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Hubble Space Telescope Measures of Mass Accretion Rates in the Orion Nebula Cluster

Manara, C. F. and Robberto, M. and Rio, N. Da and Hillenbrand, L. A. and Stassun, K. G. and Soderblom, D. R. (2012) Hubble Space Telescope Measures of Mass Accretion Rates in the Orion Nebula Cluster. Astrophysical Journal, 755 (2). Art. No. 154. ISSN 0004-637X. doi:10.1088/0004-637X/755/2/154. https://resolver.caltech.edu/CaltechAUTHORS:20121101-104124563

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Abstract

The present observational understanding of the evolution of the mass accretion rates (Ṁ_acc) in pre-main-sequence stars is limited by the lack of accurate measurements of Ṁ_acc over homogeneous and large statistical samples of young stars. Such observational effort is needed to properly constrain the theory of star formation and disk evolution. Based on Hubble Space Telescope/WFPC2 observations, we present a study of Ṁ_acc for a sample of ~700 sources in the Orion Nebula Cluster, ranging from the hydrogen-burning limit to M_* ~ 2 M_☉. We derive Ṁ_acc from both the U-band excess and the Hα luminosity (L_Hα), after determining empirically both the shape of the typical accretion spectrum across the Balmer jump and the relation between the accretion luminosity (L acc) and L_Hα, which is L_acc/L_☉ = (1.31 ± 0.03) ⋅ L_Hα/L_☉ + (2.63 ± 0.13). Given our large statistical sample, we are able to accurately investigate relations between Ṁ_acc and the parameters of the central star such as mass and age. We clearly find Ṁ_acc to increase with stellar mass and decrease over evolutionary time, but we also find strong evidence that the decay of Ṁ_acc with stellar age occurs over longer timescales for more massive PMS stars. Our best-fit relation between these parameters is given by log(Ṁ_acc)/M_☉ yr) = (–5.12 ± 0.86) – (0.46 ± 0.13) ⋅ log(t/yr) – (5.75 ± 1.47) ⋅ log(M */M ☉) + (1.17 ± 0.23) ⋅ log(t/yr) ⋅ log(M_*/M_☉). These results also suggest that the similarity solution model could be revised for sources with M_* ≳ 0.5 M_☉. Finally, we do not find a clear trend indicating environmental effects on the accretion properties of the sources.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/0004-637X/755/2/154DOIArticle
http://iopscience.iop.org/0004-637X/755/2/154PublisherArticle
ORCID:
AuthorORCID
Manara, C. F.0000-0003-3562-262X
Stassun, K. G.0000-0002-3481-9052
Soderblom, D. R.0000-0002-0322-8161
Additional Information:© 2012 American Astronomical Society. Received 2012 May 3; accepted 2012 June 19; published 2012 August 6. This work was made possible by GO program 10246 of the Hubble Space Telescope, which is operated by the Space Telescope Science Institute. C.F.M. thanks James Pringle and Philip J. Armitage for insightful discussions. Facility: HST (WFPC2)
Funders:
Funding AgencyGrant Number
Hubble Space TelescopeGO 10246
Space Telescope Science InstituteUNSPECIFIED
Subject Keywords:accretion, accretion disks; protoplanetary disks; stars: formation; stars: pre-main sequence
Issue or Number:2
DOI:10.1088/0004-637X/755/2/154
Record Number:CaltechAUTHORS:20121101-104124563
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20121101-104124563
Official Citation:Hubble Space Telescope Measures of Mass Accretion Rates in the Orion Nebula Cluster C. F. Manara et al. 2012 ApJ 755 154
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:35239
Collection:CaltechAUTHORS
Deposited By: Jason Perez
Deposited On:01 Nov 2012 20:29
Last Modified:09 Nov 2021 23:13

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