摘要：
In a second-order r-mode theory, Sa and Tom6 found that the r-mode oscil-lation in neutron stars (NSs) could induce stellar differential rotation, which naturally leads to a saturated state of the oscillation. Based on a consideration of the coupling of the r-modes and the stellar spin and thermal evolution, we carefully investigate the in-fluences of the differential rotation on the long-term evolution of isolated NSs and NSs in low-mass X-ray binaries, where the viscous damping of the r-modes and its resultant effects are taken into account. The numerical results show that, for both kinds of NSs, the differential rotation can significantly prolong the duration of the r-modes. As a result, the stars can keep nearly a constant temperature and constant angular velocity for over a thousand years. Moreover, the persistent radiation of a quasi-monochromatic gravitational wave would also be predicted due to the long-term steady r-mode oscillation and stellar rotation. This increases the detectability of gravitational waves from both young isolated and old accreting NSs.
作者机构：
[Yu, Y. W.; Dai, Z. G.] Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China.;[Yu, Y. W.; Zheng, X. P.] Huazhong Normal Univ, Inst Astrophys, Wuhan 430079, Peoples R China.
通讯机构：
[Yu, Y. W.] N;Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China.
关键词：
elementary particles;gamma-rays: bursts
摘要：
The observations of a nearby low-luminosity gamma-ray burst (GRB) 060218 associated with supernova SN 2006aj may imply an interesting astronomical picture where a supernova shock breakout locates behind a relativistic GRB jet. Based on this picture, we study neutrino emission for early afterglows of GRB 060218-like GRBs, where neutrinos are expected to be produced from photopion interactions in a GRB blast wave that propagates into a dense wind. Relativistic protons for the interactions are accelerated by an external shock, while target photons are basically provided by the incoming thermal emission from the shock breakout and its inverse-Compton scattered component. Because of a high estimated event rate of low-luminosity GRBs, we would have more opportunities to detect afterglow neutrinos from a single nearby GRB event of this type by IceCube. Such a possible detection could provide evidence for the picture described above.
作者：
Liu Xue-wen;Kang Miao;Yu Yun-wei（俞云伟）;Zhou Xia;Zheng Xiao-ping
期刊：
Chinese Astronomy and Astrophysics,2007年31(1):1-10 ISSN：0275-1062
通讯作者：
Xue-wen, L.
作者机构：
[Xue-wen L.] Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing, 210008, China;[Xiao-ping Z.; Miao K.; Xia Z.; Yun-wei Y.] Institute of Astrophysics, Huazhong Normal University, Wuhan, 430079, China
通讯机构：
[Xue-wen, L.] P;Purple Mountain Observatory, Chinese Academy of Sciences, China
关键词：
dense matter;magnetic field;neutrino;nuclear reaction;star: neutron star
作者：
Wang, W. L.*;Huang, F.;Zhang, Z. Y.;Yu, Y. W.（俞云伟）;Liu, F.
期刊：
JOURNAL OF PHYSICS G-NUCLEAR AND PARTICLE PHYSICS,2007年34(7):1771-1782 ISSN：0954-3899
通讯作者：
Wang, W. L.
作者机构：
[Wang, W. L.] Huazhong Normal Univ, Inst Particle Phys, Wuhan 430070, Peoples R China.;CCAST World Lab, Beijing 100080, Peoples R China.;Inst High Energy Phys, Beijing 100049, Peoples R China.
通讯机构：
[Wang, W. L.] H;Huazhong Normal Univ, Inst Particle Phys, Wuhan 430070, Peoples R China.
摘要：
The energies of the low- lying isoscalar and isovector udss configurations with spin-parity J(P) = 0(+), 1(+) and 2(+) are calculated in a non-relativistic constituent quark model by using the variational method. The contributions of various parts of the quark-quark interacting potentials including the s-channel interaction are investigated, and the effect of different forms of the confinement potential is examined. The model parameters are determined by the same method as in our previous work, and they still can satisfactorily describe the nucleon-nucleon scattering phase shifts and the hyperon-nucleon cross sections. The parameters of the s- channel interaction are fixed by the masses of K and K* mesons, for which the size parameter is taken to be two possible values. When it is chosen to be the same as baryons', the numerical results show that the masses of all the udss configurations are higher than the corresponding meson-meson thresholds. But when the size parameter for the K and K* mesons is adjusted to be smaller than that for the baryons, the udss configuration with I = 0 and J(P) = 1(+) is found to lie lower than the K* K* threshold, furthermore, this state has a very small KK* component and the interaction matrix elements between this state and KK* is comparatively small, thus its coupling to the KK* channel will consequently be weak and it might be regarded as a possible tetraquark candidate.
作者机构：
CCAST, World Lab, Beijing 100080, Peoples R China.;Huazhong Normal Univ, Inst Particle Phys, Wuhan 430079, Peoples R China.;Inst High Energy Phys, Beijing 100049, Peoples R China.;[Huang, F.] CCAST, World Lab, POB 8730, Beijing 100080, Peoples R China.
通讯机构：
[Huang, F.] C;CCAST, World Lab, POB 8730, Beijing 100080, Peoples R China.
摘要：
A preliminary investigation of K¯N interaction is performed within a chiral constituent quark model by solving the resonating group method (RGM) equation. The model parameters are taken from our previous work, which gave a satisfactory description of the S-, P-, D-, F-wave KN scattering phase shifts. The channel-coupling between K¯N,πΛ and πΣ is considered, and the scattering phase shifts as well as the bound-state problem of K¯N are dynamically studied. The results show that the S-wave K¯N interaction in the isospin I=0 channel is attractive, and in the extended chiral SU(3) quark model such an attraction can make for a K¯N bound state, which appears as a πΣ resonance in the coupled-channel calculation, while the chiral SU(3) quark model cannot accommodate the existence of a K¯N bound state. It seems that the vector meson exchanges are necessary to be introduced in the quark-quark interactions if one tries to explain the Λ(1405) as a K¯N bound state or a πΣ- K¯N resonance state.
作者：
Wang, W. L.*;Huang, F.;Zhang, Z. Y.;Yu, Y. W.（俞云伟）;Liu, F.
期刊：
EUROPEAN PHYSICAL JOURNAL A,2007年32(3):293-297 ISSN：1434-6001
通讯作者：
Wang, W. L.
作者机构：
[Wang, W. L.] Huazhong Normal Univ, Inst Particle Phys, Wuhan 430070, Peoples R China.;CCAST, World Lab, Beijing 100080, Peoples R China.;Inst High Energy Phys, Beijing 100039, Peoples R China.
通讯机构：
[Wang, W. L.] H;Huazhong Normal Univ, Inst Particle Phys, Wuhan 430070, Peoples R China.
摘要：
We studied the evolution of isolated strange stars (SSs) synthetically, considering the influence of r-mode instability. Our results show that the cooling of SSs with non-ultrastrong magnetic fields is delayed by heating due to r-mode damping for millions of years, while the spin-down of the stars is dominated by gravitational radiation (GR). Especially for the SSs in a possible existing colour–flavour locked (CFL) phase, the effect of r-mode instability on the evolution of stars becomes extremely important because the viscosity, neutrino emissivity and specific heat involving pairing quarks are blocked. It leads to the cooling of these colour superconducting stars being very slow and the stars can remain at high temperature for millions of years, which differs completely from previous understanding. In this case, an SS in CFL phase can be located at the bottom of its r-mode instability window for a long time, but does not spin-down to a very low frequency for hours.
期刊：
Monthly Notices of the Royal Astronomical Society,2006年371(4):1659-1662 ISSN：0035-8711
通讯作者：
Zheng, Xiaoping
作者机构：
[Yu, Yunwei; Zheng, Xiaoping; Zhou, Xia; Zheng, XP] Huazhong Normal Univ, Inst Astrophys, Wuhan 430079, Peoples R China.
通讯机构：
[Zheng, Xiaoping] H;Huazhong Normal Univ, Inst Astrophys, Wuhan 430079, Peoples R China.
关键词：
dense matter;stars: evolution;stars: neutron;pulsars: general
摘要：
Under the combination effect of recommencement heating due to the spin-down of strange stars (SSs) and heat preservation due to the weak conduction heat of the crust, Cooper pair breaking and formation (PBF) in colour superconducting quark matter arises. We investigate the cooling of SSs with a crust in the colour superconductivity phase including both deconfinement heating (DH) and the PBF process. We find that DH can delay the thermal evolution of SSs and the PBF process suppresses the early temperature rise of the stars. The cooling SSs behave within the brightness constraint of young compact objects when the colour superconductivity gap is small enough.
