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Volumn 280, Issue 5362, 1998, Pages 407-409

Is GRO J1744-28 a strange star?

Author keywords

[No Author keywords available]

Indexed keywords

ARTICLE; ASTRONOMY; MAGNETIC FIELD; PRIORITY JOURNAL; X RAY;

EID: 0032540425     PISSN: 00368075     EISSN: None     Source Type: Journal    
DOI: 10.1126/science.280.5362.407     Document Type: Article
Times cited : (70)

References (43)
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    • X-ray bursts are sudden increases in the x-ray flux of x-ray sources, with rise times of ≤1 s, and subsequent decay with characteristic times ranging from 10 s to a few minutes. They are classified as type I or type II. Type I x-ray bursts are characterized by the relatively long burst intervals (hours to days) and the significant spectral softening during the burst decay relative to their type II counterparts. The differences between type I (and type II) bursts and the HXRBs are discussed by W. H. G. Lewin, R. E. Rutledge, J. M. Kommers, J. van Paradijs, C. Kouveliotou, Astrophys. J. 462, L39 (1996).
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    • Pure hadronic matter can exist inside compact stars, for example, neutron stars in which most stellar masses are in the form of free protons and neutrons. In conditions of extremely high density, the smaller constituents (quarks) inside the protons and neutrons are no longer confined and a new phase of matter (that is, quark matter) can occur. For discussions of the possibility of such a phase of matter in compact stars, see A. R. Bodmer, Phys. Rev. D 4, 1601 (1971); E. Witten, ibid. 30, 272 (1984).
    • (1971) Phys. Rev. D , vol.4 , pp. 1601
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    • Pure hadronic matter can exist inside compact stars, for example, neutron stars in which most stellar masses are in the form of free protons and neutrons. In conditions of extremely high density, the smaller constituents (quarks) inside the protons and neutrons are no longer confined and a new phase of matter (that is, quark matter) can occur. For discussions of the possibility of such a phase of matter in compact stars, see A. R. Bodmer, Phys. Rev. D 4, 1601 (1971); E. Witten, ibid. 30, 272 (1984).
    • (1984) Phys. Rev. D , vol.30 , pp. 272
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  • 42


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