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

Metallicity is the first parameter to influence the horizontal branch (HB)morphology of globular clusters (GCs). It has been found, however, that someother parameters may also play an important role in affecting the morphology.While the nature of these important parameters remains unclear, they arebelieved to be likely correlated with wind mass-loss of red giants, since thismass loss determines their subsequent locations on the HB. Unfortunately, themass loss during the red giant stages of the stellar evolution is poorlyunderstood at present. The stellar winds of red giants may be tidally enhancedby companion stars if they are in binary systems. We investigate evolutionaryconsequences of red giants in binaries by including tidally enhanced stellarwinds, and examine the effects on the HB morphology of GCs. We find that red,blue, and extreme horizontal branch stars are all produced under the effects oftidally enhanced stellar wind without any additional assumptions on themass-loss dispersion. Furthermore, the horizontal branch morphology is found tobe insensitive to the tidal enhancement parameter, Bw. We compare ourtheoretical results with the observed horizontal branch morphology of globularcluster NGC 2808, and find that the basic morphology of the horizontal branchcan be well reproduced. The number of blue horizontal branch stars in ourcalculations, however, is lower than that of NGC 2808.

Effects of tidally enhanced stellar wind on the horizontal branch morphology of globular clusters