EDP Sciences
Free Access
Volume 433, Number 3, April III 2005
Page(s) 1047 - 1054
Section Stellar structure and evolution
DOI https://doi.org/10.1051/0004-6361:20042019
Published online 29 March 2005

A&A 433, 1047-1054 (2005)
DOI: 10.1051/0004-6361:20042019

A survey for Fe 6.4 keV emission in young stellar objects in $\mathsf{\rho}$ Oph: The strong fluorescence from Elias 29

F. Favata1, G. Micela2, B. Silva1, S. Sciortino2 and M. Tsujimoto3

1  Astrophysics Division - Research and Science Support Department of ESA, ESTEC, Postbus 299, 2200 AG Noordwijk, The Netherlands
    e-mail: Fabio.Favata@rssd.esa.int
2  INAF - Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy
3  Department of Astronomy and Astrophysics - Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802, USA

(Received 15 September 2004 / Accepted 13 December 2004 )

We report the results of a search for 6.4 keV Fe fluorescent emission in Young Stellar Objects (YSOs) with measured accretion luminosities in the $\rho$ Oph cloud, using the existing Chandra and XMM-Newton observations of the region. A total of nine such YSOs have X-ray data with sufficiently high S/N for the 6.4 keV line to be potentially detected if present. A positive detection of the Fe 6.4 keV line is reported for one object, Elias 29, in both the XMM-Newton and the Chandra data. The 6.4 keV line is detected in Elias 29 both during quiescent and flaring emission, unlikely all previously reported detections of 6.4 keV Fe fluorescence in YSOs which were made during intense flaring. The observed equivalent width of the fluorescent line is large, $W_\alpha \simeq 160$ eV, ruling out fluorescence from diffuse circumstellar material. It is also larger than expected for simple reflection from a solar-composition photosphere or circumstellar disk, but it is compatible with being due to fluorescence from a centrally illuminated circumstellar disk. The X-ray spectrum of Elias 29 is also peculiar in terms of its high (ionized) Fe abundance, as evident from the very intense Fe XXV 6.7 keV line emission; we speculate on the possible mechanism leading to the observed high abundance.

Key words: stars: coronae -- stars: formation -- stars: individual: Elias 29 -- stars: individual: $\rho$ Oph

SIMBAD Objects

© ESO 2005

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