Magnetic Fields in Astrophysics: Origins and Evolution. Kinwah Wu Mullard Space Science Laboratory University College London
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1 Magnetic Fields in Astrophysics: Origins and Evolution Kinwah Wu Mullard Space Science Laboratory University College London
2 Maxwell s equations covariant form in flat space time Lorentz force equation:
3 Astrophysical magnetic fields magnetic field (gauss) walls? voids? clusters galaxies stars white dwarfs neutron stars magnetars > linear size (cm) ~ mass (solar mass)
4 Cosmological-scale fields vs stellar fields magnetic flux - magnetars - neutron stars - white dwarfs - solar-like stars - galaxies - galaxy clusters - superclusters and beyond Gcm Gcm Gcm Gcm 2 ~10 41 Gcm 2 ~10 43 Gcm 2??? t ds n B = t V d 3 x B = 0 flux conservation
5 Cosmological magnetic field (I) - light elements in metal poor halo stars 6 Li abundance indicating that the galaxy was bombarded by cosmic ray before it was formed (Rollinde et al. 2005) - pulsar rotational measurement and timing study indicating a dipolar field in the Milky Way (Han 2008) - Faraday rotation in damped Lyman-α forest systems at z ~ 2, suggesting large-scale magnetic field B ~ 10-6 G (Blasi, Burles & Olinto 1999) - in quasars, where MRI operates in accretion disks and jets, at z > 5
6 Cosmological magnetic field (II) Cosmological magneto-genesis - fundamental issues standard plasma physics or exotic physics? bottom-up process or top-down process? Angular momentum regulation - proto-star formation in the early universe - fueling and growing supermassive black holes (quasars at high z )
7 Magneto-genesis: Biermann battery (I) Faraday s Law Ohm s Law (omitting the current for the time being) The Biermann battery equation
8 Magneto-genesis: Biermann battery (II) in co-moving frame barotropic fluid - isobaric surface coincide with isopynic surface slow moving flux conservation
9 Magneto-genesis: bottom up scenario (I) (1) Biermann battery operations in small scales - stars, disks, accretion inflows (2) Dynamo growth - scaled by rotation rates - in favour of compact objects which are fast rotators (3) Field expelled from stellar objects - via supernovae, jets, outflows (4) Diffusion and connection/combination of small-scale fields - building up large-scale fields
10 Magneto-genesis: bottom up scenario (II) field generation in galaxies via supernova remnants (SNR) - suppose in a plerion SNR - SNR overlapping when - reaching pressure equilibrium at - diffusion coefficient (via ambipolar process) timescale to fill a galaxy with SNR generated field expected Strength of the random field (Zweibel 2006)
11 Magneto-genesis: bottom up scenario (III) the difficulty for field spreading beyond galaxies - typical size of a rich galaxy cluster - diffusion coefficient timescale for a galactic field to spread over within a galaxy clusters How about magnetic fields in large structures beyond galaxy clusters???
12 Magneto-genesis: top down scenario (I) behind the photon last scattering surface - the media are opaque to light - photons, electrons and protons are strongly coupled Thomson cross sections of charged particles near the last scattering surface - photons preferentially scatter off electrons rather than protons - velocity difference between charged particles, i.e. electric currents - anisotropy in the photon radiation field leading to micro-rotation
13 Magneto-genesis: top down scenario (II) - Faraday induction equation - Ohm s law - Euler equation - metric for space-time structure magnetic field evolution equation (Ichiki et al. 2007) scalar perturbation tensor perturbation vorticity photon density contrast baryon-photon slip stress anisotropy
14 Neutrinos standard model for particle physics - lepton family ν e ν µ ν τ e µ τ + their anti-particles - neutrinos have non-zero mass - neutrino oscillations/mixing during propagation - neutrinos interact with their leptons via weak interaction k α Ii (k β ) x α + Γ α βγk β k γ Ii (k β ) k α = u δ k δ j χ ij 0 (xβ, k β )I j (k β ) + η i 0(x β, k β ) + d 4 k j 0 (xβ, k β, k β )I j (k β ) σ ij destruction/conversion creation scattering
15 Cosmological fields (I) - neutrino last scattering surfaces (CNB!) - 3 scattering surfaces instead of 1 only surface - charge particle slip - in dense early universe scalar perturbation tensor perturbation the corresponding field evolutionary equation for neutrino scattering neutrino density contrast? Lepton-neutrino slip? stress anisotropy? vorticity (coupled w/ helicity???)
16 Epilogue (1): galaxy merging and magnetic field
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