Wind Braking of Magnetars

Tong, H.; Xu, R. X.; Song, Liming; Qiao, G. J.

doi:10.1088/0004-637x/768/2/144

Cited by 68 publications

(92 citation statements)

References 70 publications

(157 reference statements)

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“…Observationally, two magnetars 4U 0142+61 and 1E 2259+586 may have fallback disks (Wang et al 2006;Kaplan et al 2009). Timing observations of these two magnetars showed that their surface dipole field are both around or smaller than 10 14 G, depending on the assumed braking mechanism (Tong et al 2013;Olausen & Kaspi 2014). The two observed magnetar/fallback disk systems are consistent with the calculations here 6 .…”

Section: Calculations For Typical Magnetar Parameterssupporting

confidence: 85%

Rotational Evolution of Magnetars in the Presence of a Fallback Disk

Tong¹,

Wang²,

Liu³

et al. 2016

ApJ

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Magnetars may have strong surface dipole field. Observationally, two magnetars may have passive fallback disks. In the presence of a fallback disk, the rotational evolution of magnetars may be changed. In the self-similar fallback disk model, it is found that: (1) When the disk mass is significantly smaller than 10 −6 M ⊙ , the magnetar is unaffected by the fallback disk and it will be a normal magnetar. (2) When the disk mass is large, but the magnetar's surface dipole field is about or below 10 14 G, the magnetar will also be a normal magnetar. A magnetar plus a passive fallback disk system is expected. This may correspond to the observations of magnetars 4U 0142+61, and 1E 2259+586. (3) When the disk mass is large, and the magnetar's surface dipole field is as high as 4 × 10 15 G, the magnetar will evolve from the ejector phase to the propeller phase, and then enter rotational equilibrium. The magnetar will be slowed down quickly in the propeller phase. The final rotational period can be as high 2 × 10 4 s. This may correspond to the super-slow magnetar in the supernova remnant RCW 103. Therefore, the three kinds of magnetars can be understood in a unified way.

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Section: Calculations For Typical Magnetar Parameterssupporting

confidence: 85%

Rotational Evolution of Magnetars in the Presence of a Fallback Disk

Tong¹,

Wang²,

Liu³

et al. 2016

ApJ

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“…The ray-tracing discussed in Section 2 can be used for rays passing through a pulsar wind, introducing relativistic and plasma effects into models of binary eclipses for a double NS or NS-black hole binary that is nearly edge on with respect to the observer. In the case of an aligned rotator we expect a wind density proportional to 1/r, such that h = 1 (Contopoulos, Kazanas & Fendt 1999;Harding, Contopoulos & Kazanas 1999;Kirk, Lyubarsky & Petri 2009;Tong, Xu, Song & Qiao 2013), shown in Fig. 2.…”

Section: Discussionmentioning

confidence: 97%

Frequency-dependent effects of gravitational lensing within plasma

Rogers

2015

Monthly Notices of the Royal Astronomical Society

131

120

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The interaction between refraction from a distribution of inhomogeneous plasma and gravitational lensing introduces novel effects to the paths of light rays passing by a massive object. The plasma contributes additional terms to the equations of motion, and the resulting ray trajectories are frequency-dependent. Lensing phenomena and circular orbits are investigated for plasma density distributions N ∝ 1/r h with h ≥ 0 in the Schwarzschild space-time. For rays passing by the mass near the plasma frequency refractive effects can dominate, effectively turning the gravitational lens into a mirror. We obtain the turning points, circular orbit radii, and angular momentum for general h. Previous results have shown that light rays behave like massive particles with an effective mass given by the plasma frequency for a constant density h = 0. We study the behaviour for general h and show that when h = 2 the plasma term acts like an additional contribution to the angular momentum of the passing ray. When h = 3 the potential and radii of circular orbits are analogous to those found in studies of massless scalar fields on the Schwarzschild background. As a physically motivated example we study the pulse profiles of a compact object with antipodal hotspots sheathed in a dense plasma, which shows dramatic frequency-dependent shifts from the behaviour in vacuum. Finally, we consider the potential observability and applications of such frequency-dependent plasma effects in general relativity for several types of neutron star.

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“…A physical spin down mechanism must be based on the existence of a magnetosphere [25]. One candidate at present is the wind braking model [80,93].…”

Section: Introductionmentioning

confidence: 99%

Pulsar braking: magnetodipole vs. wind

Tong

2015

Sci. China Phys. Mech. Astron.

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Pulsars are good clocks in the universe. One fundamental question is that why they are good clocks? This is related to the braking mechanism of pulsars. Nowadays pulsar timing is done with unprecedented accuracy. More pulsars have braking indices measured. The period derivative of intermittent pulsars and magnetars can vary by a factor of several. However, during pulsar studies, the magnetic dipole braking in vacuum is still often assumed. It is shown that the fundamental assumption of magnetic dipole braking (vacuum condition) does not exist and it is not consistent with the observations. The physical torque must consider the presence of the pulsar magnetosphere. Among various efforts, the wind braking model can explain many observations of pulsars and magnetars in a unified way. It is also consistent with the up-to-date observations. It is time for a paradigm shift in pulsar studies: from magnetic dipole braking to wind braking. As one alternative to the magnetospheric model, the fallback disk model is also discussed. Tong H. Pulsar braking: magnetodipole vs. wind.

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Wind Braking of Magnetars

Cited by 68 publications

References 70 publications

Rotational Evolution of Magnetars in the Presence of a Fallback Disk

Rotational Evolution of Magnetars in the Presence of a Fallback Disk

Frequency-dependent effects of gravitational lensing within plasma

Pulsar braking: magnetodipole vs. wind

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