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Volumn 69, Issue 8, 2004, Pages 10-

Restricting quark matter models by gravitational wave observation

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EID: 2442702841     PISSN: 15507998     EISSN: 15502368     Source Type: Journal    
DOI: 10.1103/PhysRevD.69.084008     Document Type: Article
Times cited : (132)

References (63)
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    • Drake et al. 33 got a 99% confidence upper limit of 2.7% on the unaccelerated pulse fraction from (Formula presented) to 100 Hz. Most recently Burwitz et al. reported that a subsequent observation of RX J1856.5-3754 with XMM-Newton allows the upper limit on the periodic variation in the x-ray region to be reduced to 1.3% at 99% C.L. from (Formula presented) to 50 Hz 39
    • Drake et al. 33 got a 99% confidence upper limit of 2.7% on the unaccelerated pulse fraction from (Formula presented) to 100 Hz. Most recently Burwitz et al. reported that a subsequent observation of RX J1856.5-3754 with XMM-Newton allows the upper limit on the periodic variation in the x-ray region to be reduced to 1.3% at 99% C.L. from (Formula presented) to 50 Hz 39.
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    • Particle Data Group, K. Hagiwara, Phys. Rev. D 66, 010001 (2002).
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    • For an ordinary class of neutron stars whose compactness is large, the damping rate of some of relatively lower w modes is certainly smaller than that of (Formula presented) modes 7. Thus, only about the detection of them, the w modes would be more significant than the (Formula presented) modes in this class of neutron stars. For the models of the quark star adopted in this work, however, all damping rates of w modes are larger than that of the lowest (Formula presented) mode, because the compactness is smaller than that of such neutron stars 44. This tendency is discussed and clearly stated in Ref. 44. Therefore, we investigate the parameter dependence of the (Formula presented) modes for our current purposes
    • For an ordinary class of neutron stars whose compactness is large, the damping rate of some of relatively lower w modes is certainly smaller than that of (Formula presented) modes 7. Thus, only about the detection of them, the w modes would be more significant than the (Formula presented) modes in this class of neutron stars. For the models of the quark star adopted in this work, however, all damping rates of w modes are larger than that of the lowest (Formula presented) mode, because the compactness is smaller than that of such neutron stars 44. This tendency is discussed and clearly stated in Ref. 44. Therefore, we investigate the parameter dependence of the (Formula presented) modes for our current purposes.


* 이 정보는 Elsevier사의 SCOPUS DB에서 KISTI가 분석하여 추출한 것입니다.