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Photometric determination of the mass accretion rates of pre-mainsequence stars – III. Results in the Large Magellanic Cloud

Authors

  • L. Spezzi,

    Corresponding author
    1. European Space Agency (ESTEC), PO Box 299, 2200 AG Noordwijk, the Netherlands
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  • G. De Marchi,

    1. European Space Agency (ESTEC), PO Box 299, 2200 AG Noordwijk, the Netherlands
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  • N. Panagia,

    1. Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
    2. INAFCT, Osservatorio Astrofisico di Catania, Via S. Sofia 78, I-95123 Catania, Italy
    3. Supernova Limited, OYV No. 131, Northsound Road, Virgin Gorda, 3700, British Virgin Islands
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  • A. Sicilia-Aguilar,

    1. Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
    2. Departamento de Física Teórica, Universidad Autónoma de Madrid, Cantoblanco 28049, Madrid, Spain
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  • B. Ercolano

    1. Ludwig-Maximilians-Universitaet, University Observatory Munich, Scheinerstr. 1, D-81679 München, Germany
    2. Cluster of Excellence ‘Origin and Structure of the Universe’, Boltzmannstr. 2, 85748 Garching, Germany
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E-mail: lspezzi@rssd.esa.int

ABSTRACT

We present a multiwavelength study of three star-forming regions, spanning the age range 1–14 Myr, located between the 30 Doradus complex and supernova SN 1987A in the Large Magellanic Cloud (LMC). We reliably identify about 1000 pre-main-sequence (PMS) star candidates actively undergoing mass accretion and estimate their stellar properties and mass accretion rate (inline image). Our measurements represent the largest inline image data set of low-metallicity stars presented so far. As such, they offer a unique opportunity to study on a statistical basis the mass accretion process in the LMC and, more in general, the evolution of the mass accretion process around low-metallicity stars. We find that the typical inline image of PMS stars in the LMC is higher than for galactic PMS stars of the same mass, independently of their age. Taking into account the caveats of isochronal age and inline image estimates, the difference in inline image between the LMC and our Galaxy appears to be about an order of magnitude. We review the main mechanisms of disc dispersal and find indications that typically higher inline image are to be expected in low-metallicity environments. However, many issues of this scenario need to be clarified by future observations and modelling. We also find that, in the mass range 1–2 M, inline image of PMS stars in the LMC increases with stellar mass as inline image, with b≈ 1, i.e. slower than the second power law found for galactic PMS stars in the same mass regime.

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