Home News About Us Contact Contributors Disclaimer Privacy Policy Help FAQ

Quick Search
My eDoc
Session History
Support Wiki
Direct access to
document ID:

          Institute: MPI für Radioastronomie     Collection: Publikationen des MPI für Radioastronomie     Display Documents

ID: 12245.0, MPI für Radioastronomie / Publikationen des MPI für Radioastronomie
Systematic molecular differentiation in starless cores
Authors:Tafalla, M.; Myers, P. C.; Caselli, P.; Walmsley, C. M.; Comito, C.
Date of Publication (YYYY-MM-DD):2002-04-20
Title of Journal:Astrophysical Journal
Journal Abbrev.:Astrophys. J.
Issue / Number:2
Start Page:815
End Page:835
Review Status:Peer-review
Audience:Experts Only
Abstract / Description:We present evidence that low-mass starless cores, the simplest units of star formation, are systematically differentiated in their chemical composition. Some molecules, including CO and CS, almost vanish near the core centers, where the abundance decreases by at least 1 or 2 orders of magnitude with respect to the value in the outer core. At the same time, the N2H+ molecule has a constant abundance, and the fraction of NH3 increases toward the core center. Our conclusions are based on a systematic study of five mostly round starless cores ( L1498, L1495, L1400K, L1517B, and L1544), which we have mapped in (CO)-O-18 (1-0), CS (2-1), N2H+ (1-0), NH3 (1, 1) and (2, 2), and the 1.2 mm continuum [ complemented with (CO)-O-17 (1-0) and (CS)-S-34 (2-1) data for some systems]. For each core we have built a spherically symmetric model in which the density is derived from the 1.2 mm continuum, the kinetic temperature is derived from NH3, and the abundance of each molecule is derived using a Monte Carlo radiative transfer code, which simultaneously fits the shape of the central spectrum and the radial pro le of integrated intensity. Regarding the cores for which we have (CO)-O-17 (1-0) and (CS)-S-34 (2-1) data, the model fits these observations automatically when the standard isotopomer ratio is assumed. As a result of this modeling, we also find that the gas kinetic temperature in each core is constant at approximately 10 K. In agreement with previous work, we find that if the dust temperature is also constant, then the density profiles are centrally flattened, and we can model them with a single analytic expression. We also find that for each core the turbulent line width seems constant in the inner 0.1 pc. The very strong abundance drop of CO and CS toward the center of each core is naturally explained by the depletion of these molecules onto dust grains at densities of (2-6) 10(4) cm(-3). N2H+ seems unaffected by this process up to densities of several times 10(5) cm(-3), or even 10(6) cm(-3), while the NH3 abundance may be enhanced by its lack of depletion and by reactions triggered by the disappearance of CO from the gas phase. With the help of the Monte Carlo modeling, we show that chemical differentiation automatically explains the discrepancy between the sizes of CS and NH3 maps, a problem that has remained unexplained for more than a decade. Our models, in addition, show that a combination of radiative transfer effects can give rise to the previously observed discrepancy in the line width of these two tracers. Although this discrepancy has been traditionally interpreted as resulting from a systematic increase of the turbulent line width with radius, our models show that it can arise in conditions of constant gas turbulence.
Free Keywords:ISM : abundances; ISM : clouds; ISM : molecules; stars : formation
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Radioastronomie
External Affiliations:Observ Astron Nacl, Alfonso XII 3, E-28014 Madrid, Spain; Observ Astron Nacl, E-28014 Madrid, Spain; Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA; Osserv Astrofis Arcetri, I-50125 Florence, Italy; Max Planck Inst Radioastron, D-53121 Bonn, Germany
The scope and number of records on eDoc is subject to the collection policies defined by each institute - see "info" button in the collection browse view.