EDP Sciences
Free Access
Issue
A&A
Volume 439, Number 1, August III 2005
Page(s) 195 - 203
Section Interstellar and circumstellar matter
DOI https://doi.org/10.1051/0004-6361:20052792


A&A 439, 195-203 (2005)
DOI: 10.1051/0004-6361:20052792

Line profiles of molecular ions toward the pre-stellar core LDN 1544

F. F. S. van der Tak1, P. Caselli2 and C. Ceccarelli3

1  Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
    e-mail: vdtak@mpifr-bonn.mpg.de
2  INAF - Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy
3  Laboratoire Astrophysique de l'Observatoire de Grenoble, BP 53, 38041 Grenoble, France

(Received 31 January 2005 / Accepted 28 April 2005)

Abstract
Velocity profiles of ground state lines of H2D+, HC18O+ and N2H+, observed previously with the CSO and IRAM 30 m telescopes, are modeled with a Monte Carlo radiative transfer program to study the temperature, density and velocity structure of the pre-stellar core LDN 1544. The H2D+ line is double-peaked like that of the other ions, but previous models that fit the HC18O+ and N2H+ profiles are found not to fit the H2D+ data. Matching the H2D+ observations requires at least three modifications to the model at small radii: (1) the density profile must continue to rise inward and not flatten off toward the center; (2) the gas temperature must be nearly constant and not drop inwards significantly; (3) the infall velocity must increase inward, in a fashion intermediate between "quasi-static" (ambipolar diffusion) and "fully dynamic" (Larson-Penston) collapse. The C18O emission indicates a chemical age of $\la$0.1 Myr. The effects of a flattened structure and rotation on the line profiles are shown to be unimportant, at least on the scales probed by single-dish telescopes. Alternatively, the H2D+ profile is affected by absorption in the outer layers of the core, if gas motions in these layers are sufficiently small.


Key words: ISM: molecules -- circumstellar matter -- stars: formation -- astrochemistry -- molecular processes -- line: profiles

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© ESO 2005

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