Oscillation-Driven Magnetospheric Activity in Pulsars

Lin, Meng-Xiang; Xu, R. X.; Zhang, Bing

doi:10.1088/0004-637x/799/2/152

Cited by 27 publications

(25 citation statements)

References 38 publications

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“…After the outburst, when the magnetar return back to the quiescent state, it will become radio-quiet again (Ref. [17] obtained a similar conclusion using a different model for magnetars). The final radio disappearance of these two radio-loud magnetars [9,15] are consistent with the general expectations in the wind braking model.…”

Section: Decreasing Torque During Outburstsmentioning

confidence: 69%

Understanding Recent Magnetar Observations from the Magnetospheric Point of View

Tong

2018

Proceedings of the Workshop on Quarks and Compact Stars 2017 (QCS2017)

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The wind braking model and its applications to magnetars are discussed. The decreasing torque of magnetars during outbursts, anti-glitch, and anti-correlations between radiation and timing are understandable in the wind braking model. Recent timing observations of magnetars are also consistent with the previous modeling. A magnetism-powered wind nebula and a braking index smaller than three are the two predictions. Besides isolated magnetars, there may also be accreting magnetars in binary systems and magnetars accreting from fallback disks. Observationally, ultra-luminous X-ray pulsars may be accreting magnetars, while super-slow magnetars may be magnetars with fallback disks in the past. Many works are needed for both isolated magnetars and accreting magnetars.

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Section: Decreasing Torque During Outburstsmentioning

confidence: 69%

Understanding Recent Magnetar Observations from the Magnetospheric Point of View

Tong

2018

Proceedings of the Workshop on Quarks and Compact Stars 2017 (QCS2017)

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“…It is reasonable that electromagnetic [17,19] non-atomic X-rays Plankian radiation of X-ray very thin atmosphere above surface [10,11] absorption in thermal spectra hydromagnetic oscillation of e − sea [23] strangeness barrier low-z emission, type-I XRB 2-flavored matter separated from 3-f [9] optical/UV excess of XDINS bremsstrahlung radiation [10] global stiff EoS high M max (2 ∼ 3M ⊙ ) non-relativistic strangeon, hard core [3,4,24,25] anisotropic pressure SGR/AXPs burst and flare quake-induced energy release [20,26,27] rigidity precession, GW radiation solid, mountain building [2,28] matter should be separated sharply from strong matter. Bare surface of strangeon star could help in understanding the non-atomic spectra of XDINSs [11].…”

Section: Strangeon Star Identificationmentioning

confidence: 99%

Strangeon Stars

Lu¹,

Xu²

2018

Proceedings of the Workshop on Quarks and Compact Stars 2017 (QCS2017)

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Stable micro-nucleus is 2-flavored (u and d), whereas stable macro-nucleus could be 3-flavored (u, d and s) if the light flavor symmetry restores there. Nucleons are the constituent of a nucleus, while strangeons are named as the constituent of 3-flavored baryonic matter. Gravity-compressed baryonic object created after core-collapse supernova could be strangeon star if the energy scale (∼ 0.5 GeV) cannot be high enough for quark deconfinement and if there occurs 3-flavor symmetry restoration. Strangeon stars are explained here, including their formation and manifestation/identification. Much work, coupled with effective micro-model of strangeon matter, is needed to take advantage of the unique opportunities advanced facilities will provide. KEYWORDS: pulsar: general, dense matter, equation of stateAlthough the state equation of dense matter around nuclear density is a great challenge for physicists, it is usually a thought that strangeness could be relevant to the solution. As noted in the QC-S2014 proceedings [1], such kind of strange matter is conjectured to be strangeon matter, being manifested in the form of compact stars, cosmic rays, and even dark matter. In this contribution, we are focusing on strangeon star, which is a key ingredient of strangeon matter in astrophysics.It is half a century since the first pulsar was discovered, but the real nature of pulsar remains one of the most puzzling problems both in physics and in astronomy. Pulsars are always thought to be neutron stars, but the issue of their real structure is still controversial. Different observations (e.g., the spin period, the measurements of mass and radius) show that the typical density of pulsar-like compact stars could be only a few nuclear density, and the separation between quarks is ∼ 0.5 fm and hence the energy scale is order of ∼ 0.5 GeV according to Heisenberg's uncertainty relation. The pulsar structure is then a problem of non-perturbative QCD (quantum chromo-dynamics), an unsolved issue for fundamental strong interaction at low energy regime ( 1 GeV). Similar to the issue of turbulence, the strong interaction physics at low-energy is still challenging though QCD is mathematically well-defined. In fact, both of "Navier-Stokes Equation" and "Yang-Mills and Mass Gap" are prize problems named by the Clay Mathematical Institute. Hitherto now, no one can derive pulsar structure from ab-initio calculations, nonetheless astrophysicists could speculate phenomenologically.In Fig. 1, we summarize pulsar inner structures (i.e., models) speculators suggest. All of the pulsar structure models fell into four categories: hadron star, quark star, hybrid/mixed star and strangeon star, as are shown in Fig. 1. In the hadron star model, quarks are confined in hadrons, and the hadron liquid is the dominated part of the star. Hadron stars are bounded by gravity, and they must have crusts composed of ions and electrons. A hadron star is called a neutron star if only the nucleon (proton and neutron) degree of freedom is introduced. Conversely, a quark...

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“…When the oscillation amplitude K is small, the star is under the death line and thus radio quiet; after K exceeds a critical value, the star would be activated above the death line, and thus could be ratio loud. Table 1 in Lin et al [7] shows such critical values for all detected radio AXP/SGRs.…”

Section: In Solid Quark Star Modelmentioning

confidence: 99%

“…Lin et al [7] systematically studied the stellar oscillations' effect on magnetospheric activity within the framework of inner gap model [8] , and applied this physical model to explain the radio behaviors of AXP/SGRs and glitch-induced radio profile change of PSR J1119-6127. In this letter, based on Lin et al [7] , we mainly focus on the work about radio behaviors of AXP/SGRs and give a brief summary to it.…”

Section: Introductionmentioning

confidence: 99%

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Preface: The 8th International Symposium on Measurement Techniques for Multiphase Flows

Li¹

2014

AIP Conference Proceedings

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We suggest stellar oscillations are responsible for the strange radio behaviors of Anomalous X-ray pulsars and soft Gamma-ray repeaters (AXP/SGRs), within the framework of both solid quark star model and magnetar model. In solid quark star model, the extra voltage provided by oscillations activates the star from under death line to above death line. In magnetar model, oscillations enlarge the radio beam so that increase the possibility to detect it. Later radio emission decays and vanishes as oscillations damp.

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Oscillation-Driven Magnetospheric Activity in Pulsars

Cited by 27 publications

References 38 publications

Understanding Recent Magnetar Observations from the Magnetospheric Point of View

Understanding Recent Magnetar Observations from the Magnetospheric Point of View

Strangeon Stars

Preface: The 8th International Symposium on Measurement Techniques for Multiphase Flows

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