Polarimetry of Magnetars and Isolated Neutron Stars

Caiazzo, Ilaria; Turolla, R.

doi:10.1007/978-3-030-19715-5_12

Cited by 4 publications

(3 citation statements)

References 84 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…28 and θ m measures how circular the propagation modes are and can be calculated using Eq. 12.29 of Caiazzo et al (2019). Because the resonance lies at different energies along the column, the net effect of the vacuum resonance is modest.…”

Section: Including the Effect Of Vacuum Birefringencementioning

confidence: 99%

“…The results of Gnedin et al (1978) indicate that at this density, the vacuum dominates the birefringence for photon energies above about 2 keV and below the cyclotron energy. In the vicinity of this critical energy, or vacuum resonance (see Caiazzo et al 2019, and references therein), the propagation modes through the magnetised plasma are approximately circular as opposed to approximately linear elsewhere. This could result in a modest depolarisation of the radiation near this energy, if a substantial depolarisation can occur between scattering events.…”

Section: Including the Effect Of Vacuum Birefringencementioning

confidence: 99%

See 1 more Smart Citation

Polarisation of Accreting X-ray Pulsars. I. A New Model

Caiazzo¹

2020

Preprint

Self Cite

View full text Add to dashboard Cite

A new window is opening in high-energy astronomy: X-ray polarimetry. With many missions currently under development and scheduled to launch as early as 2021, observations of the Xray polarisation of accreting X-ray pulsars will soon be available. As polarisation is particularly sensitive to the geometry of the emission region, the upcoming polarimeters will shed new light on the emission mechanism of these objects, provided that we have sound theoretical models that agree with current spectroscopic and timing observation and that can make predictions of the polarisation parameters of the emission. We here present a new model for the polarised emission of accreting X-ray pulsars in the accretion column scenario that for the first time takes into account the macroscopic structure and dynamics of the accretion region and the propagation of the radiation toward the observer, including relativistic beaming, gravitational lensing and quantum electrodynamics. In this paper we present all the details of the model, while in a companion paper, we apply our model to predict the polarisation parameters of the bright X-ray pulsar Hercules X-1.

show abstract

Section: Including the Effect Of Vacuum Birefringencementioning

confidence: 99%

Section: Including the Effect Of Vacuum Birefringencementioning

confidence: 99%

Polarisation of Accreting X-ray Pulsars. I. A New Model

Caiazzo¹

2020

Preprint

Self Cite

View full text Add to dashboard Cite

show abstract

“…This combination results in a complicated picture, where parameters of polarisation depend on the atmosphere of the NS (or on existence of the condensate), value of the field, its topology, and orientation of spin and field relative to the line of sight. A detailed review on all these ingredients can be found in [216].…”

Section: Polarisationmentioning

confidence: 99%

Evolution of Neutron Star Magnetic Fields

2021

View full text Add to dashboard Cite

Neutron stars are natural physical laboratories allowing us to study a plethora of phenomena in extreme conditions. In particular, these compact objects can have very strong magnetic fields with non-trivial origin and evolution. In many respects, its magnetic field determines the appearance of a neutron star. Thus, understanding the field properties is important for the interpretation of observational data. Complementing this, observations of diverse kinds of neutron stars enable us to probe parameters of electro-dynamical processes at scales unavailable in terrestrial laboratories. In this review, we first briefly describe theoretical models of the formation and evolution of the magnetic field of neutron stars, paying special attention to field decay processes. Then, we present important observational results related to the field properties of different types of compact objects: magnetars, cooling neutron stars, radio pulsars, and sources in binary systems. After that, we discuss which observations can shed light on the obscure characteristics of neutron star magnetic fields and their behaviour. We end the review with a subjective list of open problems.

show abstract

Polarization of accreting X-ray pulsars. I. A new model

Caiazzo

2020

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

A new window is opening in high-energy astronomy: X-ray polarimetry. With many missions currently under development and scheduled to launch as early as 2021, observations of the X-ray polarisation of accreting X-ray pulsars will soon be available. As polarisation is particularly sensitive to the geometry of the emission region, the upcoming polarimeters will shed new light on the emission mechanism of these objects, provided that we have sound theoretical models that agree with current spectroscopic and timing observation and that can make predictions of the polarisation parameters of the emission. We here present a new model for the polarised emission of accreting X-ray pulsars in the accretion column scenario that for the first time takes into account the macroscopic structure and dynamics of the accretion region and the propagation of the radiation toward the observer, including relativistic beaming, gravitational lensing and quantum electrodynamics. In this paper, we present all the details of the model, while in a companion paper, we apply our model to predict the polarisation parameters of the bright X-ray pulsar Hercules X-1.

show abstract

Polarimetry of Magnetars and Isolated Neutron Stars

Cited by 4 publications

References 84 publications

Polarisation of Accreting X-ray Pulsars. I. A New Model

Polarisation of Accreting X-ray Pulsars. I. A New Model

Evolution of Neutron Star Magnetic Fields

Polarization of accreting X-ray pulsars. I. A new model

Contact Info

Product

Resources

About