FLAMES spectroscopy of low-mass stars in the young clusters σ Ori and Ori

被引：0
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作者：
Sacco, G.G. [1 ,2 ]
Franciosini, E. [1 ]
Randich, S. [4 ]
Pallavicini, R. [1 ,3 ]
机构：
[1] INAF, Osservatorio Astronomico di Palermo, Piazza del Parlamento, 1, 90134 Palermo, Italy
[2] Consorzio COMETA, via S. Sofia, 64, 95123 Catania, Italy
[3] INAF, Headquarters, viale del Parco Mellini 84, 00136 Roma, Italy
[4] INAF, Osservatorio Astrofisico di Arcetri, Largo E. Fermi, 50125 Firenze, Italy
来源：
Astronomy and Astrophysics | 2008年 / 488卷 / 01期
关键词：
Aims. We performed a detailed membership selection and studied the accretion properties of low-mass stars in the two apparently very similar young (1-10 Myr) clusters Ori and Ori. Methods. We observed 98 and 49 low-mass (0.2-1.0 ) stars in Ori and Ori respectively; using the multi-object optical spectrograph FLAMES at the VLT; with the high-resolution () HR15N grating (6470-6790 Å). We used radial velocities; Li and H to establish cluster membership and H and other optical emission lines to analyze the accretion properties of members.Results. We identified 65 and 45 members of the Ori and Ori clusters; respectively; and discovered 16 new candidate binary systems. We also measured rotational broadening for 20 stars and estimated the mass accretion rates in 25 stars of the Ori cluster; finding values between and yr and in 4 stars of the Ori cluster; finding values between and yr. Comparing our results with the infrared photometry obtained by the Spitzer satellite; we find that the fraction of stars with disks and the fraction of active disks is larger in the Ori cluster (% and %) than in Ori (% and %). Conclusions. The different disk and accretion properties of the two clusters could be due either to the effect of the high-mass stars and the supernova explosion in the Ori cluster or to different ages of the cluster populations. Further observations are required to draw a definitive conclusion. © 2008 ESO;
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页码：167 / 179
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