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dc.contributor.authorCubarsí Morera, Rafael
dc.contributor.authorStojanovic, Milan
dc.contributor.authorNinkovic, Slobodan
dc.date.accessioned2022-01-18T10:49:16Z
dc.date.available2022-01-18T10:49:16Z
dc.date.issued2021-08
dc.identifier.citationCubarsi, R.; Stojanovic, M.; Ninkovic, S. Orbital eccentricities as indicators of stellar populations. II. Vertical velocity distribution from the Gaia DR2 catalogue. "Astronomy and astrophysics", Agost 2021, vol. 652, p. A58:1-A58:17.
dc.identifier.issn0004-6361
dc.identifier.urihttp://hdl.handle.net/2117/359890
dc.description.abstractContext. In previous work, we showed how the planar and vertical eccentricities of disc stars, e and e' , could be used as indicators of the stars’ kinematic populations. For a local stellar sample drawn from the Gaia DR2 catalogue, these populations were represented geometrically in the eccentricity diagram, e'² vs e² , approximately separated by straight lines. Aims. In the current work, we propose a new relationship between the star’s perpendicular velocity and its vertical eccentricity, allowing for a reevaluation of the critical vertical eccentricity and maximum height, z_max, specific to each population component. Methods. We approximated the local potential function to be consistent with the actual shape of the curve that relates the maximum vertical speed of a star and its maximum height. The curve corresponds to a non-linear restoring vertical force, where the stiffness decreases with an increase in the maximum height. The constants involved in this fitting, together with the population velocity dispersions, determine the specific region for each population in the eccentricity diagram. Results. The new classification determines 88% of the sample is made up of thin disc stars and 9% of thick disc stars, whereby 3% of the stars have been relabelled, by providing thinner thin and thick discs. Nested thin disc subsamples allow us to estimate Strömberg’s asymmetric drift equation, leading to a heliocentric velocity of the circular orbit of V_c ˜ -12.9 km s -1 , an absolute rotation velocity of T_c ˜ 227 km s -1 , and a rotation component of the Galactocentric velocity of the Sun at T_¿ ˜ 240 km s -1 . Conclusions. The thin disc stars of our local sample are characterised based on values 0 = e = 0.32, 0 = e' = 0.09, and z_max = 0.7 kpc. Disc stars satisfy 0 = e = 0.44, 0 = e' = 0.18, z_max = 1.5 kpc. The maximum vertical peculiar velocity for disc stars is found to be w_0 = 115 km s -1 . The assumed potential provides a stellar density of the disc vanishing at z_0 = 1.8 kpc. The approximate behaviour in the local disc is that a small decrease in the stiffness is associated with a relative decrease in the limiting velocity, which produces a thinner disc and a loss of stars in the local cylinder, both in a similar proportion to the limiting velocity.
dc.language.isoeng
dc.publisherEDP Sciences
dc.subjectÀrees temàtiques de la UPC::Matemàtiques i estadística::Matemàtica aplicada a les ciències
dc.subjectÀrees temàtiques de la UPC::Matemàtiques i estadística::Impacte ambiental
dc.subject.lcshKinematics
dc.subject.lcshAstronomy and astrophysics
dc.subject.otherGalaxy: Kinematics and dynamics – Galaxy: Disc – Stars: Kinematics and dynamics – Stars: Population II
dc.titleOrbital eccentricities as indicators of stellar populations. II. Vertical velocity distribution from the Gaia DR2 catalogue
dc.typeArticle
dc.subject.lemacCinemàtica
dc.subject.lemacAstronomia
dc.identifier.doi10.1051/0004-6361/202140835
dc.description.peerreviewedPeer Reviewed
dc.subject.amsClassificació AMS::70 Mechanics of particles and systems::70B Kinematics
dc.subject.amsClassificació AMS::85 Astronomy and astrophysics
dc.relation.publisherversionhttps://www.aanda.org/articles/aa/pdf/forth/aa40835-21.pdf
dc.rights.accessOpen Access
local.identifier.drac31825070
dc.description.versionPostprint (author's final draft)
local.citation.authorCubarsi, R.; Stojanovic, M.; Ninkovic, S.
local.citation.publicationNameAstronomy and astrophysics
local.citation.volume652
local.citation.startingPageA58:1
local.citation.endingPageA58:17


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