SpringerLink
Forum Springer Astron. Astrophys.
Forum Whats New Search Orders


Astron. Astrophys. 329, 1028-1034 (1998)

Next Section Table of Contents

HST - GHRS observations of CO and CI in the [FORMULA]-Pictoris circumstellar disk*

A. Jolly 1, J.B. McPhate 2, A. Lecavelier 3, A.M. Lagrange 4, J.L. Lemaire 1, 5, P.D. Feldman 2, A. Vidal Madjar 3, R. Ferlet 3, D. Malmasson 1 and F. Rostas 1

1 DAMAP et URA 812 du CNRS, Observatoire de Paris-Meudon, F-92195 Meudon Cedex, France
2 Department of Physics and Astronomy, Johns Hopkins University, Baltimore, Maryland 21218, USA
3 Institut d'Astrophysique de Paris, CNRS, 98bis Bd Arago, F-75014 Paris, France
4 Grouped'Astrophysique de Grenoble, CERMO BP53X, F-38041 Grenoble Cedex, France
5 Université de Cergy-Pontoise, 33 Bd du Port, F-95011 Cergy-Pontoise, France

Received 1 April 1997 / Accepted 11 July 1997

Abstract

GHRS-EchA and G160M spectra of [FORMULA] -Pictoris have been obtained in the 1400-1600 Å range. A detailed analysis of the CO A-X (0-0, 1-0, 2-0) bands and of the CI [FORMULA] 1561 Å multiplet is presented. A column density of the order of 2 1015 cm-2 is found for both species. For CO, the rotational temperature is found close to 20 K and the turbulent Doppler width is b=0.8 km.s-1. Including the 13 CO lines in the fit allows an estimate of the 13 CO abundance: R=12 CO/13 CO=20. This anomalous ratio is tentatively interpreted as being due to chemical fractionation. For the CI triplet, the absorption profile is best fitted by a combination of four velocity components matching those observed independently at the same moment from ground in the CaII H and K lines. The most intense component corresponds to zero relative velocity while the others are shifted by 3 to 10 km s-1. The large turbulent width of the components (4.2 km s-1), the statistical population of the ground state fine structure levels and the similar column densities of CI and CO are interpreted as indicating that CI is formed by photodissociation of CO and destroyed by photoionization. The velocity structure would then indicate that part of CI is formed at large distance ([FORMULA] 100 AU) from CO evaporating from cometary bodies while another part originates closer to the star from fast moving cometary bodies with high excentricity.

Key words: stars: circumstellar matter – stars: fi-Pictoris

* Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute which is operated by the Association of Universities for Research in Astronomy Inc., under NASA Contract NAS5-26555.

Send offprint requests to: F. Rostas

SIMBAD Objects

Contents

Next Section Table of Contents

© European Southern Observatory (ESO) 1998

Online publication: December 16, 1997
helpdesk.link@springer.de