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Astron. Astrophys. 345, 181-186 (1999)

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The ISO spectrum of the young star HD 142527 *

K. Malfait 1, C. Waelkens 1, J. Bouwman 2, A. De Koter 2 and L.B.F.M. Waters 2

1 Instituut voor Sterrenkunde, K.U.Leuven, Celestijnenlaan 200B, B-3001 Leuven, Belgium
2 Astronomical Institute `Anton Pannekoek', University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands

Received 21 October 1998 / Accepted 16 February 1999

Abstract

We present a detailed analysis of SWS (2.35-45 µm) and LWS (43-200 µm) spectra obtained with the Infrared Space Observatory (ISO) (Kessler et al. 1996) of the dusty circumstellar disk surrounding the isolated young Fe star HD 142527. Two dust populations can be clearly discriminated: a warm component which is dominated by very strong silicate emission at 10 µm, but in which C-rich dust is observable as well, and a cool component, of which the spectrum is dominated by O-rich dust features (C-rich dust not cause obvious features in the far infrared). Besides silicates, crystalline water-ice and hydrous silicates - which are also found in interplanetary dust particles - are present in the cold circumstellar environment. The ISO spectrum of HD 142527 differs markedly from that of HD 100546 (Malfait et al. 1998b) and other objects in a similar evolutionary stage and with a similar broad-band energy distribution. No clear correlations between the spectral dust signatures and the stellar parameters can be found at the present stage.

Key words: stars: circumstellar matter – stars: individual: HD 142527 – infrared: ISM: lines and bands – inteplanetary medium

* Based on observations with ISO, an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, the Netherlands and the United Kingdom) and with the participation of ISAS and NASA

Send offprint requests to: Koen Malfait, Leuven (koenm@ster.kuleuven.ac.be)

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© European Southern Observatory (ESO) 1999

Online publication: April 12, 1999
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