Volume 574, February 2015
|Number of page(s)||15|
|Section||Interstellar and circumstellar matter|
|Published online||28 January 2015|
The HIFI spectral survey of AFGL 2591 (CHESS)
III. Chemical structure of the protostellar envelope⋆
1 SRON Netherlands Institute for Space Research, Landleven 12, 9747 AD Groningen, The Netherlands
2 Max-Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany
3 Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, The Netherlands
4 Universidad de Chile, Camino del Observatorio 1515, Las Condes, Santiago, Chile
5 Institute for Space Imaging Science, Department of Physics & Astronomy, University of Lethbridge, Lethbridge AB, Canada
Received: 23 July 2014
Accepted: 4 December 2014
Aims. The aim of this work is to understand the richness of chemical species observed in the isolated high-mass envelope of AFGL 2591, a prototypical object for studying massive star formation.
Methods. Based on HIFI and JCMT data, the molecular abundances of species found in the protostellar envelope of AFGL 2591 were derived with a Monte Carlo radiative transfer code (Ratran), assuming a mixture of constant and 1D stepwise radial profiles for abundance distributions. The reconstructed 1D abundances were compared with the results of the time-dependent gas-grain chemical modeling, using the best-fit 1D power-law density structure. The chemical simulations were performed considering ages of 1−5 × 104 years, cosmic ray ionization rates of 5−500 × 10-17 s-1, uniformly-sized 0.1−1 μm dust grains, a dust/gas ratio of 1%, and several sets of initial molecular abundances with C/O < 1 and >1. The most important model parameters varied one by one in the simulations are age, cosmic ray ionization rate, external UV intensity, and grain size.
Results. Constant abundance models give good fits to the data for CO, CN, CS, HCO+, H2CO, N2H+, CCH, NO, OCS, OH, H2CS, O, C, C+, and CH. Models with an abundance jump at 100 K give good fits to the data for NH3, SO, SO2, H2S, H2O, HCl, and CH3OH. For HCN and HNC, the best models have an abundance jump at 230 K. The time-dependent chemical model can accurately explain abundance profiles of 15 out of these 24 species. The jump-like radial profiles for key species like HCO+, NH3, and H2O are consistent with the outcome of the time-dependent chemical modeling. The best-fit model has a chemical age of ~10−50 kyr, a solar C/O ratio of 0.44, and a cosmic-ray ionization rate of ~5 × 10-17 s-1. The grain properties and the intensity of the external UV field do not strongly affect the chemical structure of the AFGL 2591 envelope, whereas its chemical age, the cosmic-ray ionization rate, and the initial abundances play an important role.
Conclusions. We demonstrate that simple constant or jump-like abundance profiles constrained with 1D Ratran line radiative transfer simulations are in agreement with time-dependent chemical modeling for most key C-, O-, N-, and S-bearing molecules. The main exceptions are species with very few observed transitions (C, O, C+, and CH) or with a poorly established chemical network (HCl, H2S) or whose chemistry is strongly affected by surface processes (CH3OH).
Key words: ISM: individual objects: AFGL 2591 / stars: formation / ISM: abundances / ISM: molecules / evolution / submillimeter: ISM
© ESO, 2015
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.