Astro2020 Science White Paper: Magnetic Fields and Polarization in the Diffuse Interstellar Medium

Clark, Susan; Heiles, Carl; Robishaw, Timothy

doi:10.48550/arxiv.1903.07671

Cited by 3 publications

(3 citation statements)

References 27 publications

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“…Magnetic fields are observed across all scales within the universe, from the interstellar medium (ISM) on the scales of molecular clouds (e.g., Heiles & Crutcher 2005;Crutcher 2012;Clark et al 2014Clark et al , 2019Hu et al 2019;Sullivan et al 2021) over the large-scale field structure in galaxies (e.g., Basu & Roy 2013;Beck & Krause 2005;Greaves et al 2000;Jones et al 2020;Lacki & Beck 2013;Robishaw et al 2008;Tabatabaei et al 2008;Watson & Wyld 2001) to the intracluster medium (ICM; e.g., Bonafede et al 2009Bonafede et al , 2010Bonafede et al , 2013Böhringer et al 2016;Clarke et al 2001;Hu et al 2020).…”

Section: Introductionmentioning

confidence: 99%

On the Small-scale Turbulent Dynamo in the Intracluster Medium: A Comparison to Dynamo Theory*

Steinwandel

Boess

Dolag

et al. 2022

ApJ

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We present non-radiative, cosmological zoom-in simulations of galaxy-cluster formation with magnetic fields and (anisotropic) thermal conduction of one massive galaxy cluster with M vir ∼ 2 × 1015 M ⊙ at z ∼ 0. We run the cluster on three resolution levels (1×, 10×, 25×), starting with an effective mass resolution of 2 × 108 M ⊙, subsequently increasing the particle number to reach 4 × 106 M ⊙. The maximum spatial resolution obtained in the simulations is limited by the gravitational softening reaching ϵ = 1.0 kpc at the highest resolution level, allowing one to resolve the hierarchical assembly of the structures in fine detail. All simulations presented are carried out with the SPMHD code gadget3 with an updated SPMHD prescription. The primary focus of this paper is to investigate magnetic field amplification in the intracluster medium. We show that the main amplification mechanism is the small-scale turbulent dynamo in the limit of reconnection diffusion. In our two highest resolution models we start to resolve the magnetic field amplification driven by the dynamo and we explicitly quantify this with the magnetic power spectra and the curvature of the magnetic field lines, consistent with dynamo theory. Furthermore, we investigate the ∇ · B = 0 constraint within our simulations and show that we achieve comparable results to state-of-the-art AMR or moving-mesh techniques, used in codes such as enzo and arepo. Our results show for the first time in a cosmological simulation of a galaxy cluster that dynamo action can be resolved with modern numerical Lagrangian magnetohydrodynamic methods, a study that is currently missing in the literature.

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Section: Introductionmentioning

confidence: 99%

On the Small-scale Turbulent Dynamo in the Intracluster Medium: A Comparison to Dynamo Theory*

Steinwandel

Boess

Dolag

et al. 2022

ApJ

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“…Magnetic fields are observed across all scales within the Universe, from the Interstellar medium (ISM) on the scales of molecular clouds (e.g. Clark et al 2014Clark et al , 2019Crutcher 2012;Heiles & Crutcher 2005;Sullivan et al 2021;Hu et al 2019) over the large scale field structure in galaxies (e.g. Basu & Roy 2013;Beck & Krause 2005;Greaves et al 2000;Jones et al 2020;Lacki & Beck magnetic field strength from the Faraday Rotation Measurement (RM) of radio galaxies that are located in the foreground and background of the cluster of interest (e.g.…”

Section: Introductionmentioning

confidence: 99%

On the small scale turbulent dynamo in the intracluster medium: A comparison to dynamo theory

Steinwandel,

Boess,

Dolag

et al. 2021

Preprint

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We present non-radiative, cosmological zoom-simulations of galaxy cluster formation with magnetic fields and (anisotropic) thermal conduction of one very massive galaxy cluster with a mass at redshift zero that corresponds to M vir ∼ 2 × 10 15 M . We run the cluster on three resolution levels (1X, 10X, 25X), starting with an effective mass resolution of 2 × 10 8 M , subsequently increasing the particle number to reach 4 × 10 6 M . The maximum spatial resolution obtained in the simulations is limited by the gravitational softening reaching = 1.0 kpc at the highest resolution level, allowing to resolve the hierarchical assembly of the structures in very fine detail. All simulations presented, have been carried out with the SPMHD-code gadget-3 with a heavily updated SPMHD prescription. The primary focus is to investigate magnetic field amplification in the Intracluster Medium (ICM). We show that the main amplification mechanism is the small scale-turbulent-dynamo in the limit of reconnection diffusion. In our two highest resolution models we start to resolve the magnetic field amplification driven by this process and we explicitly quantify this with the magnetic power-spectra and the magnetic tension that limits the bending of the magnetic field lines consistent with dynamo theory. Furthermore, we investigate the ∇•B = 0 constraint within our simulations and show that we achieve comparable results to state-of-the-art AMR or moving-mesh techniques, used in codes such as enzo and arepo. Our results show for the first time in a fully cosmological simulation of a galaxy cluster that dynamo action can be resolved in the framework of a modern Lagrangian magnetohydrodynamic (MHD) method, a study that is currently missing in the literature.

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“…Current facilities, e.g., SOFIA and ALMA, already have the capability to cover the submillimeter band for the spectral polarimetry observation. One can also mention the linear polarization of the 21 cm line (e.g., Clark et al 2019).…”

Section: Polarization Of Other Linesmentioning

confidence: 99%

ESA Voyage 2050 white paper: A complete census of the gas phases in and around galaxies, far-UV spectropolarimetry as a prime tool for understanding galaxy evolution and star formation

Lebouteiller,

Yan,

Richter

et al. 2019

Preprint

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Lebouteiller et al.: A complete census of the gas phases in and around galaxies Another interesting prospect is to transpose the same level of details that has been reached for the Milky Way to the ISM in external galaxies, in particular in metal-poor galaxies, where the ISM chemical composition, physical conditions, and topology (arrangement of various phases) change dramatically, with significant consequences on the star-formation properties and on the overall galaxy evolution. We need to know, in particular, how star formation proceeds in quasi-pristine or pristine environments and what is the role of accreting clouds and compact objects in regulating the star formation process. To circumvent systematic biases in column density determinations and to examine the ISM enrichment as a function of the environment, next far-UV missions should be versatile enough to observe stellar clusters and individual O/B stars at distances of few Mpc to few 100s Mpc respectively, with a spectral resolution power R ∼ 10 5 and 10 4 respectively. Such requirements are also necessary to perform statistical analyses of background quasar lines of sight intersecting the CGM of galaxies at various redshifts. The CGM is an important component of galaxies that connects the galaxy to the cosmic web and is, as such, at the center of many processes that we do not yet fully understand. With future UV missions, we ought to be able to fill the gap between the various physical scales and phases and to comprehend the role of gas exchanges and flows for galaxy evolution. We advocate a far-UV space telescope that will be able to tackle these issues. Such an observatory would enable access to the range ≈ 900 − 3100 Å, and would require an exceptionally large mirror > 5 m. The optimal observation mode would be spectropolarimetry with a resolution of R 10 5 .

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Astro2020 Science White Paper: Magnetic Fields and Polarization in the Diffuse Interstellar Medium

Cited by 3 publications

References 27 publications

On the Small-scale Turbulent Dynamo in the Intracluster Medium: A Comparison to Dynamo Theory*

On the Small-scale Turbulent Dynamo in the Intracluster Medium: A Comparison to Dynamo Theory*

On the small scale turbulent dynamo in the intracluster medium: A comparison to dynamo theory

ESA Voyage 2050 white paper: A complete census of the gas phases in and around galaxies, far-UV spectropolarimetry as a prime tool for understanding galaxy evolution and star formation

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