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Milestones in the Observations of Cosmic Magnetic Fields
Open accessAbstract
Magnetic fields are observed everywhere in the universe. In this review, we concentrate on the observational aspects of the magnetic fields of Galactic and extragalactic objects. Readers can follow the milestones in the observations of cosmic magnetic fields obtained from the most important tracers of magnetic fields, namely, the star-light polarization, the Zeeman effect, the rotation measures (RMs, hereafter) of extragalactic radio sources, the pulsar RMs, radio polarization observations, as well as the newly implemented sub-mm and mm polarization capabilities. The magnetic field of the Galaxy was first discovered in 1949 by optical polarization observations. The local magnetic fields within one or two kpc have been well delineated by starlight polarization data. The polarization observations of diffuse Galactic radio background emission in 1962 confirmed unequivocally the existence of a Galactic magnetic field. The bulk of the present information about the magnetic fields in the Galaxy comes from analysis of rotation measures of extragalactic radio sources and pulsars, which can be used to construct the 3-D magnetic field structure in the Galactic halo and Galactic disk. Radio synchrotron spurs in the Galactic center show a poloidal field, and the polarization mapping of dust emission and Zeeman observation in the central molecular zone reveal a toroidal magnetic field parallel to the Galactic plane. For nearby galaxies, both optical polarization and multifrequency radio polarization data clearly show the large-scale magnetic field following the spiral arms or dust lanes. For more distant objects, radio polarization is the only approach available to show the magnetic fields in the jets or lobes of radio galaxies or quasars. Clusters of galaxies also contain widely distributed magnetic fields, which are reflected by radio halos or the RM distribution of background objects. The intergalactic space could have been magnetized by outflows or galactic superwinds even in the early universe. The Zeeman effect and polarization of sub-mm and mm emission can be used for the study of magnetic fields in some Galactic molecular clouds but it is observed only at high intensity. Both approaches together can clearly show the role that magnetic fields play in star formation and cloud structure, which in principle would be analogous to galaxy formation from protogalactic clouds. The origin of the cosmic magnetic fields is an active field of research. A primordial magnetic field has not been as yet directly detected, but its existence must be considered to give the seed field necessary for many amplification processes that have been developed. Possibly, the magnetic fields were generated in protogalactic plasma clouds by the dynamo process, and maintained again by the dynamo after galaxies were formed.
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Magnetogenesis and the primordial non-gaussianity
Seery, D. (2009) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2009/08/018 · Cited by 15
“Such magnetic fields are required by observation [7] and although a number of possible formation mechanisms are known — see, for example, ref.”
CMB limits on large-scale magnetic fields in an inhomogeneous universe
Clarkson, C., Coley, A. A., Maartens, R., & Tsagas, C. G. (2002) · CERN Document Server (European Organization for Nuclear Research) · Cited by 15
Cosmic magnetic fields from velocity perturbations in the early Universe
Betschart, G., Dunsby, P. K. S., & Marklund, M. (2003) · CERN Document Server (European Organization for Nuclear Research) · Cited by 15
Perturbations and non-Gaussianities in three-form inflationary magnetogenesis
Urban, F. R., & Koivisto, T. (2012) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2012/09/025 · Cited by 14
“Inflationary magnetogenesis has long been recognised as one of the most promising frameworks for the generation of today’s observed cosmological magnetic fields, see [1–5], and [6– 12].”
21 cm line signal from magnetic modes
Kunze, K. E. (2019) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2019/01/033 · Cited by 14
Polarization measurement analysis
Alina, D., Montier, L., Ristorcelli, I., Bernard, J.-P., Levrier, F., & Abdikamalov, E. B. (2016) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201628809 · Cited by 14
ESTIMATION OF MAGNETIC FIELD STRENGTH IN THE TURBULENT WARM IONIZED MEDIUM
Wu, Q., Kim, J., Ryu, D., Cho, J., & Alexander, P. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/705/1/l86 · Cited by 14
“The information on the field has been obtained through observations of Zeeman splitting, polarized thermal emission from dust, optical starlight polarization, radio synchrotron emission, and the Faraday rotation of polarized radio sources (see, Han & Wielebinski 2002, for a review).”
MethodLuo, J., Tu, L., Hu, Z.-K., & Luan, E.-J. (2003) · Physical Review Letters · doi:10.1103/physrevlett.91.149102 · Cited by 14
On the Magnetic Evolution in Friedmann Universes and the Question of Cosmic Magnetogenesis
Tsagas, C. G. (2016) · Symmetry · doi:10.3390/sym8110122 · Cited by 13
“The origin of cosmic magnetism remains an essentially open question despite the efforts and the established widespread presence of magnetic (B) fields in the universe [1–4].”
BackgroundGravitomagnetic amplification in cosmology
Tsagas, C. G. (2010) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.81.043501 · Cited by 13
Electroweak Baryogenesis and Primordial Hypermagnetic Fields
Piccinelli, G., & Ayala, A. (2004) · Lecture notes in physics · doi:10.1007/978-3-540-40918-2_11 · Cited by 13
Origin of primordial magnetic fields
de Souza, R. S., & Opher, R. (2008) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.77.043529 · Cited by 12
Galaxy Formation and Cosmic-Ray Acceleration in a Magnetized Universe
Vlahos, L., Tsagas, C. G., & Papadopoulos, D. (2005) · The Astrophysical Journal · doi:10.1086/444351 · Cited by 12
Estimation of Magnetic Field Strength in the Turbulent Warm Ionized MediumPreprint
Wu, Q., Kim, J., Ryu, D., Cho, J., & Alex, P. (2012) · Cited by 11
Cosmological Ohm's law and dynamics of non-minimal electromagnetism
Hollenstein, L., Jain, R. K., & Urban, F. R. (2013) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2013/01/013 · Cited by 7
“The strength of magnetic fields in galaxies and galaxy clusters is of the order of μGauss [1–4], and a lower bound of the order of 10−15 Gauss on coherent magnetic fields in the intergalactic medium has also been reported [5–9].”
Ayala, A., Bashir, A., & Sahu, S. (2004) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.69.045008 · Cited by 6
INTEGRATED OPTICAL POLARIZATION OF NEARBY GALAXIES
Jones, A. M., Wang, L., Krisciunas, K., & Freeland, E. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/748/1/17 · Cited by 5
“Galactic magnetic fields are toroidal (Han & Wielebinski 2002), so less inclined galaxies should have more of their polarization cancel out from the integration.”
BackgroundSeminal magnetic fields from inflato-electromagnetic inflation
Membiela, F. A., & Bellini, M. (2012) · The European Physical Journal C · doi:10.1140/epjc/s10052-012-2181-0 · Cited by 5
The very high energy gamma-ray spectra of AGN
Schroedter, M. (2004) · UA Campus Repository (The University of Arizona) · Cited by 5
Kislat, F. (2012) · DESY (CERN, DESY, Fermilab, IHEP, and SLAC) · doi:10.18452/16443 · Cited by 5
“The galactic magnetic field has a strength of roughly 3µG parallel to the spiral arms, but with large fluctuations (Han and Wielebinski, 2002).”
BackgroundSeminal magnetic fields from inflato-electromagnetic inflation
Membiela, F. A., & Bellini, M. (2012) · Conicet · Cited by 4
Magnetized cosmological perturbations in the post-recombination era
Vasileiou, H., & Tsagas, C. G. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv2418 · Cited by 3
Estimate of an environmental magnetic field of fast radio bursts
Lin, W., & Dai, Z.-G. (2016) · Research in Astronomy and Astrophysics · doi:10.1088/1674-4527/16/3/038 · Cited by 3
“On the other hand, since the MF equipartition is derived from radio synchrotron emission, it mainly reflects the field component perpendicular to the line of sight (Han & Wielebinski 2002).”
BackgroundSimulation Studies for Faraday Rotation Measure Observations
Xu, J., & Han, J. L. (2012) · Chinese Astronomy and Astrophysics · doi:10.1016/j.chinastron.2011.12.007 · Cited by 2
Self-citationRepeated Compton scattering in a strong magnetic field
Wang, P., Chou, C.-K., & Han, J. L. (2012) · Science China Physics Mechanics and Astronomy · doi:10.1007/s11433-012-4861-z · Cited by 2
Self-citationZweibel, E. G. (2010) · Proceedings of the International Astronomical Union · doi:10.1017/s1743921311017546 · Cited by 2
Large-scale magnetic fields in cosmology
Tsagas, C. G. (2009) · Plasma Physics and Controlled Fusion · doi:10.1088/0741-3335/51/12/124013 · Cited by 2
Large-scale magnetic fields in cosmologyPreprint
Tsagas, C. G. (2016) · Cited by 2
The mystery of cosmic magnetogenesis
Tsagas, C. G. (2012) · Proceedings of the International Astronomical Union · doi:10.1017/s1743921314011764 · Cited by 1
“The Milky Way and other spiral galaxies have coherent magnetic fields of μG-order magnitude, while galaxy clusters and remote protogalactic clouds also carry fields of similar strength (Han & Wielebinski 2002, Vallée 2011).”
BackgroundRelativistic magnetised perturbations: magnetic pressure versus magnetic tension
Tseneklidou, D., Tsagas, C. G., & Barrow, J. D. (2018) · Classical and Quantum Gravity · doi:10.1088/1361-6382/aac07f · Cited by 1
Zweibel, E. G. (2005) · The Fluid mechanics of astrophysics and geophysics/Fluid mechanics of astrophysics and geophysics · doi:10.1201/9780203017692.ch5 · Cited by 1
The SARAO MeerKAT Galactic Plane Survey filamentary source catalogue
Williams, G. M., Thompson, M. A., Mutale, M., Rigby, A. J., Bordiú, C., Riggi, S., Bietenholz, M. F., Anderson, L. D., Camilo, F., Goedhart, S., et al. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae2690 · Cited by 1
Beyond Classical Multipoles: The Magnetic Metapole as an Extended Field Source
Santis, A. D., & Dini, R. (2025) · Foundations · doi:10.3390/foundations5030025 · Cited by 1
Distribution of free electrons in the galactic plane
Andreasyan, R. R., Balayan, S. K., & Movsisyan, V. H. (2006) · Astrophysics · doi:10.1007/s10511-006-0025-z · Cited by 1
Magnetohydrodynamic flows as Newtonian-type gravitational motions
Spyrou, N., & Tsagas, C. G. (2010) · Open Physics · doi:10.2478/s11534-010-0004-1 · Cited by 1
Natural generation and amplification of magnetic seed fields
Dunsby, P. K. S., Betschart, G., & Zunckel, C. (2006) · General Relativity and Gravitation · doi:10.1007/s10714-006-0285-2
A brief history and background
Kronberg, P. P. (2015) · Cambridge University Press eBooks · doi:10.1017/cbo9780511977657.002
Relativistic magnetised perturbations: magnetic pressure versus magnetic tension
Tseneklidou, D., Tsagas, C. G., & Barrow, J. D. (2018) · Apollo (University of Cambridge) · doi:10.17863/cam.26176
Lectures on Astroparticle Physics
Günter Sigl, A. (2004) · CERN Document Server (European Organization for Nuclear Research)
Rohlfs, K., & Wilson, T. L. (2004) · Astronomy and astrophysics library · doi:10.1007/978-3-662-05394-2_3
From Magnetic Field Seeds to Planetary and Galactic Magnetism
Santis, A. D., Dini, R., & Cianchini, G. (2025) · Foundations · doi:10.3390/foundations5040032
“The magnetic field of the Milky Way has been extensively studied through radio observations and Faraday rotation measures [25].”
Metadata
- Authors
- Han, J.-L., & Wielebinski, R.
- Affiliations
- Chinese Academy of Sciences (CN)
- Max Planck Institute for Radio Astronomy (DE)
- ORCID
- Han, Jin-Lin
- Venue
- Chinese Journal of Astronomy and Astrophysics
- Publisher
- IOP Publishing
- Published
- 2002-08
- Volume
- 2
- Issue
- 4
- Pages
- 293-324
- ISSN
- 1009-9271 (ISSN-L)
- OpenAlex
- W2147397269
- Cited by
- 84
- References
- 282
- Citations by year
- 2025: 2 · 2024: 1 · 2019: 1 · 2018: 2 · 2017: 1 · 2016: 7 · 2015: 3 · 2014: 4 · 2013: 2 · 2012: 14
- FWCI
- 4.19
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Locations
- 天文和天体物理学研究：英文版 (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- CERN Document Server (European Organization for Nuclear Research) (submittedVersion)
- Max Planck Institute for Plasma Physics (submittedVersion)
- arXiv (Cornell University)
- Funders
- National Aeronautics and Space Administration
- National Natural Science Foundation of China
- Chinese Academy of Sciences
- National Astronomical Observatories, Chinese Academy of Sciences
- Topics
- Physical Sciences › Physics and Astronomy › Nuclear and High Energy Physics › Astrophysics and Cosmic Phenomena
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysical Phenomena and Observations
- Keywords
- galactic magnetic fields, stellar polarization, Zeeman effect, rotation measure, radio polarization, Galactic halo, Galactic disk, poloidal magnetic field, toroidal magnetic field, Central Molecular Zone, spiral arms, radio galaxies, quasars, galaxy clusters, radio halos, intergalactic magnetic fields, galactic superwinds, molecular clouds, star formation, dynamo, primordial magnetic fields
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