Modeling radio circular polarization in the Crab nebula

Bucciantini, N.; Olmi, Barbara

doi:10.1093/mnras/stx3231

Cited by 4 publications

(3 citation statements)

References 84 publications

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“…8), with a polarized fraction of 40-50%, and extending for several parsecs. Using the subgrid model by Bandiera & Petruk (2016) recently applied to PWNe (Bucciantini et al 2017;Bucciantini & Olmi 2018), we can estimate a typical turbulence with δB/B ∼ 0.3. On the other hand low polarization systems like the Mouse G359.23-0.82 (Yusef-Zadeh & Gaensler 2005), with polarized fraction below 10% are likely characterized by strong turbulence, in part already evident in the rapid change of polarization pattern.…”

Section: Discussionmentioning

confidence: 99%

A laminar model for the magnetic field structure in bow-shock pulsar wind nebulae

Bucciantini

2018

Monthly Notices of the Royal Astronomical Society

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Bow Shock Pulsar Wind Nebulae are a class of non-thermal sources, that form when the wind of a pulsar moving at supersonic speed interacts with the ambient medium, either the ISM or in a few cases the cold ejecta of the parent supernova. These systems have attracted attention in recent years, because they allow us to investigate the properties of the pulsar wind in a different environment from that of canonical Pulsar Wind Nebulae in Supernova Remnants. However, due to the complexity of the interaction, a full-fledged multidimensional analysis is still laking. We present here a simplified approach, based on Lagrangian tracers, to model the magnetic field structure in these systems, and use it to compute the magnetic field geometry, for various configurations in terms of relative orientation of the magnetic axis, pulsar speed and observer direction. Based on our solutions we have computed a set of radio emission maps, including polarization, to investigate the variety of possible appearances, and how the observed emission pattern can be used to constrain the orientation of the system, and the possible presence of turbulence.

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Section: Discussionmentioning

confidence: 99%

A laminar model for the magnetic field structure in bow-shock pulsar wind nebulae

Bucciantini

2018

Monthly Notices of the Royal Astronomical Society

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“…(3.9) and numerically solve it. The obtained value of V (t)/I(t) at t = τ /2 is then compared to the minimum detectable circular polarization (V /I) min = 0.01 [48,49]. If the value is discernible, the corresponding m and g aγγ are exported to construct the excluded JCAP04(2024)069 The plot illustrates the parameter space that can be excluded based on the observed circular polarization effect.…”

Section: Constraining Alps Parameter Space: the Potential Of The Schemementioning

confidence: 99%

Induced circular polarization on photons due to interaction with axion-like particles in rotating magnetic field of neutron stars

Sharifian,

Zarei,

Matarrese

et al. 2024

J. Cosmol. Astropart. Phys.

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We investigate how the photon polarization is affected by the interaction with axion-like particles (ALPs) in the rotating magnetic field of a neutron star (NS). Using quantum Boltzmann equations the study demonstrates that the periodic magnetic field of millisecond NSs enhances the interaction of photons with ALPs and creates a circular polarization on them. A binary system including an NS and a companion star could serve as a probe. When the NS is in front of the companion star with respect to the earth observer, there is a circular polarization on the previously linearly polarized photons as a result of the interaction with ALPs there. After a half-binary period, the companion star passes in front of the NS, and the circular polarization of photons disappears and changes to linear. The excluded parameter space for a millisecond NS with 300 Hz rotating frequency, highlights the coupling constant of 1.7 × 10-11 GeV-1 ≤ gaγγ ≤ 1.6 × 10-3 GeV-1 for the ALP masses in the range of 7 × 10-12 eV ≤ ma ≤ 1.5 × 103 eV.

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“…We note that the hybrid thermal/nonthermal electron energy distribution and the strong absorption of polarized photons in our model should be important when we suggest to perform Event Horizon Telescope (EHT) polarization observations. The circular polarization of pulsar wind nebula (PWN) can also be further checked if we consider the thermal electron contribution (Bucciantini & Olmi 2018). We may even consider performing our model for the diffuse synchrotron emission if the electrons in the interstellar medium also have a thermal component (Herron et al 2018).…”

Section: Possible Applicationsmentioning

confidence: 99%

Synchrotron Polarization Radiative Transfer: Relativistic Thermal Electron Contribution

Mao¹,

Covino²,

Wang³

2018

ApJ

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Relativistic thermal electrons moving in a large-scale magnetic field can produce synchrotron radiation. Linear synchrotron polarization can also be produced by the relativistic thermal electrons. In this paper, we utilize a hybrid thermalnonthermal electron energy distribution to calculate circular synchrotron polarization. We further compute the radiative transfer of the synchrotron polarization in the optical and radio bands when we consider the contribution of the thermal electrons. We attempt to apply the polarization results to some astrophysical objects, such as kilonova like AT 2017gfo/GW170817, the fast radio burst (FRB), the Gamma-ray burst (GRB) afterglow, and the supernova remnant (SNR). The large optical depth of radiative transfer effects the small polarization degrees of these populations when the media surrounding the synchrotron sources take heavy absorption to the polarized photons. We need a strong magnetic field in our model to reproduce the linear and circular polarization properties that were observed in FRB 140514. This indicates that FRBs have a neutron star origin.

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Modeling radio circular polarization in the Crab nebula

Cited by 4 publications

References 84 publications

A laminar model for the magnetic field structure in bow-shock pulsar wind nebulae

A laminar model for the magnetic field structure in bow-shock pulsar wind nebulae

Induced circular polarization on photons due to interaction with axion-like particles in rotating magnetic field of neutron stars

Synchrotron Polarization Radiative Transfer: Relativistic Thermal Electron Contribution

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