Search results for "individual: Chamaeleon I"

showing 3 items of 3 documents

The Gaia-ESO survey: Metallicity of the chamaeleon i star-forming region

2014

Context. Recent metallicity determinations in young open clusters and star-forming regions suggest that the latter may be characterized by a slightly lower metallicity than the Sun and older clusters in the solar vicinity. However, these results are based on small statistics and inhomogeneous analyses. The Gaia-ESO Survey is observing and homogeneously analyzing large samples of stars in several young clusters and star-forming regions, hence allowing us to further investigate this issue. Aims. We present a new metallicity determination of the Chamaeleon I star-forming region, based on the products distributed in the first internal release of the Gaia-ESO Survey. Methods. 48 candidate member…

AstrofísicaStars: abundanceMetallicityFOS: Physical sciencesTechniques: spectroscopicContext (language use)AstrophysicsOpen clusters and associations: individual: Chamaeleon ISolar and Stellar Astrophysics (astro-ph.SR)Line (formation)Physics85A04open clusters and associations: individual: Chamaeleon I stars: pre-main sequence stars: abundances techniques: spectroscopicStars: abundancesAstronomy and AstrophysicsSurface gravityAstronomíaStarsAstrophysics - Solar and Stellar AstrophysicsSpace and Planetary ScienceChamaeleonStars: pre-main sequenceOpen clusters and associations: individual: Chamaeleon I; Stars: abundances; Stars: pre-main sequence; Techniques: spectroscopicindividual: Chamaeleon I stars: pre-main sequence stars: abundances techniques: spectroscopic [open clusters and associations]Equivalent widthOpen cluster
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The Gaia-ESO Survey: Chromospheric emission, accretion properties, and rotation in gamma Velorum and Chamaeleon

2015

Aims: One of the goals of the Gaia-ESO Survey (GES), which is conducted with FLAMES at the VLT, is the census and the characterization of the low-mass members of very young clusters and associations. We conduct a comparative study of the main properties of the sources belonging to γ Velorum (γ Vel) and Chamaeleon I (Cha I) young associations, focusing on their rotation, chromospheric radiative losses, and accretion. Methods: We used the fundamental parameters (effective temperature, surface gravity, lithium abundance, and radial velocity) delivered by the GES consortium in the first internal data release to select the members of γ Vel and Cha I among the UVES and GIRAFFE spectroscopic obser…

Astrofísicastars: chromospheresAstrophysics::High Energy Astrophysical PhenomenaAstrophysicsAstrophysics::Cosmology and Extragalactic AstrophysicsRotationStars: chromosphereOpen clusters and associations: individual:γVelorumstars: low-massStars: low-maAstrophysics::Solar and Stellar AstrophysicsOpen clusters and associations: individual: Chamaeleon Iopen clusters and associations: individual: γ VelorumQCAstrophysics::Galaxy AstrophysicsQBLine (formation)PhysicsAccretion (meteorology)stars: chromospheres ; stars: low-mass; open clusters and associations: individual: γ VelorumDiagramStars: rotationSpectral densityAstronomy and AstrophysicsAstronomy and AstrophysicStarsDistribution (mathematics)Astrophysics - Solar and Stellar AstrophysicsSpace and Planetary ScienceChamaeleonStars: pre-main sequenceAstrophysics::Earth and Planetary AstrophysicsOpen clusters and associations: individual: Chamaeleon I; Open clusters and associations: individual:γVelorum; Stars: chromospheres; Stars: low-mass; Stars: pre-main sequence; Stars: rotation
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The Gaia-ESO Survey: Structural and dynamical properties of the young cluster Chamaeleon i

2017

Investigating the physical mechanisms driving the dynamical evolution of young star clusters is fundamental to our understanding of the star formation process and the properties of the Galactic field stars. The young (~2 Myr) and partially embedded cluster Chamaeleon I is one of the closest laboratories for the study of the early stages of star cluster dynamics in a low-density environment. The aim of this work is to study the structural and kinematical properties of this cluster combining parameters from the high-resolution spectroscopic observations of the Gaia-ESO Survey with data from the literature. Our main result is the evidence of a large discrepancy between the velocity dispersion …

astro-ph.SRStellar populationopen clustersand associations: individual: Chamaeleon IIndividual: Chamaeleon I [Open clusters and associations]Open clusters and associations: Individual: Chamaeleon I; Stars: Kinematics and dynamics; Stars: Pre-main sequence; Techniques: Spectroscopicastro-ph.GAstars: kinematics and dynamicsFOS: Physical sciencesAstrophysicsAstrophysics::Cosmology and Extragalactic Astrophysicsstars: pre-main sequence01 natural sciencesVirial theoremKinematics and dynamics [Stars]Stars: Kinematics and dynamic0103 physical sciencesCluster (physics)Mass segregationAstrophysics::Solar and Stellar Astrophysics010303 astronomy & astrophysicsStellar evolutionQCSolar and Stellar Astrophysics (astro-ph.SR)Astrophysics::Galaxy AstrophysicsQBPhysicsPre-main sequence [Stars]open clusters and associations: individual: Chamaeleon I010308 nuclear & particles physicsVelocity dispersionAstronomy and AstrophysicsAstrophysics - Astrophysics of Galaxies[SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]stars: kinematics and dynamics; stars: pre-main sequence; open clustersand associations: individual: Chamaeleon I; techniques: spectroscopicStar clusterAstrophysics - Solar and Stellar AstrophysicsSpace and Planetary ScienceAstrophysics of Galaxies (astro-ph.GA)Astrophysics::Earth and Planetary AstrophysicsSpectroscopic [Techniques]Equivalent widthtechniques: spectroscopicQB799
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