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 Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

We present results from an optical spectroscopic investigation of the massivebinary system [L72] LH~54-425 in the LH 54 OB association in the LargeMagellanic Cloud. We revise the ephemeris of [L72] LH 54-425 and find anorbital period of 2.247409 +/- 0.000010 days. We find spectral types of O3 Vfor the primary and O5 V for the secondary. We made a combined solution of theradial velocities and previously published V-band photometry to determine theinclination for two system configurations, i = 52 degrees for the configurationof the secondary star being more tidally distorted and i = 55 degrees for theprimary as the more tidally distorted star. We argue that the latter case ismore probable, and this solution yields masses and radii of M_1 = 47 +/- 2M_Sun and R_1 = 11.4 +/- 0.1 R_Sun for the primary, and M_2 = 28 +/- 1 M_Sunand R_2 = 8.1 +/- 0.1 R_Sun for the secondary. Our analysis places LH 54-425amongst the most massive stars known. Based on the position of the two starsplotted on a theoretical HR diagram, we find the age of the system to be about1.5 Myr.

Dynamical Masses for the Large Magellanic Cloud Massive Binary System [L72] LH 54-425