Magnetization of the Intergalactic Medium by Primeval Galaxies

Kronberg, P. P.; Lesch, H.; Hopp, U.

doi:10.1086/306662

Cited by 166 publications

(150 citation statements)

References 46 publications

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“…magnetize the intergalactic medium as predicted by Kronberg et al (1999) and Bertone et al (2006). The performed simulations indicate that the CR-driven dynamo can explain the observed magnetic fields in dwarf irregular galaxies.…”

Section: Discussionsupporting

confidence: 65%

3D model of magnetic fields evolution in dwarf irregular galaxies

Siejkowski¹,

Soida²,

Otmianowska-Mazur³

et al. 2010

Proc. IAU

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Abstract. Radio observations show that magnetic fields are present in dwarf irregular galaxies (dIrr) and its strength is comparable to that found in spiral galaxies. Slow rotation, weak shear and shallow gravitational potential are the main features of a typical dIrr galaxy. These conditions of the interstellar medium in a dIrr galaxy seem to unfavourable for amplification of the magnetic field through the dynamo process. Cosmic-ray driven dynamo is one of the galactic dynamo model, which has been successfully tested in case of the spiral galaxies. We investigate this dynamo model in the ISM of a dIrr galaxy. We study its efficiency under the influence of slow rotation, weak shear and shallow gravitational potential. Additionally, the exploding supernovae are parametrised by the frequency of star formation and its modulation, to reproduce bursts and quiescent phases. We found that even slow galactic rotation with a low shearing rate amplifies the magnetic field, and that rapid rotation with a low value of the shear enhances the efficiency of the dynamo. Our simulations have shown that a high amount of magnetic energy leaves the simulation box becoming an efficient source of intergalactic magnetic fields.

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Section: Discussionsupporting

confidence: 65%

3D model of magnetic fields evolution in dwarf irregular galaxies

Siejkowski¹,

Soida²,

Otmianowska-Mazur³

et al. 2010

Proc. IAU

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“…Some of them are similar to those discussed above, differing only in the time when the magnetic pollution is assumed to take place. In the present class of models the magnetic field seeds are supposed to be expelled by an early population of AGN or dwarf starburst galaxies at a redshift between 4 and 6 (Kronberg et al 1999); this process would magnetise a large fraction of the volume. Recently, the validity of such a scenario has been confirmed by a semi-analytic modelling of galactic winds (Bertone et al 2006).…”

Section: Possible Origins Of Magnetic Fieldsmentioning

confidence: 99%

Non-Thermal Processes in Cosmological Simulations

2008

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Non-thermal components are key ingredients for understanding clusters of galaxies. In the hierarchical model of structure formation, shocks and large-scale turbulence are unavoidable in the cluster formation processes. Understanding the amplification and evolution of the magnetic field in galaxy clusters is necessary for modelling both the heat transport and the dissipative processes in the hot intra-cluster plasma. The acceleration, transport and interactions of non-thermal energetic particles are essential for modelling the observed emissions. Therefore, the inclusion of the non-thermal components will be mandatory for simulating accurately the global dynamical processes in clusters. In this review, we summarise the results obtained with the simulations of the formation of galaxy clusters which address the issues of shocks, magnetic field, cosmic ray particles and turbulence.

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“…Among them, primordial magnetic fields, jets and radio lobes emerging from radio galaxies (e.g., Hoyle 1969;Chakrabarti et al 1994;Enßlin et al 1997) and galactic winds (e.g., Kronberg et al 1999;Bertone et al 2006). Simulations (Kronberg et al 1999;Kronberg et al 2001;Bertone et al 2006) show that magnetic fields can be efficiently transported into the IGM and fill most of the universe by z = 0. Bertone et al (2006) predict that galactic winds alone could be responsible for IGM magnetic fields of order 10 −6 -10 −2 µG, in agreement with observations.…”

Section: Intergalactic Magnetic Fieldsmentioning

confidence: 99%

Numerical Simulations of the Warm-Hot Intergalactic Medium

2008

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In this paper we review the current predictions of numerical simulations for the origin and observability of the warm hot intergalactic medium (WHIM), the diffuse gas that contains up to 50 per cent of the baryons at z ∼ 0. During structure formation, gravitational accretion shocks emerging from collapsing regions gradually heat the intergalactic medium (IGM) to temperatures in the range T ∼ 10 5 -10 7 K. The WHIM is predicted to radiate most of its energy in the ultraviolet (UV) and X-ray bands and to contribute a significant fraction of the soft X-ray background emission. While O VI and C IV absorption systems arising in the cooler fraction of the WHIM with T ∼ 10 5 -10 5.5 K are seen in FUSE and Hubble Space Telescope observations, models agree that current X-ray telescopes such as Chandra and XMM-Newton do not have enough sensitivity to detect the hotter WHIM. However, future missions such as Constellation-X and XEUS might be able to detect both emission lines and absorption systems from highly ionised atoms such as O VII, O VIII and Fe XVII.

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Magnetization of the Intergalactic Medium by Primeval Galaxies

Cited by 166 publications

References 46 publications

3D model of magnetic fields evolution in dwarf irregular galaxies

3D model of magnetic fields evolution in dwarf irregular galaxies

Non-Thermal Processes in Cosmological Simulations

Numerical Simulations of the Warm-Hot Intergalactic Medium

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