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

New physical elements of the early B-type eclipsing binary V346Cen are derived using the HARPS spectra downloaded from the ESOarchive and also numerous photometric observations from varioussources. A model of the observed times of primary and secondaryminima that fits them best is a combination of the apsidalmotion and an abrupt decrease in the orbital period from6(d).322123 to 6(d).321843 (shortening by 24 s), which occurredsomewhere around JD 2 439 000. Assumption of a secularlydecreasing orbital period provides a significantly worse fit.Local times of minima and the final solution of the light curvewere obtained with the program PHOEBE. Radial velocities ofboth binary components, free of line blending, were derived via2D cross-correlation with a program built on the principles ofthe program TODCOR. The oxygen lines in the secondary spectraare weaker than those in the model spectra of solar chemicalcomposition. Using the component spectra disentangled with theprogram KOREL,we find that both components rotate considerablyfaster than would correspond to the synchronization atperiastron. The apside rotation known from earlier studies isconfirmed and compared to the theoretical value.

V346 Centauri: Early-type eclipsing binary with apsidal motion and abrupt change of orbital period