منابع مشابه
Eos of Dense Matter and Fast Rotation of Neutron Stars
Neutron stars with their very strong gravity can be very fast rotators. Theoretical studies show that they could rotate at sub-millisecond periods, i.e., at frequency f = 1/period >1000 Hz. The first millisecond pulsar B1937+21, rotating at f = 641 Hz, remained the most rapid one during 24 years after its detection. In January 2006, discovery of a more rapid pulsar J1748-2446ad rotating at f = ...
متن کاملThe X-ray luminosity of rotation-powered neutron stars
As a result of recent observations with ROSAT and ASCA the number of rotation-powered pulsars seen at X-ray energies has increased substantially. In this paper we review the phenomenology of the observed X-ray emission properties. At present 27 pulsars are detected, representing a wide range of ages (103 − 7 × 109 yrs), magnetic field strength (108 − 1013 G) and spin periods (1.6 − 530 ms). Des...
متن کاملGravitational Radiation and Rotation of Accreting Neutron Stars
Recent discoveries by the Rossi X-Ray Timing Explorer indicate that most of the rapidly accreting (Ṁ ∼> 10 M⊙ yr ) weakly magnetic (B ≪ 10 G) neutron stars in the Galaxy are rotating at spin frequencies νs ∼> 250 Hz. Remarkably, they all rotate in a narrow range of frequencies (no more than a factor of two, with many within 20% of 300 Hz). I suggest that these stars rotate fast enough so that, ...
متن کاملMaximum Redshift and Minimum Rotation Period of Neutron Stars
The lower bound on the period of uniform rotation of neutron stars (NS) with causal equation of state (EOS), Pmin, is shown to be determined, with a high precision, by the upper bound on the surface redshift of static neutron star models, zmax. We obtain zmax = 0.851, which turns out to be about 5% lower than upper bound obtained by Lindblom (1984). Using then the empirical formula for the maxi...
متن کاملSpin and Isospin Asymmetry, Equation of State and Neutron Stars
In the present work, we have obtained the equation of state for neutron star matter considering the in uence of the ferromagnetic and antiferromagnetic spin state. We have also investigated the structure of neutron stars. According to our results, the spin asymmetry stiens the equation of state and leads to high mass for the neutron star.
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ژورنال
عنوان ژورنال: The Astrophysical Journal
سال: 1996
ISSN: 0004-637X,1538-4357
DOI: 10.1086/176650