Influence of rare gases on laser-chemical reactions. II. Experiments

Sazonov, V. N.; Shmerling, G V

doi:10.1070/qe1983v013n05abeh004256

Cited by 2 publications

(7 citation statements)

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“…(2) (Sazonov 1969;Pacholczyk 1970Pacholczyk , 1977Jones & Odell 1977a;Degl'innocenti & Degl'innocenti 1985;Huang & Shcherbakov 2011a;Janett & Paganini 2018), where s is the path length of the radiation; the tensor index i or j in equation (1) runs from 1 to 4, denoting the Stokes parameters I ν , Q ν , U ν and V ν , respectively. The coefficient tensor κ i j,ν accounts for the amount of absorption (through κ ν , q ν , u ν and v ν ), rotation (through f ν ) and conversion (through h ν and g ν ) of the radiation along its direction of propagation, and i,ν accounts for the amount of emission.…”

Section: Conventional Polarized Radiative Transfermentioning

confidence: 99%

“…Q ν ↔ V ν ; U ν ↔ V ν ). The equation for the transfer of polarized radiation presented at above, with variable transfer coefficients, is suitable for transport in a homogeneous or weakly anisotropic medium (Sazonov & Tsytovich 1968;Sazonov 1969;Pacholczyk 1977;Jones & Odell 1977a). Note that all quantities in equations (1) and (2) depend on the frequency of the radiation ν.…”

Section: Conventional Polarized Radiative Transfermentioning

confidence: 99%

“…We note that different handedness of coordinate systems (right-handed or left-handed), as well as the geometry of the problem, have been used in the literature that derived the polarized radiative transfer equations and the (thermal and non-thermal) transfer coefficients (see e.g. Sazonov 1969;Pacholczyk 1970;Melrose & McPhedran 1991;Huang & Shcherbakov 2011a). The sign of Stokes V ν that describes the sense of the circular polarization also varies from paper to paper.…”

Section: Conventional Polarized Radiative Transfermentioning

confidence: 99%

“…U ν ↔ V ν but Q ν V ν ) by a choice of a local coordinate system (see e.g. Sazonov 1969;Pacholczyk 1977). With the geometry defined in Fig.…”

Section: Conventional Polarized Radiative Transfermentioning

confidence: 99%

“…Electric field of an electromagnetic wave traveling along k z oscillates in the (x, y)-plane. By such a choice of configuration (or by the choice of y ỹ in the systems defined in Sazonov (1969);Pacholczyk (1977)), absorption coefficient u ν , conversion coefficient g ν and emission coefficient U,ν are zeros.…”

Section: Appendix A: Adopted Coordinate Systemmentioning

confidence: 99%

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Covariant polarized radiative transfer on cosmological scales for investigating large-scale magnetic field structures

Chan

et al. 2018

Monthly Notices of the Royal Astronomical Society

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Polarization of radiation is a powerful tool to study cosmic magnetism and analysis of polarization can be used as a diagnostic tool for large-scale structures. In this paper, we present a solid theoretical foundation for using polarized light to investigate largescale magnetic field structures: the cosmological polarized radiative transfer (CPRT) formulation. The CPRT formulation is fully covariant. It accounts for cosmological and relativistic effects in a self-consistent manner and explicitly treats Faraday rotation, as well as Faraday conversion, emission, and absorption processes. The formulation is derived from the first principles of conservation of phase-space volume and photon number. Without loss of generality, we consider a flat Friedmann-Robertson-Walker (FRW) space-time metric and construct the corresponding polarized radiative transfer equations. We propose an all-sky CPRT calculation algorithm, based on a ray-tracing method, which allows cosmological simulation results to be incorporated and, thereby, model templates of polarization maps to be constructed. Such maps will be crucial in our interpretation of polarized data, such as those to be collected by the Square Kilometer Array (SKA). We describe several tests which are used for verifying the code and demonstrate applications in the study of the polarization signatures in different distributions of electron number density and magnetic fields. We present a pencilbeam CPRT calculation and an all-sky calculation, using a simulated galaxy cluster or a model magnetized universe obtained from GCMHD+ simulations as the respective input structures. The implications on large-scale magnetic field studies are discussed; remarks on the standard methods using rotation measure are highlighted.

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Section: Conventional Polarized Radiative Transfermentioning

confidence: 99%

Section: Conventional Polarized Radiative Transfermentioning

confidence: 99%

Section: Conventional Polarized Radiative Transfermentioning

confidence: 99%

“…U ν ↔ V ν but Q ν V ν ) by a choice of a local coordinate system (see e.g. Sazonov 1969;Pacholczyk 1977). With the geometry defined in Fig.…”

Section: Conventional Polarized Radiative Transfermentioning

confidence: 99%

Section: Appendix A: Adopted Coordinate Systemmentioning

confidence: 99%

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Covariant polarized radiative transfer on cosmological scales for investigating large-scale magnetic field structures

Chan

et al. 2018

Monthly Notices of the Royal Astronomical Society

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Detecting primordial gravitational waves with circular polarization of the redshifted 21 cm line. II. Forecasts

Mishra

Hirata

2018

Phys. Rev. D

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In the first paper of this series, we showed that the CMB quadrupole at high redshifts results in a small circular polarization of the emitted 21 cm radiation. In this paper we forecast the sensitivity of future radio experiments to measure the CMB quadrupole during the era of first cosmic light (z ∼ 20). The tomographic measurement of 21 cm circular polarization allows us to construct a 3D remote quadrupole field. Measuring the B-mode component of this remote quadrupole field can be used to put bounds on the tensor-to-scalar ratio r. We make Fisher forecasts for a future Fast Fourier Transform Telescope (FFTT), consisting of an array of dipole antennas in a compact grid configuration, as a function of array size and observation time. We find that a FFTT with a side length of 100 km can achieve σðrÞ ∼ 4 × 10 −3 after ten years of observation and with a sky coverage f sky ∼ 0.7. The forecasts are dependent on the evolution of the Lyman-α flux in the pre-reionization era, that remains observationally unconstrained. Finally, we calculate the typical order of magnitudes for circular polarization foregrounds and comment on their mitigation strategies. We conclude that detection of primordial gravitational waves with 21 cm observations is in principle possible, so long as the primordial magnetic field amplitude is small, but would require a very futuristic experiment with corresponding advances in calibration and foreground suppression techniques.

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Influence of rare gases on laser-chemical reactions. II. Experiments

Cited by 2 publications

References 1 publication

Covariant polarized radiative transfer on cosmological scales for investigating large-scale magnetic field structures

Covariant polarized radiative transfer on cosmological scales for investigating large-scale magnetic field structures

Detecting primordial gravitational waves with circular polarization of the redshifted 21 cm line. II. Forecasts

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