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

Using infrared, radio, and gamma-ray data,we investigate the propagationcharacteristics of cosmic-ray (CR) electrons and nuclei in the 30 Doradus(30\,Dor) star-forming region in the Large Magellanic Cloud (LMC) using aphenomenological model based on the radio-far-infrared correlation withingalaxies. Employing a correlation analysis, we derive an average propagationlength of \sim 100-140 pc for \sim 3 GeV CR electrons resident in 30 Dor fromconsideration of the radio and infrared data. Assuming that the observedgamma-ray emission towards 30 Dor is associated with the star-forming region,and applying the same methodology to the infrared and gamma-ray data, weestimate a \sim 20 GeV propagation length of 200-320 pc for the CR nuclei. Thisis approximately twice as large as for\sim 3 GeV CR electrons, corresponding toa spatial diffusion coefficient that is \sim 4 times higher, scaling as(R/GV)^{\delta} with \delta \approx 0.7-0.8 depending on the smearing kernelused in the correlation analysis. This value is in agreement with the resultsfound by extending the correlation analysis to include \sim 70 GeV CR nucleitraced by the 3-10 GeV gamma-ray data (\delta \approx 0.66+/-0.23). Using themean age of the stellar populations in 30 Dor and the results from ourcorrelation analysis, we estimate a diffusion coefficient D_{R} \approx 0.9-1.0\times10^27 (R/GV)^{0.7} cm^2 s^-1. We compare the values of the CR electronpropagation length and surface brightness for 30 Dor and the LMC as a wholewith those of entire disk galaxies. We find that the trend of decreasingaverage CR propagation distance with increasing disk-averaged star formationactivity holds for the LMC, and extends down to single star-forming regions, atleast for the case of 30 Dor.

Characterizing Cosmic-Ray Propagation in Massive Star-Forming Regions: The Case of 30 Doradus and the Large Magellanic Cloud