Resistive and Multi-fluid RMHD on Graphics Processing Units

Wright, A.; Hawke, Ian

doi:10.3847/1538-4365/aaf1b0

Cited by 6 publications

(5 citation statements)

References 39 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…All results have been generated using the METHOD code 2 . Details of the numerical schemes used in METHOD can be found in more detail in [13]. Briefly, the numerical flux is computed using flux splitting, with a third order WENO Larger resistivities lead to a greater rate of magnetic diffusion and thus greater smearing out compared to the ideal MHD solution.…”

Section: Methodsmentioning

confidence: 99%

“…One issue with more physically complex models that prevents the wide spread adoption of the resistive GRMHD equations is the additional computation required in their evolution. Due to the possibly stiff source term of resistive GRMHD [2], an implicit integrator, often the IMEX schemes of [10], is required to keep execution times rea-sonable [2,3,11,12,13]. Whilst these schemes allow for a faster evolution than would be possible using traditional explicit schemes for the majority of the parameter space, they still result in at least a factor 5× slow-down compared to conventional, ideal GRMHD models [5].…”

Section: Motivationmentioning

confidence: 99%

See 1 more Smart Citation

A resistive extension for ideal MHD

Wright,

Hawke

2019

Preprint

View full text Add to dashboard Cite

We present an extension to the special relativistic, ideal magnetohydrodynamics (MHD) equations, designed to capture effects due to resistivity. The extension takes the simple form of an additional source term which, when implemented numerically, is shown to emulate the behaviour produced by a fully resistive MHD description for a range of initial data. The extension is developed from first principle arguments, and thus requires no fine tuning of parameters, meaning it can be applied to a wide range of dynamical systems. Furthermore, our extension does not suffer from the same stiffness issues arising in resistive MHD, and thus can be evolved quickly using explicit methods, with performance benefits of roughly an order of magnitude compared to current methods.

show abstract

Section: Methodsmentioning

confidence: 99%

Section: Motivationmentioning

confidence: 99%

A resistive extension for ideal MHD

Wright,

Hawke

2019

Preprint

View full text Add to dashboard Cite

show abstract

“…The restrictions on 𝜎 and 𝑏/𝑎 reduce the sample to 912 galaxies. The parameters 𝑎 deV , 𝑏/𝑎, and 𝜎 fiber in 𝑟-band are taken from the catalogs PhotObjAll and SpecObjAll of DR15 (Aguado et al 2019).…”

Section: 𝑀 * − 𝜎 Relationmentioning

confidence: 99%

Late growth of early-type galaxies in low-z massive clusters

Ribeiro¹,

Nascimento²,

Morell³

et al. 2023

Preprint

View full text Add to dashboard Cite

We study a sample of 936 early-type galaxies (ETGs) located in 48 low-z regular galaxy clusters with 𝑀 200 ≥ 10 14 𝑀 at 𝑧 < 0.1. We examine variations in the concentration index, radius, and color gradient of ETGs as a function of their stellar mass and loci in the projected phase space (PPS) of the clusters. We aim to understand the environmental influence on the growth of ETGs according to the time since infall into their host clusters. Our analysis indicates a significant change in the behavior of the concentration index 𝐶 and color gradient around 𝑀 * ≈ 2 × 10 11 𝑀 ≡ M * . Objects less massive than M * present a slight growth of 𝐶 with 𝑀 * with negative and approximately constant color gradients in all regions of the PPS. Objects more massive than M * present a slight decrease of 𝐶 with 𝑀 * with color gradients becoming less negative and approaching zero. We also find that objects more massive than M * , in all PPS regions, have smaller 𝑅 90 for a given 𝑅 50 , suggesting a smaller external growth in these objects or even a shrinkage possibly due to tidal stripping. Finally, we estimate different dark matter fractions for galaxies in different regions of the PPS, with the ancient satellites having the largest fractions, 𝑓 𝐷 𝑀 ≈ 65%. These results favor a scenario where cluster ETGs experience environmental influence the longer they remain and the deeper into the gravitational potential they lie, indicating a combination of tidal stripping + harassment, which predominate during infall, followed by mergers + feedback effects affecting the late growth of ancient satellites and BCGs.

show abstract

“…In RHD and RMHD codes, this task requires solving a highly nonlinear algebraic system of equations, which constitutes one of the most challenging tasks from the point of view of computational efficiency. The recovery of primitive variables is usually considered as one of the bottlenecks for the speed-up of the code (Wright & Hawke 2019). Of the different strategies that exist in the literature (see, e.g, Martí & Müller 2015, and references therein), we chose to recover the set of primitive variables following the inversion scheme of Mignone & McKinney (2007).…”

Section: A22 Spatial Cell Reconstructionmentioning

confidence: 99%

3D RMHD simulations of jet-wind interactions in high-mass X-ray binaries

López-Miralles

Perucho

Martí

et al. 2022

A&A

View full text Add to dashboard Cite

Context. Relativistic jets are ubiquitous in the Universe. In microquasars, especially in high-mass X-ray binaries, the interaction of jets with the strong winds driven by the massive and hot companion star in the vicinity of the compact object is fundamental for understanding the jet dynamics, nonthermal emission, and long-term stability. However, the role of the jet magnetic field in this process is unclear. In particular, it is still debated whether the magnetic field favors jet collimation or triggers more instabilities that can jeopardize the jet evolution outside the binary. Aims. We study the dynamical role of weak and moderate to strong toroidal magnetic fields during the first several hundred seconds of jet propagation through the stellar wind, focusing on the magnetized flow dynamics and the mechanisms of energy conversion. Methods. We developed the code Lóstrego v1.0, a new 3D relativistic magnetohydrodynamics code to simulate astrophysical plasmas in Cartesian coordinates. Using this tool, we performed the first 3D relativistic magnetohydrodynamics numerical simulations of relativistic magnetized jets propagating through the clumpy stellar wind in a high-mass X-ray binary. To highlight the effect of the magnetic field in the jet dynamics, we compared the results of our analysis with those of previous hydrodynamical simulations. Results. The overall morphology and dynamics of weakly magnetized jet models is similar to previous hydrodynamical simulations, where the jet head generates a strong shock in the ambient medium and the initial overpressure with respect to the stellar wind drives one or more recollimation shocks. On the timescales of our simulations (i.e., t < 200 s), these jets are ballistic and seem to be more stable against internal instabilities than jets with the same power in the absence of fields. However, moderate to strong toroidal magnetic fields favor the development of current-driven instabilities and the disruption of the jet within the binary. A detailed analysis of the energy distribution in the relativistic outflow and the ambient medium reveals that magnetic and internal energies can both contribute to the effective acceleration of the jet. Moreover, we verified that the jet feedback into the ambient medium is highly dependent on the jet energy distribution at injection, where hotter, more diluted and/or more magnetized jets are more efficient. This was anticipated by feedback studies in the case of jets in active galaxies.

show abstract

Resistive and Multi-fluid RMHD on Graphics Processing Units

Cited by 6 publications

References 39 publications

A resistive extension for ideal MHD

A resistive extension for ideal MHD

Late growth of early-type galaxies in low-z massive clusters

3D RMHD simulations of jet-wind interactions in high-mass X-ray binaries

Contact Info

Product

Resources

About