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Circumstellar Disks in the Orion Nebula Cluster

Hillenbrand, Lynne A. and Strom, Stephen E. and Calvet, Nuria and Merrill, K. Michael and Gatley, Ian and Makidon, Russell B. and Meyer, Michael R. and Skrutskie, Michael F. (1998) Circumstellar Disks in the Orion Nebula Cluster. Astronomical Journal, 116 (4). pp. 1816-1841. ISSN 0004-6256. https://resolver.caltech.edu/CaltechAUTHORS:20170801-141657805

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Abstract

We combine our previous optical spectroscopic and photometric analysis of ~1600 stars located in the Orion Nebula Cluster (ONC) with our own and published near-infrared photometric surveys of the region in order to investigate the evidence for and properties of circumstellar disks. We use the near-infrared continuum excess as our primary disk diagnostic, although we also study sources with Ca II triplet emission and those designated as "proplyds." The measured near-infrared excess is influenced by (1) the presence or absence of a circumstellar disk, (2) the relative importance of disk accretion and inner disk holes, (3) the relative contrast between photospheric and disk emission, and (4) system inclination. After attempting to understand the effects of these influences, we estimate the frequency of circumstellar disks and discuss the evidence for trends in the disk frequency with stellar mass (over the mass range <0.1–50 M_⊙), stellar age (over the age range <0.1–2 Myr), and projected cluster radius (over the radial range 0–3 pc). We find that the fraction of stars retaining their inner (<0.1 AU) circumstellar disks to the present time is at least 55% and probably no more than 90%, averaged over the entire range in stellar mass and stellar age represented in the ONC and over the entire area of our survey. We find no trend in the disk fraction with stellar age, at least not over the limited age range of the cluster. We find that more massive stars are less likely to have disks, consistent with a scenario in which the evolutionary timescales are more rapid for disks surrounding more massive stars than for disks surrounding less massive stars. We also find that the disk frequency begins to decrease toward the lowest masses, although objects of all masses (including those that appear to be substellar) can have disks. We find that the disk frequency increases toward the cluster center. We then argue, using several lines of evidence, that a large fraction of the disks associated with stars in the ONC are accretion disks. The observed trends with stellar age, stellar mass, and projected cluster radius in the disk frequency may, in fact, be driven primarily by trends in the disk accretion properties. From the magnitude of the near-infrared excess above that expected from pure irradiation disks, we find an accretion disk fraction among the stars identified as having disks of 61%–88%. In addition, approximately 20% of the stars in our optical spectroscopic sample show broad (several hundred km s^(-1) FWHM) Ca II emission lines, which are features often associated with accretion disk/wind phenomena; another 50% of the sample have Ca II lines that (at our spectral resolution) are "filled in," indicating an independently derived accretion disk frequency of ~70%. Finally, we discuss the near-infrared and optical emission-line properties of that portion of our sample identified from Hubble Space Telescope imaging as having a dark silhouette or an externally ionized structure. This sample, proposed in the literature to have accretion disks, appears to be no different in terms of its stellar or circumstellar properties from the rest of the ONC population. The only feature distinguishing these objects from their ONC siblings thus may be their current (but short-lived) proximity to the massive stars near the cluster center.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1086/300536DOIArticle
http://iopscience.iop.org/article/10.1086/300536PublisherArticle
ORCID:
AuthorORCID
Calvet, Nuria0000-0002-3950-5386
Meyer, Michael R.0000-0003-1227-3084
Additional Information:© 1998 American Astronomical Society. Received 1998 February 3. Accepted 1998 May 27. We thank J. Carpenter for insightful comments on a draft of this manuscript and an anonymous referee for a careful review of our work. Support to L. A. H. for this work was provided by NASA through grant HF1060.01-94A from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Publication of this work was supported by a grant to L. A. H. from NASA administered by the American Astronomical Society and from NASA Origins of Solar Systems grant NAG 5-7501. Support to N. C. was provided by NASA grants NAGW-2306 and NAG5-4282
Funders:
Funding AgencyGrant Number
NASAHF1060.01-94A
NASANAS5-26555
NASANAG 5-7501
NASANAGW-2306
NASANAG5-4282
Subject Keywords:galaxies: open clusters and associations; stars: circumstellar matter; stars: formation; stars: pre-main sequence
Issue or Number:4
Record Number:CaltechAUTHORS:20170801-141657805
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20170801-141657805
Official Citation:Lynne A. Hillenbrand et al 1998 AJ 116 1816
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:79702
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:01 Aug 2017 22:21
Last Modified:09 Mar 2020 13:19

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