English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

General solutions of the maser polarization problem are presented forarbitrary absorption coefficients. The results are used to calculatepolarization for masers permeated by magnetic fields with arbitrary values of\xB, the ratio of Zeeman splitting to Doppler linewidth, and for anisotropicpumping. The $\xb \to 0$ limit of the magnetic solution reproduces the linearpolarization derived in previous studies, which were always conducted at thisunphysical limit. While terms of higher order in \xb\ have a negligible effecton the magnitude of $q$, they produce some major new results. In particular,the linear polarization is accompanied by circular polarization, proportionalto \xb. Because \xb\ is proportional to the transition wavelength, the circularpolarization of SiO masers should decrease with rotation quantum number, asobserved. In the absence of theory for $\xb < 1$, previous estimates ofmagnetic fields from detected maser circular polarization had to rely onconjectures in this case and generally need to be revised downward. The fieldsin SiO masers are \about\ 2--10 G and were overestimated by a factor of 8. TheOH maser regions around supergiants have fields of \about\ 0.1--0.5 mG, whichwere overestimated by factors of 10--100. The fields were properly estimatedfor OH/IR masers ($\la$ 0.1 mG) and \H2O masers in star-forming regions(\about\ 15--50 mG). Spurious solutions that required stability analysis fortheir removal in all previous studies are never reproduced here; in particular,there are no stationary physical solutions for propagation at $\sin^2\theta <\third$, where $\theta$ is the angle from the direction of the magnetic field,so such radiation is unpolarized. These spurious solutions can be identified asthe \xb\ = 0 limits of non-physical solutions and they never arise at finiteComment: 31 pages Latex file, uses AASTeX v4.0. Postscript figures available  upon reques

Polarization of Astronomical Maser Radiation. III. Arbitrary Zeeman Splitting and Anisotropic Pumping