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

Clusters or associations of early-type stars are often associated with a'superbubble' of hot gas. The formation of such superbubbles is caused by thefeedback from massive stars. The complex N206 in the Large Magellanic Cloudexhibits a superbubble and a rich massive star population. We observed thesemassive stars using the FLAMES multi-object spectrograph at ESO-VLT. AvailableUV spectra from HST, IUE, and FUSE are also used. The spectral analysis isperformed with Potsdam Wolf-Rayet (PoWR) model atmospheres. We present thestellar and wind parameters of the OB stars and the two WR binaries in the N206complex. Twelve percent of the sample show Oe/Be type emission lines, althoughmost of them appear to rotate far below critical. We found eight runaway starsbased on their radial velocity. The wind-momentum luminosity relation of our OBsample is consistent with the expectations. The HRD of the OB stars reveals alarge age spread (1-30 Myr), suggesting different episodes of star formation inthe complex. The youngest stars are concentrated in the inner part of thecomplex, while the older OB stars are scattered over outer regions. We derivedthe present day mass function for the entire N206 complex as well as for thecluster NGC2018. Three very massive Of stars are found to dominate the feedbackamong 164 OB stars in the sample. The two WR winds alone release about as muchmechanical luminosity as the whole OB star sample. The cumulative mechanicalfeedback from all massive stellar winds is comparable to the combinedmechanical energy of the supernova explosions that likely occurred in thecomplex. Accounting also for the WR wind and supernovae, the mechanical inputover the last five Myr is ~$2.3\times10^{52}$ erg, which exceeds the currentenergy content of the complex by more than a factor of five. The morphology ofthe complex suggests a leakage of hot gas from the superbubble.

Stellar population of the superbubble N206 in the LMC II. Parameters of the OB and WR stars, and the total massive star feedback