English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

Despite their ubiquity, the origin of cosmic magnetic fields remains unknown.Various mechanisms have been proposed for their existence including primordialfields generated by inflation, or amplification and injection by compactastrophysical objects. Separating the potential impact of each magnetogenesisscenario on the magnitude and orientation of the magnetic field and theirimpact on gas dynamics may give insight into the physics that magnetised ourUniverse. In this work, we demonstrate that because the induction equation andsolenoidal constraint are linear with $B$, the contribution from differentsources of magnetic field can be separated in cosmological magnetohydrodynamicssimulations and their evolution and influence on the gas dynamics can betracked. Exploiting this property, we develop a magnetic field tracer algorithmfor cosmological simulations that can track the origin and evolution ofdifferent components of the magnetic field. We present a suite of cosmologicalmagnetohydrodynamical RAMSES simulations that employ this algorithm where theprimordial field strength is varied to determine the contributions of theprimordial and supernovae-injected magnetic fields to the total magnetic energyas a function of time and spatial location. We find that, for our specificmodel, the supernova-injected fields rarely penetrate far from haloes, despiteoften dominating the total magnetic energy in the simulations. The magneticenergy density from the supernova-injected field scales with density with apower-law slope steeper than 4/3 and often dominates the total magnetic energyinside of haloes. However, the star formation rates in our simulations are notaffected by the presence of magnetic fields, for the ranges of primordial fieldstrengths examined. These simulations represent a first demonstration of themagnetic field tracer algorithm (abridged).

Magnetogenesis at Cosmic Dawn: Tracing the Origins of Cosmic Magnetic Fields