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

Efforts to detect low-mass exoplanets using stellar radial velocities (RVs)are currently limited by magnetic photospheric activity. Suppression ofconvective blueshift is the dominant magnetic contribution to RV variability inlow-activity Sun-like stars. Due to convective plasma motions, the magnitude ofRV contributions from the suppression of convective blueshift is related to thedepth of formation of photospheric spectral lines of a given species used tocompute the RV time series. Meunier et al. (2017), used this relation todemonstrate a method for spectroscopic extraction of the suppression ofconvective blueshift in order to isolate RV contributions, including planetaryRVs, that contribute equally to the timeseries for each spectral line. Here, weextract disk-integrated solar RVs from observations over a 2.5 year time spanmade with the solar telescope integrated with the HARPS-N spectrograph at theTelescopio Nazionale Galileo (La Palma, Canary Islands, Spain). We apply themethods outlined by Meunier et al. (2017). We are not, however, able to isolatephysically meaningful contributions of the suppression of convective blueshiftfrom this solar dataset, potentially because our dataset is from solar minimumwhen the suppression of convective blueshift may not sufficiently dominateactivity contributions to RVs. This result indicates that, for low-activitySun-like stars, one must include additional RV contributions from activitysources not considered in the Meunier et al. (2017) model at differenttimescales as well as instrumental variation in order to reach the sub-meterper second RV sensitivity necessary to detect low-mass planets in orbit aroundSun-like stars.

Testing the Spectroscopic Extraction of Suppression of Convective Blueshift