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

We investigated the space velocity components of 6610 red clump (RC) stars interms of vertical distance, Galactocentric radial distance and Galacticlongitude. Stellar velocity vectors are corrected for differential rotation ofthe Galaxy which is taken into account using photometric distances of RC stars.The space velocity components estimated for the sample stars above and belowthe Galactic plane are compatible only for the space velocity component in thedirection to the Galactic rotation of the thin disc stars. The space velocitycomponent in the direction to the Galactic rotation (V) shows a smoothvariation relative to the mean Galactocentric radial distance (Rm), while itattains its maximum at the Galactic plane. The space velocity components in theGalactic centre (U) and in the vertical direction (W) show almost flatdistributions relative to Rm with small changes in their trends at Rm=7.5 kpc.U values estimated for the RC stars in quadrant 180<l<=270 are larger than theones in quadrants 0<l<=90 and 270<l<=360. The smooth distribution of the spacevelocity dispersions reveals that the thin and thick discs are kinematicallycontinuous components of the Galaxy. Based on the W space velocity componentsestimated in the quadrants 0<l<=90 and 270<l<=360, in the inward directionrelative to the Sun, we showed that RC stars above the Galactic plane movetowards the North Galactic Pole, whereas those below the Galactic plane move inthe opposite direction. In the case of quadrant 180<l<=270, their behaviour isdifferent, i.e. the RC stars above and below the Galactic plane move towardsthe Galactic plane. We stated that the Galactic long bar is the probable originof many, but not all, of the detected features.

Local stellar kinematics from RAVE data- V. Kinematic investigation of the Galaxy with red clump stars