Differences in chemical evolution between isolated and embedded prestellar cores
arXiv:2211.12529 · doi:10.1093/mnras/stac3444
Abstract
Models of prestellar cores often assume that the cores are isolated from their environment - material outside the core boundary plays no role in the subsequent evolution. This is unlikely to be the case in reality, where cores are located within hierarchically substructured molecular clouds. We investigate the dynamical and chemical evolution of prestellar cores, modelled as Bonnor-Ebert spheres, and show that the density of the ambient medium has a large impact on the resulting chemical properties of the cores. Models embedded in high-density, low-temperature surroundings have greatly enhanced abundances of several molecules, such as CO and CS, compared to models with more diffuse surroundings, corresponding to relatively isolated cores. The predicted intensities and profile shapes of molecular lines are also affected. The density of the ambient medium has a stronger effect on the chemical evolution than whether the cores are initially in or out of equilibrium. This suggests that the impact of environment cannot be neglected when modelling chemistry in prestellar cores; the results of these models are highly sensitive to the assumptions made about the core surroundings.
arXiv comment7 pages, 5 figures. MNRAS accepted
References in corpus (26)
- Control of star formation by supersonic turbulence
- An atomic and molecular database for analysis of submillimetre line observations
- Cold Dark Clouds: The Initial Conditions for Star Formation
- The UMIST database for astrochemistry 2012
- Competitive accretion in embedded stellar cluster
- Systematic Molecular Differentiation in Starless Cores
- Phantom: A smoothed particle hydrodynamics and magnetohydrodynamics code for astrophysics
- LIME - a flexible, non-LTE line excitation and radiation transfer method for millimeter and far-infrared wavelengths
- Molecular Evolution in Collapsing Prestellar Cores III: Contraction of A Bonnor-Ebert Sphere
- A Survey for Infall Motions toward Starless Cores. I. CS (2-1) and NH (1-0) Observations
- UCLCHEM: A Gas-Grain Chemical Code
- The dynamics of collapsing cores and star formation
- Smoothed Particle Hydrodynamics simulations of expanding HII regions. I. Numerical methods and tests
- Line Profiles of Cores within Clusters: I. The Anatomy of a Filament
- Line Profiles of Cores within Clusters: II Signatures of Dynamical Collapse during High Mass Star Formation
- An ALMA study of hub-filament systems I. On the clump mass concentration within the most massive cores
- Hydrodynamics with gas-grain chemistry and radiative transfer: comparing dynamical and static models
- Non-Equilibrium Chemistry of Dynamically Evolving Prestellar Cores: I. Basic Magnetic and Non-Magnetic Models and Parameter Studies
- The accretion history of high-mass stars: An ArTéMiS pilot study of Infrared Dark Clouds
- GASTON: Galactic Star Formation with NIKA2. Evidence for the mass growth of star-forming clumps
- On the role of ambient environments in the collapse of Bonnor-Ebert spheres
- On the emergent System Mass Function: the contest between accretion and fragmentation
- Timescales for Low-Mass Star Formation in Extragalactic Environments: Implications for the Stellar IMF
- Non-ideal MHD simulations of subcritical prestellar cores with non-equilibrium chemistry
- Investigating the role of magnetic fields in star formation using molecular line profiles
- The initial magnetic criticality of prestellar cores