Astrochemical confirmation of the rapid evolution of massive YSOs and explanation for the inferred ages of hot cores

  title={Astrochemical confirmation of the rapid evolution of massive YSOs and explanation for the inferred ages of hot cores},
  author={Steven D. Doty and E. F. van Dishoeck and J. C. Tan},
  journal={Astronomy and Astrophysics},
Aims. To understand the roles of infall and protostellar evolution on the envelopes of massive young stellar objects (YSOs). Methods. The chemical evolution of gas and dust is traced, including infall and realistic source evolution. The temperatures are determined self-consistently. Both ad/desorption of ices using recent laboratory temperature-programmed-desorption measurements are included. Results. The observed water abundance jump near 100 K is reproduced by an evaporation front which moves… 

Figures from this paper

Energetic radiation and the sulfur chemistry of protostellar envelopes: Submillimeter interferometry of AFGL 2591
Context. The chemistry in the inner few thousand AU of accreting envelopes around young stellar objects is predicted to vary greatly with far-UV and X-ray irradiation by the central star. Aims. We
The Herschel Space Observatory enables observations in the far-infrared at high spectral and spatial resolution. A particular class of molecules will be directly observable: light diatomic hydrides
The Raw Material of Cluster Formation: Observational Constraints
Hydrodynamical simulations of star cluster formation trace the conversion of gas into stars and it is thus important that the initial conditions of such simulations are informed by observations of
Upcoming facilities such as the Herschel Space Observatory or Atacama Large Millimeter Array will deliver a wealth of molecular line observations of young stellar objects (YSOs). Based on line
The SOFIA Massive (SOMA) Star Formation Survey: I. Overview and First Results
We present an overview and first results of the Stratospheric Observatory For Infrared Astronomy Massive (SOMA) Star Formation Survey, which is using the FORCAST instrument to image massive
Modeling the water line emission from the high-mass star-forming region AFGL 2591
Context. Observations of water lines are a sensitive probe of the geometry, dynamics and chemical structure of dense molecular gas. The launch of Herschel with on board HIFI and PACS allows to probe
Massive star formation exhibits an extremely rich chemistry. However, few evolutionary details are known yet, especially at high spatial resolution. Therefore, we synthesize previously published
Chemical complexity in high-mass star formation
Aims. In order to understand the observed molecular diversity in high-mass star-forming regions, we have to determine the underlying physical and chemical structure of those regions at high angular
Multidimensional Chemical Modeling of Young Stellar Objects. II. Irradiated Outflow Walls in a High-Mass Star-Forming Region
Observations of the high-mass star-forming region AFGL 2591 reveal a large abundance of CO+, a molecule known to be enhanced by far-ultraviolet (FUV) and X-ray irradiation. In chemical models
Evolution of complex organic molecules in hot molecular cores: Synthetic spectra at (sub-)mm wavebands
Hot molecular cores (HMCs) are intermediate stages of high-mass star formation and are also known for their rich emission line spectra at (sub-)mm wavebands. The observed spectral feature of HMCs


Chemical Evolution in Protostellar Envelopes: Cocoon Chemistry
We have modeled the chemistry that occurs in the envelopes surrounding newborn stars as they are gradually heated by the embedded protostar and the ice mantles of dust grains evaporate, resulting in
Evolution of Chemistry and Molecular Line Profiles during Protostellar Collapse
Understanding the chemical evolution in star-forming cores is a necessary precondition to correctly assessing physical conditions when using molecular emission. We follow the evolution of chemistry
Structure and Evolution of the Envelopes of Deeply Embedded Massive Young Stars
The physical structure of the envelopes around a sample of 14 massive young stars is investigated using maps and spectra in submillimeter continuum and lines of C^(17)O, CS, C^(34)S, and H_2CO. Nine
Evaporation of ices near massive stars: models based on laboratory temperature programmed desorption data
Hot cores and their precursors contain an integrated record of the physics of the collapse process in the chemistry of the ices deposited during that collapse. In this paper, we present results from
Abundant gas-phase H2O in absorption toward massive protostars ?
We present infrared spectra of gas-phase H 2 O around 6  μ m toward 12 deeply embedded massive protostars obtained with the Short Wavelength Spectrometer on board the Infrared Space Observatory
Chemistry as a probe of the structures and evolution of massive star-forming regions
We present detailed thermal and gas-phase chemical models for the envelope of the massive star-forming region AFGL 2591. By considering both time- and space-dependent chemistry, these models are used
Chemical differentiation between star-forming regions : the Orion Hot Core and Compact Ridge
We present a dynamical-chemical model of massive star-forming regions, in which gas and dust grains are included. We consider the last 10 5 . yr of the accretion phase of a protostellar object
Water in the envelopes and disks around young high-mass stars
Single-dish spectra and interferometric maps of (sub-)millimeter lines of H 18 2 O and HDO are used to study the chemistry of water in eight regions of high-mass star formation. The spectra indicate
The Physical and Chemical Structure of Hot Molecular Cores
We have made self-consistent models of the density and temperature profiles of the gas and dust surrounding embedded luminous objects using a detailed radiative transfer model together with
Thermal desorption of water ice in the interstellar medium
Water (H2O) ice is an important solid constituent of many astrophysical environments. To comprehend the role of such ices in the chemistry and evolution of dense molecular clouds and comets, it is