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Published: 10 December 2022
Last updated: 28 January 2023

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1

Weiss, Peter. "Strange Stars?" Science News 161, no. 16 (April 20, 2002): 246. http://dx.doi.org/10.2307/4013349.

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2

Alcock, Charles. "Strange stars." Nuclear Physics B - Proceedings Supplements 24, no. 2 (December 1991): 93–102. http://dx.doi.org/10.1016/0920-5632(91)90305-x.

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3

Alcock, Charles, Edward Farhi, and Angela Olinto. "Strange stars." Astrophysical Journal 310 (November 1986): 261. http://dx.doi.org/10.1086/164679.

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4

Reddy, Sanjay. "Strange crusts on strange stars." Journal of Physics G: Nuclear and Particle Physics 32, no. 12 (November 17, 2006): S267—S274. http://dx.doi.org/10.1088/0954-3899/32/12/s33.

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5

Gondek, Dorota. "Neutron stars and strange stars." International Astronomical Union Colloquium 160 (1996): 133–34. http://dx.doi.org/10.1017/s0252921100041282.

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If strange quark plasma is the real ground state of baryonic matter (Witten 1984), then some of neutron stars (NS) could actually be strange stars (SS). It is difficult to distinguish SS from NS observationally. They have similar radii and masses and their crusts are built of the same matter. It seems that a good method for testing the existence of SS would be the studies of phenomena related to the stellar pulsations. In 1976 Boriakoff proposed that radial oscillations of NS could be observed within radio subpulses of pulsars. While various modes of pulsations of NS were studied by a number of authors, little attention was paid to seismological signatures of SS. The radial oscilations of bare SS were studied by Väth & Chanmugam (1992). Recently Weber (this volume) studied properties of stars made of matter described by BPS equation of state (EOS) (Baym et al. 1971) with a ball of strange matter inside, but they mainly concentrated on stability of white-dwarf-like SS. In this work I present fully relativistic calculations of the radial oscillation frequencies of SS. I determined the fundamental frequency for bare SS and SS with two different types of crusts depending on origin (Alcock et al. 1986) of SS and showed differences between them.
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6

Weber, Fridolin, and Norman K. Glendenning. "Neutron Stars, Strange Pulsars and Strange Dwarfs." International Astronomical Union Colloquium 160 (1996): 135–36. http://dx.doi.org/10.1017/s0252921100041294.

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The hypothesis that strange quark matter may be the absolute ground state of the strong interaction (not56Fe) has been raised independently by Boder and Witten. If the hypothesis is true, then a separate class of compact stars could exist, which are calledstrange matter stars. The properties of the complete sequence of such stars, which range from compact neutron-star-like strange stars to strange dwarfs to strange planets. The latter two constitute the strange counterparts of ordinary white dwarfs and planets, respectively. The properties of these objects are discussed in this paper.
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7

Haensel, Pawel, and Julian L. Zdunik. "Accreting strange stars." Nuclear Physics B - Proceedings Supplements 24, no. 2 (December 1991): 139–43. http://dx.doi.org/10.1016/0920-5632(91)90312-3.

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8

Glendenning, N. K., Ch Kettner, and F. Weber. "From Strange Stars to Strange Dwarfs." Astrophysical Journal 450 (September 1995): 253. http://dx.doi.org/10.1086/176136.

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9

Xu, R. X. "Strange Quark Stars — A Review." Symposium - International Astronomical Union 214 (2003): 191–98. http://dx.doi.org/10.1017/s0074180900194392.

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A pedagogical overview of strange quark matter and strange stars is presented. After a historical notation of the research and an introduction to quark matter, a major part is devoted to the physics and astrophysics of strange stars, with attention being paid to the possible ways by which neutron stars and strange stars can be distinguished in astrophysics. Recent possible evidence for bare strange stars is also discussed.
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10

Olinto, Angela. "Converting neutron stars into strange stars." Nuclear Physics B - Proceedings Supplements 24, no. 2 (December 1991): 103–9. http://dx.doi.org/10.1016/0920-5632(91)90306-y.

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11

Xu, R. X., G. J. Qiao, and B. Zhang. "Are Pulsars Bare Strange Stars?" International Astronomical Union Colloquium 177 (2000): 665–66. http://dx.doi.org/10.1017/s0252921100060954.

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AbstractIt is believed that pulsars are neutron stars or strange stars with crusts. However we suggest here that pulsars may bebare strange stars(i.e., strange stars without crust). Due to rapid rotation and strong emission, young strange stars produced in supernova explosions should be bare when they act as radio pulsars. Because of strong magnetic field,twopolar-crusts would shield the polar caps of an accreting strange star. Such a suggestion can be checked by further observations.
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12

Grassi, F. "Quark core stars, quark stars and strange stars." Zeitschrift f�r Physik C Particles and Fields 44, no. 1 (March 1989): 129–38. http://dx.doi.org/10.1007/bf01548591.

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13

Weber, Fridolin, M. K. Weigel, and N. K. Glendenning. "Neutron stars, strange pulsars and strange dwarfs." Nuclear Physics A 621, no. 1-2 (August 1997): 385–87. http://dx.doi.org/10.1016/s0375-9474(97)00276-5.

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14

WEBER, FRIDOLIN, and NORMAN K. GLENDENNING. "Fast Pulsars, Strange Stars, and Strange Dwarfs†." Annals of the New York Academy of Sciences 759, no. 1 (September 1995): 303–7. http://dx.doi.org/10.1111/j.1749-6632.1995.tb17550.x.

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15

Menezes, Debora P., and Don B. Melrose. "Strange Star Equations of State Revisited." Publications of the Astronomical Society of Australia 22, no. 4 (2005): 292–97. http://dx.doi.org/10.1071/as05022.

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AbstractMotivated by recent suggestions that strange stars can be responsible for glitches and other observational features of pulsars, we review some possible equations of state and their implications for models of neutron, hybrid, and strange stars. We consider the MIT bag model and also strange matter in the colour–flavour locked phase. The central energy densities for strange stars are higher than the central densities of ordinary neutron stars. Strange stars are bound by the strong force and so can also rotate much faster than neutron stars. These results are only weakly dependent on the model used for the quark matter. If just one of the existing mass-to-radius ratio constraint is valid, most neutron stars equations of state are ruled out, but all the strange stars equations of state presented in this work remain consistent with the constraint.
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16

CHENG, K. S., Z. G. DAI, and T. LU. "STRANGE STARS AND RELATED ASTROPHYSICAL PHENOMENA." International Journal of Modern Physics D 07, no. 02 (April 1998): 139–76. http://dx.doi.org/10.1142/s0218271898000139.

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Some historical remarks concerning the strange stars are briefly discussed. The recent developments in physics and dynamical behavior of strange stars are reviewed. Especially, various observational effects in distinguishing strange stars from neutron stars and related interesting astrophysical phenomena are also discussed.
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17

BENVENUTO, O. G., M. I. KRIVORUCHENKO, and B. V. MARTEMYANOV. "POSSIBLE SIGNATURES OF THE CONVERSION OF A NEUTRON STAR TO A STRANGE STAR." International Journal of Modern Physics D 03, no. 03 (September 1994): 653–64. http://dx.doi.org/10.1142/s0218271894000794.

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The problem of the identification of strange stars is discussed. We suggest some characteristic signatures for the search for strange stars: a two-step mechanism for supernova explosions accompanied by the occurrence of strange stars and two neutrino bursts; microstructure analysis in the profile of pulsar emission; and unusual stability in the rotation of millisecond pulsars due to the absence of internal crust in strange stars. The cooling of strange stars is faster than the cooling of ordinary neutron stars, so low surface temperature of pulsars can indicate the existence of massive quark cores in observed pulsars. Low mass strange stars as bursters and/or X-ray sources have peculiar observable features: low luminosity and (for bursters) high recurrence rate, large duration of bursts, low ratio of energy emitted between two bursts and energy emitted during the burst.
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18

AQUILANO, ROBERTO O., LUIS P. NEIRA CERVILLERA, and HÉCTOR VUCETICH. "OSCILLATTONS AND STRANGE STARS." Modern Physics Letters A 10, no. 09 (March 21, 1995): 723–31. http://dx.doi.org/10.1142/s0217732395000776.

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19

Page, Dany, and Andrew Cumming. "Superbursts from Strange Stars." Astrophysical Journal 635, no. 2 (December 8, 2005): L157—L160. http://dx.doi.org/10.1086/499520.

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20

Alpar, M. Ali. "Comment on Strange Stars." Physical Review Letters 58, no. 20 (May 18, 1987): 2152. http://dx.doi.org/10.1103/physrevlett.58.2152.

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21

Gondek-Rosińska, D., P. Haensel, J. L. Zdunik, and E. Gourgoulhon. "Rapidly rotating strange stars." International Astronomical Union Colloquium 177 (2000): 661–62. http://dx.doi.org/10.1017/s0252921100060930.

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AbstractWe study effects of the strange quark mass,ms, and of the QCD interactions, calculated to lowest order inαc, on the rapid rotation of strange stars (SS). The influence of rotation on global parameters of SS is greater than in the case of the neutron stars (NS). We show that independently ofmsandαcthe ratio of the rotational kinetic energy to the absolute value of the gravitational potential energyT/Wfor a rotating SS is significantly higher than for an ordinary NS. This might indicate that rapidly rotating SS could be important sources of gravitational waves.
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22

Bethe, H. A., G. E. Brown, and J. Cooperstein. "Stars of strange matter?" Nuclear Physics A 462, no. 4 (February 1987): 791–802. http://dx.doi.org/10.1016/0375-9474(87)90577-x.

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23

RAZEIRA, MOISÉS, BARDO E. J. BODMANN, and CÉSAR A. ZEN VASCONCELLOS. "STRANGE MATTER AND STRANGE STARS WITH TSALLIS STATISTICS." International Journal of Modern Physics D 16, no. 02n03 (February 2007): 365–72. http://dx.doi.org/10.1142/s0218271807010134.

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We investigate the properties of β-equilibrated electrically charged neutral strange matter and strange stars at finite temperature in the framework of Tsallis statistics [C. Tsallis, J. Stat. Phys.52 (1988) 479]. As the main result of our study we find out that a QHD description of nuclear matter combined with Tsallis statistics may open new possibilities for nuclear matter models.
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24

Vartanyan, Yu L., A. R. Arutyunyan, and A. K. Grigoryan. "Strange quark matter and models of strange stars." Astrophysics 37, no. 3 (July 1994): 271–80. http://dx.doi.org/10.1007/bf02058783.

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25

XIA, ChengJun. "Strange quark matter: From strangelets to strange stars." SCIENTIA SINICA Physica, Mechanica & Astronomica 46, no. 1 (December 15, 2015): 012021. http://dx.doi.org/10.1360/sspma2015-00516.

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26

YILMAZ, İHSAN, and HÜSNÜ BAYSAL. "RIGIDLY ROTATING STRANGE QUARK STARS." International Journal of Modern Physics D 14, no. 03n04 (April 2005): 697–705. http://dx.doi.org/10.1142/s0218271805006158.

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In this article, we study rotating strange quark stars in the context of general relativity. For this purpose we consider perfect fluid model composed of strange quark matter with electromagnetic field in the Gödel Universe which has rigid rotation. We solve Einstein's field equations by using equation of state for strange quark matter. Also, we discuss the features of obtained solutions.
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27

Lugones, German, and Cesar Vasquez Flores. "Relativistic Cowling approximation for fluid oscillation modes of color superconducting self-bound stars." Proceedings of the International Astronomical Union 8, S291 (August 2012): 451. http://dx.doi.org/10.1017/s1743921312024477.

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AbstractThe investigation of the quasi-normal modes of oscillation of compact stars can reveal much information about their equation of state and internal structure mainly through the analysis of the expected emission of gravitational waves. In this work we study non-radial oscillation modes of strange stars consisting of color superconducting quark matter. We focus on the fundamental and pressure oscillation modes within the frame of the Cowling approximation. We discuss the observable features that may allow a differentiation among hadronic stars, strange stars, and strange stars with color superconductivity.
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28

Bejger, M., and P. Haensel. "Surface gravity of neutron stars and strange stars." Astronomy & Astrophysics 420, no. 3 (June 2004): 987–91. http://dx.doi.org/10.1051/0004-6361:20034538.

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29

Gurovich, Victor Ts, and Leonid G. Fel. "Converting neutron stars into strange stars: Instanton model." International Journal of Modern Physics D 23, no. 09 (August 2014): 1450078. http://dx.doi.org/10.1142/s0218271814500783.

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We calculate the quasiclassical probability to emerge the quantum fluctuation which gives rise to the quark-matter drop with interface propagating as the self-similar spherical detonation wave (DN) in the ambient nuclear matter. For this purpose, we make use of instanton method which is known in the quantum field theory.
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30

Xu, Renxin. "Solid Bare Strange Quark Stars." Symposium - International Astronomical Union 218 (2004): 299–302. http://dx.doi.org/10.1017/s0074180900181215.

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The reason we need the terms “strange”, “bare” and“solid” before quark stars is presented concisely, although some fundamental issues are not certain. Observations favoring these stars are introduced.
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31

Sedrakian, D. M., M. V. Hayrapetyan, and D. S. Baghdasaryan. "MAGNETIC FIELD OF STRANGE STARS." Proceedings of the YSU A: Physical and Mathematical Sciences 50, no. 3 (241) (October 26, 2016): 47–51. http://dx.doi.org/10.46991/pysu:a/2016.50.3.047.

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The generation of a magnetic field and its distribution inside a rotating strange star are discussed. The difference between the angular velocities of the superfluid and superconducting quark core and of the normal electron plasma increases because of spin-down of the star and this leads to the generation of a magnetic field. The magnetic field distribution in a star is found for a stationary value of difference of angular velocities of these components. In all parts of the star this field is determined entirely by the total magnetic momentMof the star which can vary from 1031-1034 G·cm3 for some models of compact stars. Also the maximum possible values of magnetic field on the surface of various models of strange dwarfs have been estimated. Depending on configuration parameters, mass M and radius R of the star, the limit of 103-105 G has been established. Such values of magnetic field may be an additional condition for identification of strange dwarfs among the large class of observed white dwarfs.
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32

Mannarelli, Massimo. "Torsional oscillations of strange stars." EPJ Web of Conferences 80 (2014): 00039. http://dx.doi.org/10.1051/epjconf/20148000039.

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33

Klähn, Thomas, and David B. Blaschke. "Strange matter in compact stars." EPJ Web of Conferences 171 (2018): 08001. http://dx.doi.org/10.1051/epjconf/201817108001.

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We discuss possible scenarios for the existence of strange matter in compact stars. The appearance of hyperons leads to a hyperon puzzle in ab-initio approaches based on effective baryon-baryon potentials but is not a severe problem in relativistic mean field models. In general, the puzzle can be resolved in a natural way if hadronic matter gets stiffened at supersaturation densities, an effect based on the quark Pauli quenching between hadrons. We explain the conflict between the necessity to implement dynamical chiral symmetry breaking into a model description and the conditions for the appearance of absolutely stable strange quark matter that require both, approximately masslessness of quarks and a mechanism of confinement. The role of strangeness in compact stars (hadronic or quark matter realizations) remains unsettled. It is not excluded that strangeness plays no role in compact stars at all. To answer the question whether the case of absolutely stable strange quark matter can be excluded on theoretical grounds requires an understanding of dense matter that we have not yet reached.
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34

Pierrehumbert, Raymond T. "Strange news from other stars." Nature Geoscience 6, no. 2 (January 31, 2013): 81–83. http://dx.doi.org/10.1038/ngeo1711.

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35

Haensel, P. "Strange Matter and Neutron Stars." Progress of Theoretical Physics Supplement 91 (May 16, 2013): 268–83. http://dx.doi.org/10.1143/ptp.91.268.

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36

Ray, Subharthi, Manjari Bagchi, Jishnu Dey, and Mira Dey. "Strange stars at finite temperature." Journal of Physics: Conference Series 31 (March 21, 2006): 107–10. http://dx.doi.org/10.1088/1742-6596/31/1/018.

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37

Zhou, Xia, Lingzhi Wang, and Aizhi Zhou. "Thermal Evolution of Strange Stars." Publications of the Astronomical Society of the Pacific 119, no. 862 (December 2007): 1367–70. http://dx.doi.org/10.1086/524711.

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38

Colpi, M., and J. C. Miller. "Rotational properties of strange stars." Astrophysical Journal 388 (April 1992): 513. http://dx.doi.org/10.1086/171170.

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39

Kapoor, R. C., and C. S. Shukre. "Are radio pulsars strange stars ?" Astronomy & Astrophysics 375, no. 2 (August 2001): 405–10. http://dx.doi.org/10.1051/0004-6361:20010891.

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40

Xu, R. X. "Low-mass bare strange stars." Advances in Space Research 37, no. 10 (January 2006): 1992–95. http://dx.doi.org/10.1016/j.asr.2005.10.025.

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41

Miller, John, and Monica Colpi. "Rotational properties of strange stars." Nuclear Physics B - Proceedings Supplements 24, no. 2 (December 1991): 166–69. http://dx.doi.org/10.1016/0920-5632(91)90319-a.

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42

PAUL, B. C., P. K. CHATTOPADHYAY, S. KARMAKAR, and R. TIKEKAR. "RELATIVISTIC STRANGE STARS WITH ANISOTROPY." Modern Physics Letters A 26, no. 08 (March 14, 2011): 575–87. http://dx.doi.org/10.1142/s0217732311034943.

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We study a compact star comprising strange matter content in the presence of pressure anisotropy. Considering strange matter with equation of state p = (ρ-4B)/3, where B is Bag parameter, we analyze the effect of pressure anisotropy on the Bag parameter for a compact star described by Vaidya–Tikekar metric. The values of B inside and on surface of the star are determined for different anisotropy parameter α. It is found that in the vicinity of the center of a compact star, B parameter is almost constant. However, away from the center B varies with the radial distance and finally at the surface B attains a value independent of the anisotropy. It is also noted that for some values of α, B remains constant throughout the star. Given α and spheriodicity a, B is found to be decreasing with the increase in compactness factor. The models admitting B increasing with α for a given spheriodicity parameter (a) and compactness are also found.
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43

Cheng, K. S., and Z. G. Dai. "Chemical Heating in Strange Stars." Astrophysical Journal 468 (September 1996): 819. http://dx.doi.org/10.1086/177737.

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44

Haensel, Paweł. "Strange Matter and Neutron Stars." Progress of Theoretical Physics Supplement 91 (1987): 268–83. http://dx.doi.org/10.1143/ptps.91.268.

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45

Xu, Ren-xin, and Guo-jun Qiao. "Electric Character of Strange Stars." Chinese Physics Letters 16, no. 10 (October 1, 1999): 778–80. http://dx.doi.org/10.1088/0256-307x/16/10/028.

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46

Vartanyan, Yu L. "Superdense stars containing strange baryons." Astrophysics 53, no. 1 (January 2010): 18–31. http://dx.doi.org/10.1007/s10511-010-9095-z.

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47

Hajyan, G. S., and A. G. Alaverdyan. "Hot Strange Stars. III. Stability." Astrophysics 58, no. 2 (June 2015): 289–95. http://dx.doi.org/10.1007/s10511-015-9383-8.

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48

Schertler, K., C. Greiner, and M. H. Thoma. "Medium effects in strange quark matter and strange stars." Nuclear Physics A 616, no. 3-4 (April 1997): 659–79. http://dx.doi.org/10.1016/s0375-9474(97)00014-6.

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49

Glatzel, Wolfgang. "Linear Strange Modes in Massive Stars." International Astronomical Union Colloquium 169 (1999): 345–52. http://dx.doi.org/10.1017/s0252921100072225.

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AbstractThe occurrence and properties of strange modes and associated instabilities in massive stars are reviewed. If applicable, strange modes may be classified by the maximum of the opacity they are associated with. Whether they are still present in the limit of vanishing or infinite thermal timescales – which corresponds to the NAR and adiabatic approximations respectively – is another criterion for classification. A model for the instability mechanism of strange mode instabilities is discussed.
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50

WEBER, F., O. HAMIL, K. MIMURA, and R. NEGREIROS. "FROM CRUST TO CORE: A BRIEF REVIEW OF QUARK MATTER IN NEUTRON STARS." International Journal of Modern Physics D 19, no. 08n10 (August 2010): 1427–36. http://dx.doi.org/10.1142/s0218271810017329.

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This paper provides a short overview of the multifaceted, possible role of quark matter for compact stars (neutron stars and strange quark matter stars). We began with a variational investigation of the maximum possible energy densities in the cores of neutron stars. This is followed by a brief discussion of the possible existence of quark matter in the cores of neutron stars and how such matter could manifest itself in neutron star observables. The possible presence of color superconducting strange quark matter nuggets in the crusts of neutron stars is reviewed next, and their impact on the pycnonuclear reaction rates in the crusts of neutron stars is discussed. The second part of the paper discusses the impact of ultra-strong electric fields on the bulk properties of strange quark matter stars and presents results of a preliminary study that models the thermal evolution of radio-quiet, X-ray bright, central compact objects (CCOs).
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