Home News About Us Contact Contributors Disclaimer Privacy Policy Help FAQ

Home
Search
Quick Search
Advanced
Fulltext
Browse
Collections
Persons
My eDoc
Session History
Login
Name:
Password:
Documentation
Help
Support Wiki
Direct access to
document ID:


          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



ID: 308621.0, MPI für Astronomie / Publikationen_mpia
CB 17: Inferring the dynamical history of a prestellar core with chemodynamical models
Authors:Pavlyuchenkov, Y.; Wiebe, D.; Launhardt, R.; Henning, T.
Date of Publication (YYYY-MM-DD):2006
Journal Abbrev.:The Astrophysical Journal
Volume:645
Start Page:1212
End Page:1226
Audience:Not Specified
Abstract / Description:We present a detailed theoretical study of the isolated Bok globule CB 17 (L1389) based on spectral maps of CS, HCO+, C18O, C34S, and H13CO+ lines. The intensity of the external UV field, the probability for molecules to stick onto dust grains, the core age, the infall, and rotation velocity all significantly affect the molecular line spectra. We demonstrate that these parameters are well constrained when results of the modeling are compared to observations in multiple lines of sight through the core. We use a detailed chemical model to compute the time-dependent abundances in a number of locations within the core. Both static and dynamically evolving cloud configurations are considered. These abundances are then used to simulate the spectral maps. We developed a general criterion that allows us to quantify the difference between observed and simulated spectral maps. By minimizing this difference, we isolate the model that represents a good approximation to the core chemical and kinematic structure. The chemical age of the core is about 2 Myr, while the most probable effective sticking probability value is 0.3-0.5. The spatial distribution of intensities and self-absorption features of optically thick lines is indicative of attenuated UV radiation of the core. The line asymmetry pattern in CB 17 is reproduced by a combination of infall, rotation, and turbulent motions with velocities of ~0.05, ~0.1, and ~0.1 km s-1, respectively. These parameters correspond to energy ratios Erot/Egrav~0.03, Etherm/Egrav~0.8, and Eturb/Egrav~0.05 (the rotation parameters are determined for i=90deg). Based on the angular momentum value, we argue that the core is going to fragment, i.e., to form a binary (multiple) system.
Free Keywords:Astrochemistry; ISM: individual (CB 17); ISM: Molecules; Line: Profiles; Stars: Formation
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:URL:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bi...
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.