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

Only a few well characterized very low-mass M dwarfs are known today. Ourunderstanding of M dwarfs is vital as these are the most common stars in oursolar neighborhood. We aim to characterize the properties of a rare F+dMstellar system for a better understanding of the low-mass end of theHertzsprung-Russel diagram. We used photometric light curves and radialvelocity follow-up measurements to study the binary. Spectro- scopic analysiswas used in combination with isochrone fitting to characterize the primarystar. The primary star is an early F-type main-sequence star with a mass of(1.493 +- 0.073) Msun and a radius of (1.474 +- 0.040) Rsun. The companion isan M dwarf with a mass of (0.188 +- 0.014) Msun and a radius of (0.234 +-0.009) Rsun. The orbital period is (1.35121 +- 0:00001)d. The secondary star isamong the lowest-mass M dwarfs known to date. The binary has not reached a 1:1spin-orbit synchronization. This indicates a young main-sequence binary with anage below ~250 Myrs. The mass-radius relation of both components are inagreement with this finding.

An M dwarf Companion to an F-type Star in a young main-sequence binary