I11 : COR2DISC: From pre-stellar cores to protoplanetary discs

> Read the articles connected to the project.



    Understanding star and planet formation is one of the major goal in modern astrophysics and must now be tackled using a multidisciplinary approach.


    Here we propose to combine star formation numerical simulations of cloud collapse with microphysical evolution gas and dust models to understand how material from the Interstellar Medium (ISM) is delivered into a protoplanetary disc, such as the solar nebula.


    Confrontations to meteoritic and specraft data thanks to the coupling of ISM simulations with solar nebula disc models will trigger important progress for our knowledge of the coupling between ISM and planet formation.


    WP leader Patrick Hennebelle AIM Chercheur-ingénieur, CEA
    WP co-leader Sébastien Charnoz IPGP Professsor, Diderot university
    WP co-leader Marc Chaussidon IPGP Directeur de recherché, CNRS
    WP member Sébastien Fromang AIM Chercheur-ingénieur, CEA
    WP member Frederic MOYNIER IPGP Professor Diderot university
    WP member Yueh Ninh LEE IPGP PostDoc IPGP


    Yueh-Ning Lee, who just got her PhD, started in October 2017. Given that the main task force is really starting, the results described below should be considered has preliminary. They are nevertheless substantial and have already permitted to Yueh-Ning Lee to start working immediately.


    One of the main goals of cor2disk is to produce self-consistently protoplanetary discs from the collapse and to follow its evolution. As stressed in the original proposal, this is challenging when non-ideal magneto-hydrodynamics (mhd) is included because the timesteps induced by the second derivatives are very small, making integration over long timescales a difficult issue. On the other hand, we found it to be really necessary in order to get reliable results since it really has a strong impact onto disc formation. During the last months, we have conducted a series of numerical simulations that we are now using to conduct detailed analysis of the disk formation and evolution.

    Our work this year developed on two aspects : (1) Hydrodynamical simulations of core collapse, in order to characterize the flux, in different fluid regimes (Hydro, ideal MHD, non ideal MHD) and (2) 1d simulation of gas and dust transport in a disk fed by a molecular cloud.


    Our first goal now that a first set of simulations including tracer particles has been produced is to analyze them and extract information that will help to improve the existing disc models. For this purpose we will compute the mater fluxes across time and quantify their mean values and fluctuations. We will study the dependence of these quantities in the initial conditions and also carefully investigate the role of magnetic field. We will also use the tracer particles to i) quantify better the trajectories within the nascent solar system and ii) follow the evolution of the matter composition in postprocessing and infer abundances of various quantities such as the CAI. Compare the prediction with observations.


  • Charnoz et al., Pignatale F., 2017. Transport of refractory and volatiles elements in a viscously evolving disk. Under redaction