2022
DOI: 10.1093/mnras/stac123
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On the origin of magnetic fields in stars – II. The effect of numerical resolution

Abstract: Are the kG-strength magnetic fields observed in young stars a fossil field left over from their formation or are they generated by a dynamo? Our previous numerical study concluded that magnetic fields must originate by a dynamo process. Here, we continue that investigation by performing even higher numerical resolution calculations of the gravitational collapse of a 1 M⊙ rotating, magnetised molecular cloud core through the first and second collapse phases until stellar densities are reached. Each model includ… Show more

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Cited by 13 publications
(4 citation statements)
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“…While the high-resolution MHD model shows some minor differences, these have a negligble impact on the quantities of interest. This is consistent with Wurster et al (2022), who find that significant deviations due to resolution occur well beyond the densities analysed here. Figure B1 shows the CS midplane abundance profiles and J = 2 − 1 line intensities for the normal and higher resolution models, and the (normal) subcritical model for comparison.…”
Section: Appendix B: Resolution Testssupporting
confidence: 93%
“…While the high-resolution MHD model shows some minor differences, these have a negligble impact on the quantities of interest. This is consistent with Wurster et al (2022), who find that significant deviations due to resolution occur well beyond the densities analysed here. Figure B1 shows the CS midplane abundance profiles and J = 2 − 1 line intensities for the normal and higher resolution models, and the (normal) subcritical model for comparison.…”
Section: Appendix B: Resolution Testssupporting
confidence: 93%
“…Yet, despite this, the switch in Eq. 29 appears to provide less dissipation and work robustly in a variety of real applications, for example, within simulations of the MRI (Wissing et al, 2022) or the collapse of molecular cloud cores to stellar densities (Wurster et al, 2022). Though numerical stability is the purpose of including artificial resistivity in simulations, its implementation is equivalent to a (resolution-dependent) physical dissipation term η∇ 2 B with magnetic diffusivity…”
Section: Artificial Resistivitymentioning
confidence: 99%
“…Over the past decade, SPMHD has been used to simulate the evolution and impact of magnetic fields in a wide variety of astrophysical problems, such as the study of single and binary star formation (Bürzle et al, 2011a;Bürzle et al, 2011b;Price et al, 2012;Bate et al, 2014;Tsukamoto et al, 2015a;Tsukamoto et al, 2015b;Lewis et al, 2015;Tricco 10.3389/fspas.2023.1288219 Wurster et al, 2016;Wurster et al, 2017;Lewis and Bate, 2017;Wurster et al, 2018a;Wurster et al, 2018b;Tsukamoto et al, 2018;Tsukamoto et al, 2020;Wurster et al, 2021;Wurster et al, 2022), star cluster formation (Wurster et al, 2019;Dobbs and Wurster, 2021), star formation rates in spiral galaxies (Herrington et al, 2023), accretion discs (Forgan et al, 2017), tidal disruption events (Bonnerot et al, 2017), the magnetic field structure of spiral galaxies (Dobbs et al, 2016;Wissing and Shen, 2023), and galaxy cluster formation (Barnes et al, 2012;Barnes et al, 2018). It has been shown to yield correct behaviour for the small-scale dynamo amplification of magnetic fields (Tricco et al, 2016b), and can sustain turbulence incited by the magnetorotational instability (MRI) (Deng et al, 2019;Wissing et al, 2022).…”
Section: Introductionmentioning
confidence: 99%
“…Partial ionization effects can also be introduced in a single fluid model, through ambipolar diffusion using a generalized Ohm's law. This approach has been used in many astrophysical contexts for the study of protoplanetary disks (Lesur 2020;Cui & Bai 2021) or molecular clouds (Wurster et al 2022). A more advanced model for dynamics in partially ionized plasmas must employ a fully two-fluid model, where there are separate time evolution equations for neutrals and charged particles (ions, essentially).…”
Section: Introductionmentioning
confidence: 99%