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

This paper is written as a follow-up observations to reinterpret the radialvelocity (RV) of HD 36384, where the existence of planetary systems is known tobe ambiguous. In giants, it is, in general, difficult to distinguish thesignals of planetary companions from those of stellar activities. Thus, knownexoplanetary giant hosts are relatively rare. We, for many years, have obtainedRV data in evolved stars using the high-resolution, fiber-fed BohyunsanObservatory Echelle Spectrograph (BOES) at the Bohyunsan Optical AstronomyObservatory (BOAO). Here, we report the results of RV variations in the M giantHD 36384. We have found two significant periods of 586d and 490d. Consideringthe orbital stability, it is impossible to have two planets at so close orbits.To determine the nature of the RV variability variations, we analyze theHIPPARCOS photometric data, some indicators of stellar activities, and lineprofiles. A significant period of 580d was revealed in the HIPPARCOSphotometry. H{\alpha} EW variations also show a meaningful period of 582d.Thus, the period of 586d may be closely related to the rotational modulationsand/or stellar pulsations. On the other hand, the other significant period of490d is interpreted as the result of the orbiting companion. Our orbital fitsuggests that the companion was a planetary mass of 6.6 MJ and is located at1.3 AU from the host.

A Search for exoplanets around northern circumpolar stars VIII. filter  out a planet cycle from the multi-period radial velocity variations in M  giant HD 3638