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

Under the right conditions brown dwarfs that gain enough mass late in theirlives to cross the hydrogen burning limit will not turn into low-mass stars,but rather remain essentially brown dwarf-like. While these objects, calledeither beige dwarfs or over-massive brown dwarfs, may exist in principle, itremains unclear exactly how they would form astrophysically. We show thataccretion from AGB winds, aided by the wind Roche lobe overflow mechanism, islikely to produce a substantial population of observable overmassive browndwarfs, though other mechanisms are still plausible. Specifically we predictthat sun-like stars born with a massive brown dwarf companion on an orbit witha semi-major axis of order 10 AU will likely produce overmassive brown dwarfs,which may be found today as companions to the donor star's remnant white dwarf.The identification and characterization of such an object would produce uniqueconstraints on binary evolution because there is a solid upper limit on thebrown dwarf's initial mass.

Where to find over-massive brown dwarfs: new benchmark systems for binary evolution