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Article Contents
- ABSTRACT
- 1.INTRODUCTION
- 1.1.Review Scope and Type
- 1.2.Polarimetry
- 2.SELECTED CELESTIAL ZONES IN OUR
GALAXY
- 2.1.Methodology and Techniques
- 2.1.1.Optical dust absorption
- 2.1.2.Infrared Dust Emission
- 2.1.3.Radio Zeeman Effect
- 2.1.4.Radio Faraday Rotation
- 2.2.Interstellar objects ( ~ 1 to
50 pc)
- 2.2.1.Excess line width
Wexcess relationship with Object size R
- 2.2.2.Globules and Magnetic
Fields
- 2.2.3.Narrow Magnetized Features
- 2.2.4.Magnetic field versus Gas
density, on medium linear scales (B ~ n0.5)
- 2.2.5.Magnetic field shapes in
Dusty Elongated Molecular Clouds
- 2.3.Interstellar Superbubbles and
shells with B ~ n1 (~ 50 to 500 pc)
- 2.4.Magnetic fields and Supernovae (B ~
n1)
- 2.5.The Center of the Milky Way
Galaxy's disk (~ 8 kpc away)
- 3.THE MILKY WAY AS A WHOLE
- 3.1.Magnetic fields and
Interstellar Superbubbles
- 3.2.Magnetic fields and Spiral Arms
(~ 15 kpc)
- 3.3.Distribution of Breg,
with galactic radius
- 3.3.1.Direction of
Breg
- 3.3.2.Location of zero
Breg
- 3.3.3.Strength of
Breg
- 3.4.Distribution of
Bran, and strength
- 3.5.Larger scale view - ASS or BSS
- 3.5.1.ASS for the Milky Way
- 3.5.2.Pitfalls of the BSS model
- 3.6.Seeds of galactic magnetism
- 3.6.1.Primordial cosmological
magnetic seeds in galaxies
- 3.6.2.Battery origin for
magnetic seeds in galaxies
- 3.6.3.Recent local origins for the
magnetic seeds in galaxies
- 3.7.Galactic Magnetic field
Interpretations - dynamos or not ?
- 3.7.1.Basic notions
- 3.7.2.Future trends in Galactic
Dynamos
- 4.NEARBY SPIRAL GALAXIES
- 4.1.Methodology - different methods
to obtain the magnetic field strength
- 4.1.1.Faraday Method
- 4.1.2.Equipartition Method
- 4.1.3.Cosmic-ray Method
- 4.1.4.Comparisons
- 4.2.Galactic magnetic field B and
star formation SF
- 4.2.1.Observed weak
relationship of B with SF
- 4.2.2.Expected weak relationship
of B with SF
- 4.2.3.Magnetic fields versus Gas
density, on large linear scales (B ~ n0.2)
- 4.2.4.Gas density versus Star
Formation
- 4.2.5.Magnetic fields in violent
star-forming (starburst) galaxies
- 4.3.Magnetic field shape in Andromeda
(M31) and other galaxies
- 4.4.Magnetic field B in galactic disks
and neutral hydrogen HI
- 4.4.1.B shapes and HI masses
- 4.4.2.B shapes and HI shapes -
companions or bars
- 4.5.Magnetic fields in Halos of
spiral galaxies
- 5.ELLIPTICAL GALAXIES, DISTANT GALAXIES,
CLUSTERS AND VOIDS, QUASARS AND COSMIC SCALES
- 5.1.Individual Galaxies and
quasars (~ 200 kpc)
- 5.2.Clusters of galaxies as the
largest magnets ( ~ 5 to 50 Mpc)
- 5.2.1.Several sources per
individual cluster of galaxies
- 5.2.2.One source per individual
cluster of galaxies
- 5.2.3.Seeds for magnetic fields in
clusters of galaxies
- 5.3.Large Scale Voids in space (~
100 to 200 Mpc)
- 5.4.Cosmological scales
- 5.4.1.Foreground Cosmological
Screen (~ 20 Gigaparsecs)
- 5.4.2.Background Cosmological
Surface ( ~ 8000 Gpc)
- 6.SUMMARY AND FUTURE TRENDS
- REFERENCES