The role of thermodynamics in disc fragmentation

TL;DR

This paper investigates how different radiative transfer models affect disc fragmentation simulations, revealing that the choice of thermodynamic treatment influences fragment formation, properties, and evolution in protostellar discs.

Contribution

It compares three radiative transfer prescriptions in disc fragmentation simulations, highlighting the limitations of barotropic equations of state versus more detailed methods.

Findings

Barotropic EOS approximations do not account for local conditions or thermal inertia effects.

Number and properties of fragments vary with the radiative transfer method used.

Proto-fragments closer to the star form earlier and evolve faster than those in outer regions.

Abstract

Thermodynamics play an important role in determining the way a protostellar disc fragments to form planets, brown dwarfs and low-mass stars. We explore the effect that different treatments of radiative transfer have in simulations of fragmenting discs. Three prescriptions for the radiative transfer are used, (i) the diffusion approximation of Stamatellos et al., (ii) the barotropic equation of state (EOS) of Goodwin et al., and (iii) the barotropic EOS of Bate et al. The barotropic approximations capture the general evolution of the density and temperature at the centre of each proto-fragment but (i) they do not make any adjustments the particular circumstances of a proto-fragment forming in the disc, and (ii) they do not take into account thermal inertia effects that are important for fast-forming proto-fragments in the outer disc region. As a result, the number of fragments formed in the disc and their properties are different, when a barotropic EOS is used. This is important not only for disc studies but also for simulations of collapsing turbulent clouds, as in many cases in such simulations stars form with discs that subsequently fragment. We also examine the difference in the way proto-fragments condense out in the disc at different distances from the central star using the diffusion approximation and following the collapse of each proto-fragment until the formation of the second core (~10^{-3} g/cm3). We find that proto-fragments forming closer to the central star tend to form earlier and evolve faster from the first to the second core than proto-fragments forming in the outer disc region. The former have a large pool of material in the inner disc region that they can accrete from and grow in mass. The latter accrete more slowly and they are hotter because they generally form in a quick abrupt event.