Pulsar Wind Model for the Spin-Down Behavior of Intermittent Pulsars

Li, L.; Tong, H.; Yan, W. M.; Yuan, Jianping; Xu, R. X.; Wang, Na

doi:10.1088/0004-637x/788/1/16

Cited by 21 publications

(34 citation statements)

References 37 publications

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“…The angular factor cos 2 α appears by considering that the parallel component is mainly responsible for the particle acceleration. It is possible that the factor cos 2 α does not appear [44]. However, the difference is only quantitative.…”

Section: Wind Braking Of Pulsarsmentioning

confidence: 99%

“…This means that there may be some additional particle outflows during the on state. This particle outflow is responsible for both the radiation of radio emissions and larger spin down rate (because these outflowing particles will take away additional angular momentum of the central neutron star [44] Up to the end of 2014, three intermittent pulsars are reported [13,38,51]. The latter two intermittent pulsars can be in the off state for about one year.…”

Section: Spin Down Of Intermittent Pulsarsmentioning

confidence: 99%

“…Equation (33) is obtained by assuming that the particle density equals the Goldreich-Julian charge density and the effect of pulsar death is not considered. 12 Ω −15/7 cos 2 α [44]. The corresponding expression can be obtained for each acceleration model.…”

Section: Wind Braking Of Pulsarsmentioning

confidence: 99%

“…The magnetic dipole braking may be employed to model the spin down during the off state. Then the ratio of spin down rate between the on and off state is [44]:…”

Section: Wind Braking Of Pulsarsmentioning

confidence: 99%

“…Only in special sources, e.g. intermittent pulsars, the first order effect of particle wind can be seen [44].…”

Section: Wind Braking Of Magnetarsmentioning

confidence: 99%

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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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Section: Wind Braking Of Pulsarsmentioning

confidence: 99%

Section: Spin Down Of Intermittent Pulsarsmentioning

confidence: 99%

Section: Wind Braking Of Pulsarsmentioning

confidence: 99%

“…The magnetic dipole braking may be employed to model the spin down during the off state. Then the ratio of spin down rate between the on and off state is [44]:…”

Section: Wind Braking Of Pulsarsmentioning

confidence: 99%

“…Only in special sources, e.g. intermittent pulsars, the first order effect of particle wind can be seen [44].…”

Section: Wind Braking Of Magnetarsmentioning

confidence: 99%

See 3 more Smart Citations

Pulsar braking: magnetodipole vs. wind

Tong

2015

Sci. China Phys. Mech. Astron.

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Frame-dragging effects in obliquely rotating magnetars

Kuzur

Mallick

2021

J Astrophys Astron

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CHILI, a Nanobeam Secondary Neutral Mass Spectrometer with Extraordinary Spatial Resolution, Sensitivity, and Selectivity: First Results

et al. 2015

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CHILI, the Chicago Instrument for Laser Ionization, is a nanobeam secondary neutral mass spectrometer using laser resonance ionization that is designed for a lateral resolution as small as 10 nm, a useful yield (atoms detected per atom desorbed) of 30-50%, and nearly complete suppression of isobaric interferences from both monatomic and molecular ions [1 and references therein]. It is equipped with an Orsay Physics Cobra liquid metal ion gun with a lateral resolution of 2.5 nm for desorbing from small spots and rastered areas (less than a few µm) and a 351 nm laser for desorbing from spots or rastered areas from the µm scale upwards. An optical microscope is built into CHILI and is used to image the sample and introduce the ablation laser. An Orsay Physics e -CLIPSE-plus field emission electron gun with a resolution of 4 nm is also used for imaging samples. CHILI is equipped with six tunable Ti:sapphire lasers that we designed and built, pumped by three Photonics DM-40 40 W Nd:YLF lasers (527 nm) for simultaneous isotopic measurement of two or three elements. The Ti:sapphire lasers are tunable from ~700-1000 nm, but can be frequency doubled (350-500 nm), tripled (233-333 nm) or quadrupled (205-250 nm) with nonlinear optical crystals. We anticipate a lateral resolution of ~10 nm for resonance ionization using the Ga + primary beam, as this is the approximate analytical volume for sputtering; for laser ablation, the minimum spot size will be ~1 µm. CHILI is housed within a dedicated laboratory with controlled temperature and humidity. The analytical sequence is the following: release atoms from the surface by sputtering; eject secondary ions by applying high accelerating voltage to the cloud; apply the normal accelerating voltage; fire the photoionization lasers; and mass analyze the photoions. CHILI's removable sample holder is capable of mounting a variety of common types of samples, including 1" diameter polished sections, ½" and 1 cm diameter SEM stubs, and TEM samples.As an initial test of CHILI, we analyzed some presolar SiC grains from mount KJG#2. The grains were extracted from the Murchison CM2 meteorite more than 20 years ago [2] and represent samples of stars that lived and died before the solar system formed. In contrast to recent work on KJG grains [3][4][5], the samples in this study were not additionally treated with concentrated acids to remove parent-body or terrestrial contamination. The grains were mounted on a high purity gold foil by depositing them from a suspension and pressing them into the gold with a sapphire window. Prior to analysis, energy dispersive X-ray images of the mount were acquired in a scanning electron microscope to locate SiC grains on the gold foil; 22 grains were selected for this study. Using previously developed ionization schemes, the Ti:sapphire lasers were tuned for resonance ionization of strontium, zirconium, and barium. Isotopic standards used in this study are NIST SRM 855a with 180 ppm Sr, Zr metal, NIST SRM 1264a with 690 ppm Zr, and terrestrial BaTiO 3 , all of ...

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Pulsar Wind Model for the Spin-Down Behavior of Intermittent Pulsars

Cited by 21 publications

References 37 publications

Pulsar braking: magnetodipole vs. wind

Pulsar braking: magnetodipole vs. wind

Frame-dragging effects in obliquely rotating magnetars

CHILI, a Nanobeam Secondary Neutral Mass Spectrometer with Extraordinary Spatial Resolution, Sensitivity, and Selectivity: First Results

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