Polarization of X-ray lines from galaxy clusters and elliptical galaxies

Zhuravleva, Irina; Churazov, E.; Sazanov, S. Yu.; Sunyaev, R.; Forman, W.; Dolag, K.

doi:10.1017/cbo9780511750809.023

Cited by 5 publications

(8 citation statements)

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“…The approach used was developed by Pozdnyakov et al (1983) and, subsequently, was successfully applied to investigate the radiative transfer in galaxy clusters (Sazonov et al 2002;Zhuravleva et al 2010). …”

Section: The Scheme Of Computationmentioning

confidence: 99%

X-ray line formation in the spectrum of SS 433

Khabibullin

Sazonov

2012

Astron. Lett.

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-The mechanisms for the formation of X-ray lines in the spectrum of SS 433 are investigated by taking into account the radiative transfer inside the jets. The results of Monte Carlo numerical simulations are presented. The effect of a decrease in line intensity due to scattering inside the jet turns out to be pronounced, but it does not exceed 60 % in magnitude on the entire grid of parameters. The line broadening due to scattering, nutational motion, and the contribution of satellites can lead to overestimates of the jet opening angle Θ from the line widths in Chandra X-ray observations. The fine structure of the lines turns out to be very sensitive to the scattering effects. This makes its investigation by planned X-ray observatories equipped with high-resolution spectrometers (primarily Astro-H) a powerful tool for diagnosing the parameters of the jets in SS 433.

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Section: The Scheme Of Computationmentioning

confidence: 99%

X-ray line formation in the spectrum of SS 433

Khabibullin

Sazonov

2012

Astron. Lett.

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“…The polarization degree was first calculated by (see also Zhuravleva et al 2010a) for the Perseus and Virgo clusters (see Fig. 6).…”

Section: Polarization Due To Resonant Scatteringmentioning

confidence: 99%

“…5 (the right panel). Zhuravleva et al (2010a), used full 3D models of galaxy clusters taken from cosmological simulations (Dolag et al 2009;Springel et al 2001) to calculate the polarization degree with an account for gas motions. For one of the most massive simulated clusters (g8 in the sample of Dolag et al 2009) the polarization degree in the He-like iron line reaches ∼25 per cent at a distance of ∼500 kpc from the center if no turbulent motions are present (Fig.…”

Section: Polarization Due To Resonant Scatteringmentioning

confidence: 99%

“…The impact of resonant scattering on surface brightness profiles has been studied via radiative transfer calculations (e.g., Gilfanov et al 1987;Shigeyama 1998;Churazov et al 2004;Zhuravleva et al 2010b) and searched for in observations of clusters, groups of galaxies and individual massive elliptical galaxies. It has been realized that the scattering should also lead to a polarization of the same lines Zhuravleva et al 2010a), with the polarization degree varying from ∼0 at the center of a cluster to tens of per cent in the cluster outskirts (although the unpolarized continuum and nearby unpolarized lines will decrease this figure for an instrument with modest spectral resolution).…”

Section: Introductionmentioning

confidence: 99%

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Resonant Scattering of X-ray Emission Lines in the Hot Intergalactic Medium

et al. 2010

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While very often a hot intergalactic medium (IGM) is optically thin to continuum radiation, the optical depth in resonant lines can be of order unity or larger. Resonant scattering in the brightest X-ray emission lines can cause distortions in the surface brightness distribution, spurious variations in the abundance of heavy elements, changes in line spectral shapes and even polarization of line emission. The magnitude of these effects not only depends on the density, temperature and ionization state of the gas, but is also sensitive to the characteristics of the gas velocity field. This opens a possibility to use resonant scattering as a convenient and powerful tool to study IGM properties. We discuss the application of these effects to galaxy clusters.

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“…applied to reveal the nature of violent and exotic sources in space, such as solar flares [34][35][36], supernova blast waves [34,37], clusters of galaxies and gamma-ray burst afterglows [11,[38][39][40]. The observation of x-ray polarization provides an insightful vision for and a unique test of the new physics in these fascinating x-ray emitting sources.…”

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Resonant Polarization Spectroscopy for Hot X-ray Plasmas

Chen¹

2016

JPSA

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X-ray line polarization spectroscopy is a method of choice for probing hot plasma conditions. The precise roles of resonant structures in this method have not been realized and fully understood. With a sophisticated relativistic close coupling Dirac R-matrix calculation of polarized radiation of the quadrupole magnetic M2 line at 2.717 Å in Ba 46+ , we revealed the nature of resonant structures in x-ray line polarization spectroscopy. We found that signatures with a heavy resonance forest imprinting on polarization may be used for a sensitive new spectroscopic method. The resonant polarization spectrum was used to determine or constrain the directional beam electron distribution of the laboratory Ba plasma. Our results provide a start of resonant polarization spectroscopy as a method for diagnostics of laboratory, fusion and astrophysical plasma source conditions.

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Polarization of X-ray lines from galaxy clusters and elliptical galaxies

Cited by 5 publications

References 0 publications

X-ray line formation in the spectrum of SS 433

X-ray line formation in the spectrum of SS 433

Resonant Scattering of X-ray Emission Lines in the Hot Intergalactic Medium

Resonant Polarization Spectroscopy for Hot X-ray Plasmas

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