atypical sizes, electromagnetic fields, or surface temperatures, compared to neutron stars.

==History==
The analysis about quark stars was first proposed in 1965 by Soviet physicists [[Dmitri Ivanenko|D. D. Ivanenko]] and [[D. F. Kurdgelaidze]].<ref>{{cite journal |title=Hypothesis concerning quark stars |last1=Ivanenko |first1=Dmitri D. |last2=Kurdgelaidze |first2=D. F. |journal=Astrophysics |volume=1 |issue=4 |pages=251–252 |date=1965 |bibcode=1965Ap......1..251I |doi=10.1007/BF01042830 |s2cid=119657479 }}</ref><ref>{{cite journal |title=Remarks on quark stars |last1=Ivanenko |first1=Dmitri D. |last2=Kurdgelaidze |first2=D. F. |journal=Lettere al Nuovo Cimento |volume=2 |pages=13–16 |date=1969 |bibcode=1969NCimL...2...13I |doi=10.1007/BF02753988|s2cid=120712416 }}</ref> Their existence has not been confirmed.

The [[equation of state]] of [[quark matter]] is uncertain, as is the transition point between neutron-degenerate matter and quark matter.<ref>{{Cite journal |last=Mishra |first=H. |last2=Misra |first2=S.P. |last3=Panda |first3=P.K. |last4=Parida |first4=B.K. |date=1993 |title=NEUTRON MATTER – QUARK MATTER PHASE TRANSITION AND QUARK STAR |url=https://www.worldscientific.com/doi/abs/10.1142/S0218301393000212 |journal=International Journal of Modern Physics E |language=en |volume=02 |issue=03 |pages=547–563 |doi=10.1142/S0218301393000212 |issn=0218-3013|arxiv=nucl-th/9301003 }}</ref> Theoretical uncertainties have precluded making predictions from [[first principles]]. Experimentally, the behaviour of quark matter is being actively studied with particle colliders, but this can only produce very hot (above 10<sup>12</sup>&nbsp;[[Kelvin (unit)|K]]) [[quark–gluon plasma]] blobs the size of atomic nuclei, which decay immediately after formation. The conditions inside compact stars with extremely high densities and temperatures well below 10<sup>12</sup>&nbsp;[[Kelvin (unit)|K]] cannot be recreated artificially, as there are no known methods to produce, store or study "cold" quark matter directly as it would be found inside quark stars. The theory predicts quark matter to possess some peculiar characteristics under these conditions.{{citation needed|date=March 2024}}

==Formation==
[[File:TOV solution neutron quark star mass radius diagram.png|thumb|upright=1.75|Mass–radius relations for models of a neutron star with no exotic states (red) and a quark star (blue)<ref>F. Douchin, P. Haensel, ''A unified equation of state of dense matter and neutron star structure'', "Astron. Astrophys." 380, 151 (2001).</ref>]]
It is hypothesized that when the [[neutron-degenerate matter]], which makes up [[neutron star]]s, is put under sufficient pressure from the star's own [[gravity]] or the initial [[supernova]] creating it, the individual [[neutron]]s break down into their constituent [[quark]]s ([[up quark]]s and [[down quark]]s), forming what is known as quark matter. This conversion may be confined to the neutron star's center or it might transform the entire star, depending on the physical circumstances. Such a star is known as a quark star.<ref name="Shapiro">{{cite book |last1=Shapiro |first1=Stuart L. |last2=Teukolsky |first2=Saul A. |title=Black Holes, White Dwarfs and Neutron Stars: The Physics of Compact Objects |publisher=Wiley |year=2008 |isbn=978-0471873167}}</ref><ref>{{cite book |editor-last1=Blaschke |editor-first1=David |editor-first2=Armen |editor-last2=Sedrakian |editor-first3=Norman K. |editor-last3=Glendenning |title=Physics of Neutron Star Interiors |series=Lecture Notes in Physics |volume=578 |publisher=Springer-Verlag |year=2001 |doi=10.1007/3-540-44578-1 |isbn=978-3-540-42340-9 }}</ref>

===Stability and strange quark matter===
Ordinary quark matter consisting of up and down quarks has a very high [[Fermi energy]] compared to ordinary atomic matter and is stable only under extreme temperatures and/or pressures. This suggests that the only stable quark stars will be neutron stars with a quark matter core, while quark stars consisting entirely of ordinary quark matter will be highly unstable and re-arrange spontaneously.<ref name="Witten">{{cite journal |last1=Witten |first1=Edward |title=Cosmic separation of phases |journal=Physical Review D |volume=30 |issue=2 |pages=272–285 |date=1984 |doi=10.1103/PhysRevD.30.272 |bibcode=1984PhRvD..30..272W }}</ref><ref>{{cite journal |title=Strange matter |last1=Farhi |first1=Edward |last2=Jaffe |first2=Robert L. |journal=Physical Review D |volume=30 |issue= 11 |pages=2379 |date=1984 |bibcode=1984PhRvD..30.2379F |doi=10.1103/PhysRevD.30.2379}}</ref>

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 up and down quarks into [[strange quark]]s, as strange quarks are, relatively speaking, a very heavy type of quark particle.<ref name="Witten" /> 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–[[Edward Witten|Witten]] assumption), quark stars made entirely of quark matter would be stable if they quickly transform into strange quark matter.<ref name="Weber">{{Cite web|title=Strange-matter Stars |url=https://cds.cern.ch/record/278675 |last1=Weber |first1=Fridolin |last2=Kettner |first2=Christiane |last3=Weigel |first3=Manfred K. |last4=Glendenning |first4=Norman K. |journal= |date=1995 |access-date=2020-03-26 |archive-date=2022-03-22 |archive-url=https://web.archive.org/web/20220322124648/https://cds.cern.ch/record/278675 |url-status=live }} in {{cite book |title=International Symposium on Strangeness and Quark Matter, Kolymbari, Greece, 1-5 Sep 1994 |pages=308–317 |publisher=World Scientific |location=Singapore |editor-last1=Kumar |editor-first1=Shiva |editor-last2=Madsen |editor-first2=Jes |editor-last3=Panagiotou |editor-first3=Apostolos D. |editor-last4=Vassiliadis |editor-first4=G. }}</ref>

===Strange stars===
{{main|Strange star}}
Stars made of [[strange quark matter]] are known as strange stars.  These form a distinct subtype of quark stars.<ref name="Weber" />

Theoretical investigations have revealed that quark stars might not only be produced from neutron stars and powerful supernovas, they could also be created in the early [[Chronology of the universe#Hadron epoch|cosmic phase separations]] following the [[Big Bang]].<ref name="Witten" /> 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.<ref name="Witten" />

==Characteristics==
Quark stars have some special characteristics that separate them from ordinary neutron stars. Under the physical conditions found inside neutron stars, with extremely high densities but temperatures well below 10<sup>12</sup> K, quark matter is predicted to exhibit some peculiar characteristics. It is expected to behave as a [[Fermi liquid]] and enter a so-called color-flavor-locked (CFL) phase of [[color superconductivity]], where "color" refers to the six "charges" exhibited in the [[strong interaction]], instead of the two charges (positive and negative) in [[electromagnetism]]. At slightly lower densities, corresponding to higher layers closer to the surface of the compact star, the quark matter will behave as a non-CFL quark liquid, a phase that is even more mysterious than CFL and might include color conductivity and/or several additional yet undiscovered phases. None of these extreme conditions can currently be recreated in laboratories so nothing can be inferred about these phases from direct experiments.<ref>{{cite journal |last1=Alford |first1=Mark G. |last2=Schmitt |first2=Andreas |last3=Rajagopal |first3=Krishna |last4=Schäfer |first4=Thomas |title=Color superconductivity in dense quark matter |arxiv=0709.4635 |journal=Reviews of Modern Physics |volume=80 |issue=4 |pages=1455–1515 |year=2008 |doi=10.1103/RevModPhys.80.1455 |bibcode=2008RvMP...80.1455A |s2cid=14117263 }}</ref>

==Observed overdense neutron stars==
At least under the assumptions mentioned above, the probability of a given neutron star being a quark star is low,{{citation needed|date=March 2014}} 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 observers would be looking for the wrong type of star.{{citation needed|date=May 2018}}

A neutron star without deconfinement to quarks and higher densities cannot have a rotational period shorter than a millisecond; even with the unimaginable gravity of such a condensed object the centrifugal force of faster rotation would eject matter from the surface, so detection of a pulsar of millisecond or less period would be strong evidence of a quark star.

Observations released by the [[Chandra X-ray Observatory]] on April 10, 2002, detected two possible quark stars, designated [[RX J1856.5−3754]] and [[3C 58]], 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;<ref name="Truemper2004">{{cite journal |last1=Trümper |first1=Joachim E. |last2=Burwitz |first2=Vadim |last3=Haberl |first3=Frank W. |last4=Zavlin |first4=Vyatcheslav E. |title=The puzzles of RX J1856.5-3754: neutron star or quark star? |journal=Nuclear Physics B: Proceedings Supplements |date=June 2004 |volume=132 |pages=560–565 |doi=10.1016/j.nuclphysbps.2004.04.094 |bibcode=2004NuPhS.132..560T |arxiv=astro-ph/0312600 |citeseerx=10.1.1.314.7466 |s2cid=425112 }}</ref> and since the late 2000s, the possibility that [[RX J1856.5-3754|RX J1856]] is a quark star has been excluded.

Another star, [[XTE J1739-285]],<ref>Shiga, David; [https://www.newscientist.com/article/dn11221?DCMP=NLC-nletter&nsref=dn11221 "Fastest spinning star may have exotic heart"] {{Webarchive|url=https://web.archive.org/web/20120825035205/http://www.newscientist.com/article/dn11221?DCMP=NLC-nletter&nsref=dn11221 |date=2012-08-25 }}, ''New Scientist'', 2007 February 20</ref> has been observed by a team led by Philip Kaaret of the [[University of Iowa]] and reported as a possible quark star candidate.

In 2006, You-Ling Yue et al., from [[Peking University]], suggested that [[PSR B0943+10]] may in fact be a low-mass quark star.<ref>{{cite journal |first1=You-Ling |last1=Yue |first2=Xiao-Hong |last2=Cui |first3=Ren-Xin |last3=Xu |title=Is PSR B0943+10 a low-mass quark star? |journal=Astrophysical Journal |volume=649 |issue=2 |pages=L95–L98 |year=2006 |arxiv=astro-ph/0603468 |doi=10.1086/508421 |bibcode=2006ApJ...649L..95Y |s2cid=18183996 }}</ref>

It was reported in 2008 that observations of supernovae [[SN 2006gy]], [[SN 2005gj]] and [[SN 2005ap]] also suggest the existence of quark stars.<ref>Chadha, Kulvinder Singh; [http://astronomynow.com/080604Secondsupernovaepointtoquarkstars.html "Second Supernovae Point to Quark Stars"] {{Webarchive|url=https://web.archive.org/web/20100125145543/http://astronomynow.com/080604Secondsupernovaepointtoquarkstars.html |date=2010-01-25 }}, ''Astronomy Now Online'', 2008 June 04</ref> It has been suggested that the collapsed core of supernova [[SN 1987A]] may be a quark star.<ref>{{cite journal |author1=Chan |author2=Cheng |author3=Harko |author4=Lau |author5=Lin |author6=Suen |author7=Tian |doi=10.1088/0004-637X/695/1/732 |journal=Astrophysical Journal |title=Could the compact remnant of SN 1987A be a quark star? |volume=695 |issue=1 |pages=732–746 |year=2009 |arxiv=0902.0653|bibcode = 2009ApJ...695..732C |s2cid=14402008 }}</ref><ref>Parsons, Paul; [https://www.newscientist.com/article/mg20126964.700-quark-star-may-hold-secret-to-early-universe.html "Quark star may hold secret to early universe"] {{Webarchive|url=https://web.archive.org/web/20150318100318/http://www.newscientist.com/article/mg20126964.700-quark-star-may-hold-secret-to-early-universe.html |date=2015-03-18 }}, ''New Scientist'', 2009 February 18</ref>

In 2015, Zi-Gao Dai et al. from Nanjing University suggested that Supernova [[ASASSN-15lh]] is a newborn strange quark star.<ref>{{Cite journal |title=The Most Luminous Supernova ASASSN-15lh: Signature of a Newborn Rapidly-Rotating Strange Quark Star |arxiv=1508.07745 |date=2015-08-31 |first1=Zi-Gao |last1=Dai |first2=Shan-Qin |last2=Wang |first3=J. S. |last3=Wang |first4=Ling-Jun |last4=Wang |first5=Yun-Wei |last5=Yu |doi=10.3847/0004-637X/817/2/132 |volume=817 |issue=2 |journal=The Astrophysical Journal |page=132 |bibcode=2016ApJ...817..132D |s2cid=54823427 |doi-access=free }}</ref>

In 2022 it was suggested that GW190425, which likely formed as a merger between two neutron stars giving off gravitational waves in the process, could be a quark star.<ref>{{cite web | url=https://www.space.com/strange-quark-stars-from-neutron-star-mergers | title=Strange quark star may have formed from a lucky cosmic merger | website=[[Space.com]] | date=16 September 2022 }}</ref>

==Other hypothesized quark formations==
{{more citations needed|section|date=December 2015}}
Apart from ordinary quark matter and strange quark matter, other types of [[Quark–gluon plasma|quark-gluon plasma]] might hypothetically occur or be formed inside neutron stars and quark stars. This includes the following, some of which has been observed and studied in laboratories:

* Robert L. Jaffe 1977, suggested a [[tetraquark|four-quark]] state with strangeness (qs{{overline|qs}}).
* Robert L. 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 (QQ{{overline|qq}}).
* In 1987, a [[pentaquark]] state was first proposed with a charm anti-quark (qqqs{{overline|c}}).
* Pentaquark state with an antistrange quark and four light quarks consisting of up- and down-quarks only (qqqq{{overline|s}}).
* Light pentaquarks are grouped within an antidecuplet, the lightest candidate, Θ<sup>+</sup>, which can also be described by the diquark model of Robert L. Jaffe and Wilczek ([[Quantum chromodynamics|QCD]]).
* [[pentaquark|Θ]]<sup>++</sup> and antiparticle {{overline|Θ}}<sup>−−</sup>.
* Doubly strange pentaquark (ssdd{{overline|u}}), member of the light pentaquark antidecuplet.
* Charmed pentaquark Θ<sub>c</sub>(3100) (uudd{{overline|c}}) state was detected by the H1 collaboration.<ref name="H1">{{cite journal |author1=H1 Collaboration |doi=10.1016/j.physletb.2004.03.012 |journal=Physics Letters B |last2=Aktas |first2=A. |last3=Andreev |first3=V. |last4=Anthonis |first4=T. |last5=Asmone |first5=A. |last6=Babaev |first6=A. |last7=Backovic |first7=S. |last8=Bähr |first8=J. |last9=Baranov |first9=P. |display-authors=6 |title=Evidence for a narrow anti-charmed baryon state of mass |volume=588 |issue=1–2 |pages=17–28 |year=2004 |arxiv=hep-ex/0403017 |bibcode=2004PhLB..588...17A |s2cid=119375207 }}</ref>
* Tetraquark particles might form inside neutron stars and under other extreme conditions. In 2008, 2013 and 2014 the tetraquark particle of [[Z(4430)]], was discovered and investigated in laboratories on [[Earth]].<ref>{{cite web |url=http://www.universetoday.com/111110/how-cerns-discovery-of-exotic-particles-may-affect-astrophysics |title=How CERN's discovery of exotic particles may affect astrophysics |last=Koberlein |first=Brian |publisher=Universe Today |date=10 April 2014 |access-date=14 April 2014 |archive-date=14 April 2014 |archive-url=https://web.archive.org/web/20140414053520/http://www.universetoday.com/111110/how-cerns-discovery-of-exotic-particles-may-affect-astrophysics/ |url-status=live }}/</ref>

==See also==
{{Portal|Physics|Astronomy}}
<!-- alphabetical order please [[WP:SEEALSO]] -->
<!-- please add a short description [[WP:SEEALSO]], via {{subst:AnnotatedListOfLinks}} or {{Annotated link}} -->
{{div col|colwidth=20em|small=yes}}
* {{Annotated link |Deconfinement}}
* {{Annotated link |Neutron}}
** {{Annotated link |Neutron matter}}
** {{Annotated link |Neutron stars}}
* {{Annotated link |Planck star}}
* {{Annotated link |Quark-nova}}
* {{Annotated link |Quantum chromodynamics}}
* {{Annotated link |Tolman–Oppenheimer–Volkoff limit}}
* {{Annotated link |Degenerate matter}}
** {{Annotated link |Neutron matter}}
** {{Annotated link |Preon matter}}
** {{Annotated link |QCD matter}}
** {{Annotated link |Quark–gluon plasma}}
** {{Annotated link |Quark matter}}
** {{Annotated link |Strangelet}}
* {{Annotated link |Compact star}}
** {{Annotated link |Exotic star}}
** {{Annotated link |Magnetar}}
** {{Annotated link |Neutron star}}
** {{Annotated link |Pulsar}}
** {{Annotated link |Stellar black hole}}
** {{Annotated link |White dwarf}}
{{div col end}}
<!-- alphabetical order please [[WP:SEEALSO]] -->

==References==
{{reflist}}

==Sources and further reading==
* {{cite book |editor-last1=Blaschke |editor-first1=David |editor-last2=Sedrakian |editor-first2=David |title=Superdense QCD Matter and Compact Stars |series=NATO Science Series II: Mathematics, Physics and Chemistry |volume=197 |publisher=Springer |year=2003 |doi=10.1007/1-4020-3430-X |isbn=978-1-4020-3428-2 |url=https://cds.cern.ch/record/1338948 }}
* {{cite book |editor-last1=Blaschke |editor-first1=David |editor-first2=Armen |editor-last2=Sedrakian |editor-first3=Norman K. |editor-last3=Glendenning |title=Physics of Neutron Star Interiors |series=Lecture Notes in Physics |volume=578 |publisher=Springer-Verlag |year=2001 |doi=10.1007/3-540-44578-1 |isbn=978-3-540-42340-9 }}
* {{cite book |editor-last1=Plessas |editor-first1=Willibald |editor-last2=Mathelitsch |editor-first2=Leopold |url=https://searchworks.stanford.edu/view/4788102 |title=Lectures on Quark Matter |series=Lecture Notes in Physics |volume=583 |publisher=Springer |year=2002 |doi=10.1007/3-540-45792-5 |isbn=978-3-540-43234-0 }}

==External links==
*{{cite journal |last1=Jaffe |first1=Robert L. |title=Perhaps a Stable Dihyperon |journal=Physical Review Letters |volume=38 |issue=5 |pages=195–198 |date=1977 |doi=10.1103/PhysRevLett.38.195|bibcode = 1977PhRvL..38..195J |osti=1446298 |url=https://www.slac.stanford.edu/cgi-bin/getdoc/slac-pub-1828.pdf }}
*[http://chandra.harvard.edu/photo/2002/0211/0211_illustration_300.jpg Neutron Star/Quark Star Interior (image to print)]
*Whitfield, John; [http://www.nature.com/news/2002/020411/full/news020408-8.html "Quark star glimmers"],  ''[[Nature (journal)|Nature]]'', 2002 April 11
*[https://cerncourier.com/a/debate-sparked-on-quark-stars/ "Debate sparked on quark stars"], ''CERN Courier'' '''42''', #5, June 2002, [https://cds.cern.ch/record/1733341 page 13]
*Beck, Paul; [https://web.archive.org/web/20060313223759/http://www.popsci.com/popsci/aviationspace/a6885b4a1db84010vgnvcm1000004eecbccdrcrd.html "Wish Upon a Quark Star"], ''Popular Science'', June 2002
*{{cite journal |author1=Drake |author2=Marshall |author3=Dreizler |author4=Freeman |author5=Fruscione |author6=Juda |author7=Kashyap |author8=Nicastro |author9=Pease |display-authors=8 |doi=10.1086/340368 |journal=Astrophysical Journal |volume=572 |title=Is RX J185635-375 a Quark Star? |issue=2 |pages=996–1001 |date=2002 |arxiv=astro-ph/0204159 |bibcode = 2002ApJ...572..996D |s2cid=18481546 }}
*Krivoruchenko, M. I.; [http://www.jetpletters.ac.ru/ps/1224/article_18487.shtml "Strange, quark, and metastable neutron stars"] {{Webarchive|url=https://web.archive.org/web/20131016114425/http://www.jetpletters.ac.ru/ps/1224/article_18487.shtml |date=2013-10-16 }}, JETP Letters, vol. 46, no. 1, 10 July 1987, pages 3–6 (page 6: Perhaps a 1,700-year-old quark star in SNR MSH 15–52)
*Rothstein, Dave; [https://web.archive.org/web/20030418110053/http://curious.astro.cornell.edu/question.php?number=445 "Curious About Astronomy: What process would bring about a quark star?"], question #445, January 2003
*Nemiroff, Robert; Bonnell, Jerry; [http://antwrp.gsfc.nasa.gov/apod/ap020414.html "RX J185635-375: Candidate Quark Star"], ''Astronomy Picture of the Day'', NASA Goddard Space Flight Center, 2002 April 14
*Anderson, Mark K.: [https://web.archive.org/web/20030402151744/http://www.wired.com/news/technology/0,1282,51943-2,00.html Quarks or Quirky Neutron Stars?], ''Wired News'', 2002 April 19
*Boyce, Kevin; Still, Martin; [https://imagine.gsfc.nasa.gov/ask_astro/neutron_star.html "What is the news about a possible Strange Quark Star?"], ''Ask an Astrophysicist'', NASA Goddard Space Flight Center, 2002 April 12
*Marquit, Miranda; [http://www.physorg.com/news10646.html "Seeing 'Strange' Stars"], physorg.com, 2006 February 8
*[http://www.spacedaily.com/reports/Quark_Stars_Could_Produce_Biggest_Bang.html "Quark Stars Could Produce Biggest Bang"], spacedaily.com, 2006 June 7
*Niebergal, Brian: [https://web.archive.org/web/20090213124158/http://capca.ucalgary.ca/~bniebergal/webPHP/research.php?subdir=strangeQuarkStars "Meissner Effect in Strange Quark Stars"], Computational Astro-Physics Calgary Alberta, [[University of Calgary]]
*{{cite journal |first1=Irina |last1=Sagert |first2=Mirjam |last2=Wietoska |first3=Jurgen |last3=Schaffner-Bielich |doi=10.1088/0954-3899/32/12/S30 |journal=Journal of Physics G |volume=32 |title=Strange Exotic States and Compact Stars |issue=12 |pages=S241–S249 |date=2006 |arxiv=astro-ph/0608317 |bibcode=2006JPhG...32S.241S |citeseerx=10.1.1.257.2063 |s2cid=15151001 }}
*Bryner, Jeanna; [http://www.space.com/scienceastronomy/080603-aas-neutron-quark.html "Quark Stars Involved in New Theory of Brightest Supernovae"], ''Space.com'', 2008 June 3 (The first-ever evidence of a neutron star collapsing into a quark star is announced)
*Cramer, John G.: [http://www.npl.washington.edu/AV/altvw114.html "Quark Stars, Alternate View Column AV-114"], ''Analog Science Fiction & Fact Magazine'', November 2002

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[[Category:Unsolved problems in physics]]
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