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Above undated message substituted from Template:Dashboard.wikiedu.org assignmentbyPrimeBOT (talk) 07:35, 17 January 2022 (UTC)Reply
I can't decide whether strange stars deserve their own article, separate from strange matter. There is a Danish-language article on strange stars, so we get a nice interwiki link, and they make more sense if they link articles on the same things. But on the other hand, everything that one can say about a strange star is also something about strange matter, so we can't really remove the information from strange matter that I've moved here... Oh, I'll think about it later... -- Oliver P. 19:30 19 Jun 2003 (UTC)
It might be good to talk about Strange Matter/Quark Matter (I'd advocate the latter terminology) purely in terms of the physics of degenerate matter and the debate over it's plausibility (ie, does QCD allow the arrangement? Is the degeneracy pressure provided by the strong nuclear force strictly analogous to neutron or electron degeneracy pressure? Are exotic quark flavors required or implied by the theory?) and move the bulk of the astrophysical considerations to this writeup.
-Peter
Giant Hadron?
The star then becomes known as a "quark star" or "strange star", similar to a single gigantic hadron (but bound by gravity rather than the color force).
The force of gravity may have much to do with the binding of such a star, but wouldn't the color force also contribute to the binding energy? -- User:Kryptid Nov 2006
August 9,2011 — Preceding unsigned comment added by 78.32.66.91 (talk) 00:21, 10 August 2011 (UTC)Reply
Answers
Hello to all above in this section on "Strange Matter". Quark matter is highly unstable except under very extreme conditions of high temperature and/or pressure. This instability might change radically, by the introduction of strange quarks, at least if the Bodmer-witten assumption turns out to hold true. Therefore it is important to discuss strange quark matter in relation to quark matter and it is also important to discuss strange stars in relation to quark stars. If the Bodmer-Witten hypothesis is wrong, quark and strange stars will always by hybrid stars and could only exist as a subgroup of neutron stars. The whole idea of writing a separate article on quark stars, apart from neutron stars, is the Bodmer-Witten assumption, that strange quark matter is stable at low temperatures and pressures.
I have rewritten part of the article now and supplied some vital information on the differences and similarities of quark stars and strange stars. It can still be improved - especially the discussion on the binding forces of the "giant hadron" (not misspelled! :) and certainly the section on the "characteristics" of these stars -, but I believe the basics are represented in the article as of now. RhinoMind (talk) 13:45, 14 April 2014 (UTC)Reply
Shouldn't this article redirect to Quark Star or vice versa?
Is it strictly necessary to have strange quarks? If not then "Strange star" requres splitting into a separate section. Zzzzzzzzzzz 03:22, 10 June 2006 (UTC)Reply
Wired, Popular Science, and Astronomy Picture of the Day are not authoritative sources. Please replace these references with links to the papers they cite (or quote but don't cite).--Cherlin (talk) 21:40, 17 January 2008 (UTC)Reply
This article needs a serious overhaul. I hope to get to it in the near future, now that strangelet is in decent shape. Dark Formal (talk) 16:10, 6 February 2008 (UTC)Reply
Revised: The contents of a light containing star would be expected to be ultra relativistic. If the pressure P of ultra relativistic material is given as (rho)(c^2)/3 [where rho is the energy density], the total supporting energy or viral energy of this star would be ∫PdV = (Mc^2)/3, meaning a whopping 1/3 of the mass energy of the star would be used just to oppose the force of gravity. The gravitational binding energy of a gas star is about 1.1G(M^2)/R. Using the viral equation, if (Mc^2)/3 is equal to 1/2 of 1.1 G(M^2)/R, the radius R of this star equals 1.65GM/(c^2), or 0.82 the Schwarzschild radius. There is observational evidence that a large finite size star is contained in a black hole: Some super massive black holes have been observed spinning at about 1/10 RPM, which implies a star of very large radius. The existance of an about 0.82 Schwarschild radius star, instead of a conventional black hole point singularity, would probably mean the end of the conventional big bang model as coming from a point singularity. If 2 approximately equal mass 0.82 Schwarzchild radius stars merged the contents would be expected to be ejected at the speed of light from the contact point. This model could explain where our inflationary universe came from. It could also explain a possible ancient explosion at the center of M87. 172.162.231.22 (talk) 22:29, 16 November 2013 (UTC)BGReply
Simply stated, by a Quark star do you mean a neutron star with some quark matter production in the core? If so, shouldn't there simultaneously be much larger radiation production that the star would not contain? — Preceding unsigned comment added by 172.162.3.65 (talk) 21:44, 19 May 2014 (UTC)Reply
If neutrons in the core disintegrated collider results indicate that about 90% of the neutron mass should be converted to gamma rays (which would exit the star) and about 10% of the neutron mass should be converted to quark matter. Quark matter is mostly charged particles associated with high energy and should quickly recombine in a neutron star to form conventional nuclei. I don't see how quark matter could exist in a stable neutron star core in the way you describe. — Preceding unsigned comment added by 172.129.21.166 (talk) 23:55, 25 May 2014 (UTC)Reply
I don't think a star of ultra relativistic matter collapses even if its smaller than the Schwarzschild radius. This is because ultra relativistic pressure (like other pressures) increases as the inverse of R-cubed. The pressure increases faster than gravitational forces or gravitational potential energy108.46.17.166 (talk) 21:14, 13 July 2015 (UTC)BG.Reply
As of now, the section on Strange Stars does not describe what a strange star is. RhinoMind (talk) 23:44, 5 March 2014 (UTC)Reply
I cut this paragraph from the article:
It is speculated and subject to scientific investigation if (strange) quark matter once formed, might in fact be stable under zero external pressure (ie. in interstellar space). Nuggets of (strange) quark matter is thus one of several candidates for the theoretical and unknown dark matter, featured in many cosmological theories.[1][2]
I think it first and foremost belongs to the article on quark matter and strange quark matter respectively. It can be fitted in here as well, but it would need a solid explanation on how quark stars contribute with nuggets. They would indeed do if they exist in the first place, but it would need an explanation. RhinoMind (talk) 01:59, 6 March 2014 (UTC)Reply
References
The presence of this section needs a good explanation. The quark states discussed here, is more related to neutron stars, than quark stars. The various quark states might form at the core of neutron stars, under the extreme pressure and temperature, but they are not equivalent to what we know as quark matter.
The section at hand, has been discussed for various reasons previously. For the sake of structure and readability, I have collected these comments and discussions below.
RhinoMind (talk) 13:20, 14 April 2014 (UTC)Reply
This section should be deleted. First of all, to requote the Pentaquark page, there is "overwhelming evidence that the claimed pentaquarks do not exist".[1] The idea of 4, 5, and 6 quark hadrons has been discarded by the particle physics community. But this is besides the point, theoretical hadrons have nothing to do with structure of a quark star. It would be more appropriate to reference Quark-gluon plasma. Pulu (talk) 05:54, 27 August 2012 (UTC)Reply
I also think that this section is not relevant. Mi Tatara Buela (talk) 14:40, 20 November 2013 (UTC)Reply
All Strange stars are Quark stars. But, not all Quark stars are Strange stars. Other Quark Stars. Strange Exotic States and Compact Stars
http://xxx.lanl.gov/abs/astro-ph/0608317 Thanks, CarpD 1/07/06
References
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Be more analytical about that! It's fundamentally important! — Preceding unsigned comment added by 2.84.212.42 (talk) 01:49, 11 April 2018 (UTC)Reply