On the internal structure of starless cores. I. Physical conditions and the distribution of CO, CS, N2H+, and NH3 in L1498 and L1517B

Details On the internal structure of starless cores. I. Physical conditions and the distribution of CO, CS, N2H+, and NH3 in L1498 and L1517B On the internal structure of starless cores. I. Physical conditions and the distribution of CO, CS, N2H+, and NH3 in L1498 and L1517B

2004-01-09

arxiv.org/abs/astro-ph/0401148v3

Astrophys.Space Sci. 292 (2004) 347-354; Astron.Astrophys. 416 (2004) 191-212

Astronomy and Astrophysics

Astrophysics

A&A accepted. 23 pages, 15 figures. v2: Minor typos corrected. v3: additional clarifications on turbulent models; final journa

Scientific paper

10.1023/B:ASTR.0000045036.76044.

We have characterized the physical structure and chemical composition of two close-to-round starless cores in Taurus-Auriga, L1498 and L1517B. Our analysis is based on high angular resolution observations in at least two transitions of NH3, N2H+, CS, C34S, C18O, and C17O, together with maps of the 1.2 mm continuum. For both cores, we derive radial profiles of constant temperature and constant turbulence, together with density distributions close to those of non-singular isothermal spheres. Using these physical conditions and a Monte Carlo radiative transfer model, we derive abundance profiles for all species and model the strong chemical differentiation of the core interiors. According to our models, the NH3 abundance increases toward the core centers by a factor of several while N2H+ has a constant abundance over most of the cores. In contrast, both C18O and CS (and isotopomers) are strongly depleted in the core interiors, most likely due to their freeze out onto grains at densities of a few 10^4 cm^{-3}. Concerning the kinematics of the dense gas, we find (in addition to constant turbulence) a pattern of internal motions at the level of 0.1 km s^{-1}. These motions seem correlated with asymmetries in the pattern of molecular depletion, and we interpret them as residuals of core contraction. Their distribution and size suggest that core formation occurs in a rather irregular manner and with a time scale of a Myr. A comparison of our derived core properties with those predicted by supersonic turbulence models of core formation shows that our Taurus cores are much more quiescent than representative predictions from these models.

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