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

Phosphorus abundance is crucial for DNA-based extraterrestrial life inexoplanets. Atomic data for observed spectral lines of P-ions are needed forits accurate determination. We present the first calculations for collisionstrengths for the forbidden PIII fine structure transition $3s^23p(^2P^o_{1/2-3/2})$ within the ground state at 17.9 $\mu$m, as well as allowedUV transitions in the $3s^23p (^2P^o_{1/2,3/2}) \rightarrow 3s3p^2(^2D_{3/2,5/2}, ^2S_{1/2}, ^2P_{1/2,3/2})$ multiplets between 915-1345 $\AA$.Collision strengths are computed using the Breit-Pauli R-Matrix methodincluding the first 18 levels, and they exhibit extensive auto-ionizingresonance structures. In particular, the Maxwellian averaged effectivecollision strength for the FIR 17.9 $\mu$m transition shows a factor 3temperature variation broadly peaking at typical nebular temperatures. Itstheoretical emissivity with solar phosphorus abundance is computed relative toH$\beta$ and found to be similar to observed intensties from planetary nebulae;the abundances derived in earlier works are 3-5 times sub-solar. The resultspertain to the reported paucity of phosphorus from preferred production sitesin supernovae, and abundances in planetary nebulae and supernova remnants.

Collision strengths for FIR and UV transtions in PIII and the phosphorus abundance