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 Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Resonance spectral lines such as H I Ly {\alpha}, Mg II h&k, and Ca II H&Kthat form in the solar chromosphere are influenced by the effects of 3Dradiative transfer as well as partial redistribution (PRD). So far no one hasmodeled these lines including both effects simultaneously owing to the highcomputing demands of existing algorithms. Such modeling is howeverindispensable for accurate diagnostics of the chromosphere. We present acomputationally tractable method to treat PRD scattering in 3D modelatmospheres using a 3D non-LTE radiative transfer code. To make the methodmemory-friendly, we use the hybrid approximation of Leenaarts et al. (2012) forthe redistribution integral. To make it fast, we use linear interpolation onequidistant frequency grids. We verify our algorithm against computations withthe RH code and analyze it for stability, convergence, and usefulness ofacceleration using model atoms of Mg II with the h&k lines and H I with the Ly{\alpha} line treated in PRD. A typical 3D PRD solution can be obtained in amodel atmosphere with $252 \times 252 \times 496$ coordinate points in 50000--200 000 CPU hours, which is a factor ten slower than computations assumingcomplete redistribution. We illustrate the importance of the joint action ofPRD and 3D effects for the Mg II h&k lines for disk-center intensities as wellas the center-to-limb variation. The proposed method allows simulating PRDlines in time series of radiation-MHD models in order to interpret observationsof chromospheric lines at high spatial resolution.

Partial redistribution in 3D non-LTE radiative transfer in solar atmosphere models