Compressed baryonic matter: from nuclei to pulsars

Xu, R. X.

doi:10.1360/132013-347

Cited by 6 publications

(6 citation statements)

References 28 publications

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“…Traditionally speaking, quarks are confined in hadrons of neutron stars, while a quark star is composed of de-confined quarks. While a solid quark star is a condensed object of quark clusters, which distinguishes from conventional both neutron and quark stars (Xu 2003(Xu , 2010(Xu , 2013. The solid quark star (i.e.…”

Section: Introductionmentioning

confidence: 99%

Two types of glitches in a solid quark star model

Zhou

Tong

et al. 2014

Monthly Notices of the Royal Astronomical Society

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Glitch (sudden spinup) is a common phenomenon in pulsar observations. However, the physical mechanism of glitch is still a matter of debate because it depends on the puzzle of pulsar's inner structure, i.e., the equation of state of dense matter. Some pulsars (e.g., Vela-like) show large glitches (∆ν/ν ∼ 10 −6 ) but release negligible energy, whereas the large glitches of AXPs/SGRs (anomalous X-ray pulsars/soft gamma repeaters) are usually (but not always) accompanied with detectable energy releases manifesting as X-ray bursts or outbursts. We try to understand this aspect of glitches in a starquake model of solid quark stars. There are two kinds of glitches in this scenario: bulk-invariable (Type I) and bulk-variable (Type II) ones. The total stellar volume changes (and then energy releases) significantly for the latter but not for the former. Therefore, glitches accompanied with X-ray bursts (e.g., that of AXP/SGRs) could originate from Type II starquakes induced probably by accretion, while the others without evident energy release (e.g., that of Vela pulsar) would be the result of Type I starquakes due to, simply, a change of stellar ellipticity.

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Section: Introductionmentioning

confidence: 99%

Two types of glitches in a solid quark star model

Zhou

Tong

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…及时发现磁星的爆发并开展相关的多波段观测, 获得充分的观测数据是解决这些重要问题的关键. 尽管流行观点认为磁星是表面磁场极强的中子星, 但也有学者认为它们可能是固态奇异星 [8] , 这跟人们至今尚不能明确几倍核物质密度下冷物质的性质有关(如文献 [9]). 另外也有学者认为磁星可以是大质量、强磁场的白矮星, 辐射和普通射电脉冲星的自转驱动机制相同 [10] .…”

Section: 但其中的物理机制并不清楚比如是磁星的磁场结unclassified

Detecting magnetars with Einstein Probe

Wang

et al. 2017

Sci. Sin.-Phys. Mech. Astron.

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“…In this sub-section, we discuss the solid quark star model for AXPs/SGRs (Xu 2003(Xu , 2013. Within this model, no strong magnetic field is needed to power outbursts.…”

Section: Solid Quark Star Modelmentioning

confidence: 99%

“…The standard model is that they are neutron stars with superstrong magnetic fields, known as magnetars (Thompson & Duncan 1995. Alternatively, a solid quark star model was suggested by Xu (2003Xu ( , 2013. In the following, we discuss the radio activation mechanism within the framework of both models.…”

Section: Axps/sgrsmentioning

confidence: 99%

Oscillation-Driven Magnetospheric Activity in Pulsars

Lin

Zhang

2015

ApJ

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We study the magnetospheric activity in the polar cap region of pulsars under stellar oscillations. The toroidal oscillation of the star propagates into the magnetosphere, which provides additional voltage due to unipolar induction, changes Goldreich-Julian charge density from the traditional value due to rotation, and hence, influences particle acceleration. We present a general solution of the effect of oscillations within the framework of the inner vacuum gap model, and consider three different inner gap modes controlled by curvature radiation, inverse Compton scattering, and two photon annihilation, respectively. With different pulsar parameters and oscillation amplitudes, one of three modes would play a dominant role in defining the gap properties. When the amplitude of oscillation exceeds a critical value, mode changing would occur. Oscillations also lead to change of the size of the polar cap. As applications, we show the inner gap properties under oscillations in both normal pulsars and anomalous X-ray pulsars / soft gamma-ray repeaters (AXPs/SGRs). We interpret the onset of radio emission after glitches/flares in AXPs/SGRs as due to oscilation-driven magnetic activities in these objects, within the framework of both the magnetar model and the solid quark star model. Within the magnetar model, radio activation may be caused by the enlargement of the effective polar cap angle and the radio emission beam due to oscillation; whereas within the solid quark star angle, it may be caused by activation of the pulsar inner gap from below the radio emission death line due to an oscillation-induced voltage enhancement. The model can also explain the glitch-induced radio profile change observed in PSR J1119-6127.

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Compressed baryonic matter: from nuclei to pulsars

Cited by 6 publications

References 28 publications

Two types of glitches in a solid quark star model

Two types of glitches in a solid quark star model

Detecting magnetars with Einstein Probe

Oscillation-Driven Magnetospheric Activity in Pulsars

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