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

Young low-mass stars of equal-mass exhibit a distribution of rotationperiods. At the very early phases of stellar evolution, this distribution isset by the star-disc locking mechanism. The primordial disc lifetime and,consequently, the duration of the disc-locking mechanism, can be significantlyshortened by the presence of a close companion, making the rotation perioddistribution of close binaries different from that of either single stars orwide binaries. We use new data to investigate and better constrain the range ofages, the components separation and the mass ratio dependence at which therotation period distribution has been significantly affected by the discdispersal that is enhanced by close companions. We select a sample of closebinaries in the Upper Scorpius association (age $\sim$8 Myr) whose componentshave measured the separation and the rotation periods and compare their perioddistribution with that of coeval stars that are single stars. We find thatcomponents of close binaries have on average rotation periods shorter thansingle stars. More precisely, binaries with about equal-mass components (0.9$\le$ M2/M1 $\le$ 1.0) have rotation periods on average by $\sim$0.4 d shorterthan single stars; binaries with smaller mass ratios (0.8 $<$ M2/M1 $<$ 0.9)have rotation periods on average by $\sim$1.9 d the primary components, and by$\sim$1.0 d the secondary components shorter than single stars. A comparisonwith the older 25-Myr $\beta$ Pictoris association shows that, whereas in thelatter all close binaries with projected separation $\rho$ $\le$ 80 AU allrotate faster than single stars, in the Upper Scorpius that has happened forabout 70% stars, yet. We interpret the enhanced rotation in close binaries withrespect to single stars as the consequence of an early disc dispersal inducedby the presence of close companions.

Evidence from stellar rotation for early disc dispersal owing to close companions