An MHD gadget for cosmological simulations

By Klaus Dolag, Federico A. Stasyszyn. 2008

145 citations recorded by the source corpus.

Various radio observations have shown that the hot atmospheres of galaxy clusters are magnetized. However, our understanding of the origin of these magnetic fields, their implications on structure formation and their interplay with the dynamics of the cluster atmosphere, especially in the centers of galaxy clusters, is still very limit ed. In preparation for the upcoming new generation of radio telescopes (like EVLA, LWA, LOFAR and SKA), a huge effort is being made to learn more about cosmological magnetic fields f rom the observational perspective. Here we present the implementation of magneto-hydrodynamics in the cosmological SPH code GADGET (Springel et al. 2001; Springel 2005). We discuss the details of the implementation and various schemes to suppress numerical instabilities as well as regularization schemes, in the context of cosmological simulations. The performance of the SPH-MHD code is demonstrated in various one and two dimensional test problems, which we performed with a fully, three dimensional setup to test the code under reali stic circumstances. Comparing solutions obtained using ATHENA (Stone et al. 2008), we find exc ellent agreement with our SPH-MHD implementation. Finally we apply our SPH-MHD implementation to galaxy cluster formation within a large, cosmological box. Performing a resolution study we demonstrate the robustness of the predicted shape of the magnetic field pr ofiles in galaxy clusters, which is in good agreement with previous studies.

Subfields: Astronomy and Astrophysics, Computational Mechanics

View Paper: https://www.semanticscholar.org/paper/b39fc9148fa530ef3c58132ffb593a27cfbaa2fa

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Citations in the corpus

Smoothed particle hydrodynamics and magnetohydrodynamics (2010, methodology): “[49,12,29].”
Constraints on the distribution and energetics of fast radio bursts using cosmological hydrodynamic simulations (2014, methodology): “Furthermore, the simulation is extended with magnetic fields following the implementation of Dolag & Stasyszyn (2009).”
Simulations of magnetic fields in isolated disc galaxies (2012, result): “…in our simulations are smaller or at most of the same order than in cosmological MHD simulations carried out with the latest generation of SPH-MHD methods (Dolag & Stasyszyn 2009; Beck et al. 2012; Stasyszyn et al. 2012), which have similar properties regarding magnetic field divergence errors.”
IMPACT OF CLUSTER PHYSICS ON THE SUNYAEV–ZEL'DOVICH POWER SPECTRUM (2010, background): “…sub-grid baryonic processes, such as radiative cooling, star formation, feedback mechanisms, cosmic rays, thermal conduction and magnetic fields, on the thermal structure of the ICM (Nagai et al. 2007a; Pfrommer et al. 2007; Dolag & Stasyszyn 2009; Sijacki et al. 2007, 2008; Battaglia et al. 2010).”
Simulating galaxy formation with the IllustrisTNG model (2017, background): “…new physics in large-scale cosmological simulations for galaxy formation, particularly the amplification and evolution of a seed magnetic field (Dolag & Stasyszyn 2009; Pakmor, Bauer & Springel 2011; Hopkins & Raives 2016; Mocz et al. 2016) and the effects of & kpcscale gas outflows triggered…”
Smoothed Particle Hydrodynamics in Astrophysics (2010, methodology): “…research on developing improved SPH realizations of MHD has therefore concentrated on constructing formulations thateither eliminate the∇ ·B 6= 0 error, or at least keep it reasonably small (Dolag, Bartelmann & Lesch, 1999; Price & Monaghan, 2004a,b, 2005; Price, 2009; Dolag & Stasyszyn, 2009).”
Massive and refined - II. The statistical properties of turbulent motions in massive galaxy clusters with high spatial resolution (2010, background): “The magnetic ﬁeld is also expected to play a role along the cluster evolution (e.g. Dolag 2006; Dubois & Teyssier 2008;Dolag & Stasyszyn 2009; Donnert et al. 2009; Collins et al. 2010), even if without a ﬀ ecting the spectral properties out-lined in Sec.3.3 for a wide range of scales (e.g. Xu et…”
CRPropa 3—a public astrophysical simulation framework for propagating extraterrestrial ultra-high energy particles (2016, methodology): “For extragalactic fields one can get information at least from simulations of the cosmological large scale galaxy structure which generate magnetic fields based on models of magneto-hydrodynamics [17, 18].”
A model for cosmological simulations of galaxy formation physics: multi-epoch validation (2013, background): “Furthermore, some small-scale simulations also include magnetic fields (e.g., Teyssier et al. 2006; Dolag & Stasyszyn 2009; Collins et al. 2010; Pakmor et al. 2011; Pakmor & Springel 2012), radiative transfer (e.g., Abel & Wandelt 2002; Petkova & Springel 2010; Cantalupo & Porciani 2011), cosmic…”
Phantom: A Smoothed Particle Hydrodynamics and Magnetohydrodynamics Code for Astrophysics (2017, methodology): “…& Monaghan (2004a,b) and 1.5D results on this test with SPMHD, for comparison, can be found in e.g. Price & Monaghan (2005); Rosswog & Price (2007); Dolag & Stasyszyn (2009); Price (2010) and Vanaverbeke et al. (2014), with 2D versions shown in Price (2012a), Tricco & Price (2013) and Tricco et…”
DOUBLE-DETONATION SUB-CHANDRASEKHAR SUPERNOVAE: SYNTHETIC OBSERVABLES FOR MINIMUM HELIUM SHELL MASS MODELS (2010, background): “…, (4) where ρi is the reconstructed mass density, XZ,j is the mass fraction of element Z for tracer particle j (which lies at position xj), hj is the SPH particle smoothing length, and W(x, h) is the SPH kernel function (defined via Equations (1) and (3) of Dolag & Stasyszyn 2009, respectively).”
Theoretical Challenges in Galaxy Formation (2016, background): “…the galactic magnetic field has to be considered and significant progress has been made recently (Dolag, Bykov & Diaferio 2008; Dolag et al. 2005; Dolag & Stasyszyn 2009; Dubois & Teyssier 2010; Kotarba et al. 2010, 2009; Pakmor, Marinacci & Springel 2014; Pakmor et al. 2016; Pakmor & Springel…”