Volume 525, January 2011
|Number of page(s)||18|
|Section||Stellar structure and evolution|
|Published online||30 November 2010|
Osservatorio Astrofisico di Arcetri, INAF, Largo E. Fermi 5,
2 Università di Firenze, Dipartimento di Astronomia, Largo E. Fermi 2, 50125 Firenze, Italy
3 ESO, Karl-Schwarszchild Strasse 2, 85748 Garching bei München, Germany
Received: 29 June 2010
Accepted: 9 October 2010
This paper presents the results of an U band survey with FORS1/VLT of a large area in the σ Ori star-forming region. We combine the U-band photometry with literature data to compute accretion luminosity and mass accretion rates from the U-band excess emission for all objects (187) detected by Spitzer in the FORS1 field and classified by Hernandez et al. as likely members of the cluster. The sample stars range in mass from ~0.06 to ~1.2 M⊙; 72 of them show evidence of disks and we measure mass accretion rates Ṁacc between <10-11 and few 10-9 M⊙/y, using the colors of the diskless stars as photospheric templates. Our results confirm the dependence of Ṁacc on the mass of the central object, which is stronger for low-mass stars and flattens out for masses larger than ~0.3 M⊙; the spread of Ṁacc for any value of the stellar mass is ~2 orders of magnitude. We discuss the implications of these results in the context of disk evolution models. Finally, we analyze the relation between Ṁacc and the excess emission in the Spitzer bands, and find that at Ṁacc ~ 10-10 M⊙/y the inner disks change from optically thin to optically thick.
Key words: stars: formation / accretion, accretion disks / open clusters and associations: individual:σOrionis
Based on observations collected at the European Southern Observatory, Chile. Program 082.C-0313(A).
Appendices are only available in electronic form at http://www.aanda.org
© ESO, 2010
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