Please note that eDoc will be permanently shut down in the first quarter of 2021!      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 Astronomie     Collection: Publikationen_mpia     Display Documents

ID: 607202.0, MPI für Astronomie / Publikationen_mpia
Hot HCN around young massive stars at 0.1'' resolution
Authors:Rolffs, R.; Schilke, P.; Wyrowski, F.; Dullemond, C.; Menten, K. M.; Thorwirth, S.; Belloche, A.
Date of Publication (YYYY-MM-DD):2011
Journal Abbrev.:Astronomy and Astrophysics
Audience:Not Specified
Abstract / Description:Massive stars form deeply embedded in dense molecular gas, which they stir and heat up and ionize. During an early phase, the ionization is confined to hypercompact Hii regions, and the stellar radiation is entirely absorbed by dust, giving rise to a hot molecular core. To investigate the innermost structure of such high-mass star-forming regions, we observed vibrationally excited HCN (via the direct â„“-type transition of v2 = 1, ΔJ = 0, J = 13, which lies 1400 K above ground) toward the massive hot molecular cores G10.47+0.03, SgrB2-N, and SgrB2-M with the Very Large Array (VLA) at 7 mm, reaching a resolution of about 1000 AU (0.1''). We detect the line both in emission and in absorption against Hii regions. The latter allows to derive lower limits on the column densities of hot HCN, which are several times 1019 cm-2. We see indication of expansion motions in G10.47+0.03 and detect velocity components in SgrB2-M at 50, 60, and 70 km s-1 relative to the Local Standard of Rest. The emission originates in regions of less than 0.1 pc diameter around the hypercompact Hii regions G10.47+0.03 B1 and SgrB2-N K2, and reaches brightness temperatures of more than 200 K. Using the three-dimensional radiative transfer code RADMC-3D, we model the sources as dense dust cores heated by stars in the Hii regions, and derive masses of hot (>300 K) molecular gas of more than 100 solar masses (for an HCN fractional abundance of 10-5), challenging current simulations of massive star formation. Heating only by the stars in the Hii regions is sufficient to produce such large quantities of hot molecular gas, provided that dust is optically thick to its own radiation, leading to high temperatures through diffusion of radiation.
Free Keywords:ISM: molecules; ISM: structure; ISM: clouds; stars: formation
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
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.