dc.contributor.author | Wurster, James | |
dc.contributor.author | Bate, Matthew | |
dc.date.accessioned | 2019-08-28T09:02:58Z | |
dc.date.issued | 2019-08-28 | |
dc.date.updated | 2019-08-28T03:28:56Z | |
dc.description.abstract | We investigate the formation and fragmentation of discs using a suite of three-dimensional smoothed particle radiative magnetohydrodynamics simulations. Our models are initialised as 1 solar mass rotating Bonnor-Ebert spheres that are threaded with a uniform magnetic field. We examine the effect of including ideal and non-ideal magnetic fields, the orientation and strength of the magnetic field, and the initial rotational rate. We follow the gravitational collapse and early evolution of each system until the final classification of the protostellar disc can be determined. Of our 105 models, 41 fragment, 21 form a spiral structure but do not fragment, and another 12 form smooth discs. Fragmentation is more likely to occur for faster initial rotation rates and weaker magnetic fields. For stronger magnetic field strengths, the inclusion of non-ideal MHD promotes disc formation, and several of these models fragment, whereas their ideal MHD counterparts do not. For the models that fragment, there is no correlation between our parameters and where or when the fragmentation occurs. Bipolar outflows are launched in only 17 models, and these models have strong magnetic fields that are initially parallel to the rotation axis. Counter-rotating envelopes form in four slowly-rotating, strong-field models – including one ideal MHD model – indicating they form only in a small fraction of the parameter space investigated. | en_GB |
dc.description.sponsorship | European Research Council (ERC) | en_GB |
dc.description.sponsorship | Science and Technology Facilities Council (STFC) | en_GB |
dc.description.sponsorship | Science and Technology Facilities Council (STFC) | en_GB |
dc.description.sponsorship | Science and Technology Facilities Council (STFC) | en_GB |
dc.description.sponsorship | Science and Technology Facilities Council (STFC) | en_GB |
dc.description.sponsorship | Science and Technology Facilities Council (STFC) | en_GB |
dc.identifier.doi | 10.24378/exe.1743 | |
dc.identifier.grantnumber | FP7/2007- 2013 grant agreement no. 339248 | en_GB |
dc.identifier.grantnumber | ST/K000373/1 | en_GB |
dc.identifier.grantnumber | ST/K0003259/1 | en_GB |
dc.identifier.grantnumber | ST/K000373/1 | en_GB |
dc.identifier.grantnumber | ST/R002363/1 | en_GB |
dc.identifier.grantnumber | ST/R001014/1 | en_GB |
dc.identifier.uri | http://hdl.handle.net/10871/38469 | |
dc.language.iso | en | en_GB |
dc.publisher | University of Exeter | en_GB |
dc.relation.url | http://hdl.handle.net/10871/37605 | en_GB |
dc.rights | CC BY 4.0 | en_GB |
dc.subject | methods: numerical | en_GB |
dc.subject | MHD | en_GB |
dc.subject | magnetic fields | en_GB |
dc.subject | stars: formation | en_GB |
dc.subject | planets and satellites: formation | en_GB |
dc.subject | accretion: accretion discs | en_GB |
dc.title | Disc formation and fragmentation using radiative non-ideal magnetohydrodynamics (dataset) | en_GB |
dc.type | Dataset | en_GB |
dc.date.available | 2019-08-28T09:02:58Z | |
dc.description | This is the data created for Wurster & Bate (2019): Disc formation and fragmentation using radiative non-ideal magnetohydrodynamics. This dataset was created using the smoothed particle magnetohydrodynamics code sphNG, which included v1.2.1 of the NICIL library (Wurster 2016) to calculate the non-ideal MHD coefficients. The raw data and important files have been uploaded; the data files can be read with either sphNG (proprietary SPH code), or with the public graphics programme Splash (Price 2007).
Each model has been tarred in its own file, where the model name is the file name. For the hydrodynamic models, the names are HObb.tar.gz, where bb is 100 times the initial rotation in terms of the orbital radius. For the magnetised models, the names are aObbMuccBdd.tar.gz, where a=I (N) for ideal (non-ideal) MHD, bb is as above, cc is the normalised mass-to-flux ratio, and dd the magnetic field direction (xn for -B_x, zn for -B_z, zp for +B_z).
01_Misc.tar.gz contains some useful analysis routines and lists; 02_Images.tar.gz includes the images and code required for the figures in the manuscript, and addition figures and code that were used in the analysis. Due to high time resolution of some models, several intermediate/redundant dump files were deleted during production to save space; thus the dump numbers are not sequential in these .tar.gz files, and the missing number represent the deleted dump files. | en_GB |
dc.description | The article associated with this dataset is located in ORE at: http://hdl.handle.net/10871/37605 | en_GB |
dc.rights.uri | https://creativecommons.org/licenses/by/4.0 | en_GB |
rioxxterms.version | NA | en_GB |
rioxxterms.type | Other | en_GB |
refterms.dateFOA | 2019-08-28T09:03:03Z | |