A grid of 1D low-mass star formation collapse models

Abstract

The current study was developed to provide a database of relatively simple numerical simulations of protostellar collapse, as a template library for observations of cores and very young protostars, and for researchers who wish to test their chemical modeling under dynamic astrophysical conditions. It was also designed to identify statistical trends that may appear when running many models of the formation of low-mass stars by varying the initial conditions. A large set of 143 calculations of the gravitational collapse of an isolated sphere of gas with uniform temperature and a Bonnor-Ebert like density profile was undertaken using a 1D fully implicit Lagrangian radiation hydrodynamics code. The parameter space covered initial masses from 0.2 to 8 Msun, temperatures of 5-30 K and radii between 3000 and 30,000 AU. A spread in the thermal evolutionary tracks of the runs was found, due to differing initial conditions and optical depths. Within less than an order of magnitude, all first and second Larson cores had masses and radii independent of the initial conditions. The time elapsed between the formation of the first and second cores was found to strongly depend on the first core mass accretion rate, and no first core in our grid of models lived for longer than 2000 years, before the onset of the second collapse. The end product of a protostellar cloud collapse, the second Larson core, is, at birth, a canonical object with a mass and radius of about 3 Mjup and 8 Rjup, independent of its initial conditions. The evolution sequence which brings the gas to stellar densities can however proceed in a variety of scenarios, on different timescales, along different isentropes, but each story line can largely be predicted by the initial conditions. All the data from the simulations are publicly available at this address: http://starformation.hpc.ku.dk/grid-of-protostars.

24 pages, 14 figures, accepted for publication in A&A

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• The Formation of Stellar Clusters in Magnetized, Filamentary Infrared Dark Clouds
• Stellar mass spectrum within massive collapsing clumps II. Thermodynamics and tidal forces of the first Larson core
• Zooming in on Individual Star Formation: Low- and High-mass Stars
• Planet formation around M dwarfs via disc instability: Fragmentation conditions and protoplanet properties
• Chemical Variation among Protostellar Cores: Dependence on Prestellar Core Conditions
• The Origin of the Stellar Mass Distribution and Multiplicity
• What is the role of stellar radiative feedback in setting the stellar mass spectrum?
• Explaining the luminosity spread in young clusters: proto and pre-main sequence stellar evolution in a molecular cloud environment
• First Core Properties: From Low- to High-mass Star Formation
• Constraining the Infalling Envelope Models of Embedded Protostars: BHR 71 and its Hot Corino
• Birth of convective low-mass to high-mass second Larson cores
• On the episodic excursions of massive protostars in the Hertzsprung-Russell diagram
• How first hydrostatic cores, tidal forces and gravo-turbulent fluctuations set the characteristic mass of stars
• Stellar mass spectrum within massive collapsing clumps III. Effects of temperature and magnetic field
• The efficiency of photodissociation for molecules in interstellar ices
• Imprint of planet formation in the deep interior of the Sun
• The birth and early evolution of a low mass protostar
• Mixing is easy: New insights for cosmochemical evolution from pre-stellar core collapse
• What can the SEDs of first hydrostatic core candidates reveal about their nature?
• A Model for Protostellar Cluster Luminosities and the Impact on the CO-H${}_2$ Conversion Factor
• Mapping Synthetic Observations to Prestellar Core Models: An Interpretable Machine Learning Approach
• Radiation Hydrodynamics Simulations of Spherical Protostellar Collapse for Very Low Mass Objects
• A 1000 AU Scale Molecular Outflow Driven by a Protostar with an age of <4000 Years
• Insights into the first and second hydrostatic core stages from numerical simulations
• Protostellar spin-up and fast rotator formation through binary star formation
• Turn up the light: Radiative efficiency of protostars at birth
• A fast and accurate method of radiation hydrodynamics calculation in spherical symmetry
• Protoplanetary disk formation from the collapse of a prestellar core