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 report on radial velocity time series for two M0.0V stars, GJ338B andGJ338A, using the CARMENES spectrograph, complemented by ground-telescopephotometry from Las Cumbres and Sierra Nevada observatories. We aim to explorethe presence of small planets in tight orbits using the spectroscopic radialvelocity technique. We obtained 159 and 70 radial velocity measurements ofGJ338B and A, respectively, with the CARMENES visible channel. We also compiledadditional relative radial velocity measurements from the literature and acollection of astrometric data that cover 200 a of observations to solve forthe binary orbit. We found dynamical masses of 0.64$\pm$0.07M$_\odot$ forGJ338B and 0.69$\pm$0.07M$_\odot$ for GJ338A. The CARMENES radial velocityperiodograms show significant peaks at 16.61$\pm$0.04 d (GJ338B) and16.3$^{+3.5}_{-1.3}$ d (GJ338A), which have counterparts at the samefrequencies in CARMENES activity indicators and photometric light curves. Weattribute these to stellar rotation. GJ338B shows two additional, significantsignals at 8.27$\pm$0.01 and 24.45$\pm$0.02 d, with no obvious counterparts inthe stellar activity indices. The former is likely the first harmonic of thestar's rotation, while we ascribe the latter to the existence of a super-Earthplanet with a minimum mass of 10.27$^{+1.47}_{-1.38}$$M_{\oplus}$ orbitingGJ338B. GJ338B b lies inside the inner boundary of the habitable zone aroundits parent star. It is one of the least massive planets ever found around anymember of stellar binaries. The masses, spectral types, brightnesses, and eventhe rotational periods are very similar for both stars, which are likely coevaland formed from the same molecular cloud, yet they differ in the architectureof their planetary systems.

The CARMENES search for exoplanets around M dwarfs. A super-Earth planet orbiting HD 79211 (GJ 338 B)