Cosmic Magnetic Fields

E. M. de Gouveia Dal Pino

REVIEW

Cosmic Magnetic Fields

E. M. de Gouveia Dal Pino

Astrophysics · Submitted 2 Mar 2006 · 36 references

Pith's verdict: Useful orientation review with no new science; the cluster/IGM field numbers are quoted too confidently and a few factual errors need fixing.

T0 · AI review

How this review was made: An AI referee (deepseek-v4-flash) read the paper on August 28, 2026 and answered a fixed list of questions about it. T0 is the starting level every paper gets. The levels describe how deeply Pith has checked the paper, never the authors.

T0 AI review An AI read the paper and answered a fixed list of questions.
T1 Audit Automatic checks that the references and files the paper relies on exist and match.
T2 Compute The paper's code or calculations re-run with the same results.
T3 Formal statement The claims written out in a formal math language a computer can read.
T4 Proof Those claims proved, and the proof checked by computer.

How Pith checks papers →

· 2 major objections · 6 minor · Ask about this paper · The compiled record · Read the full review →

Challenge this review Comment (0) Read on arXiv ↗

Cite ▾

arXiv IDastro-ph/0603065 (version 1)

Pith ID2LW2Z2IQ, Pith's permanent record of this paper and its review

CitationE. M. de Gouveia Dal Pino. "Cosmic Magnetic Fields." arXiv:astro-ph/0603065 (2006). https://pith.science/paper/2LW2Z2IQ

Cite this reviewBibTeX for Pith's review of this paper

Claim paper

Why Pith says this

Highlight any text to comment on it.

Editor's note

read the letter

This is an invited review lecture, not a research paper. There is no new derivation, dataset, or prediction; the novelty is zero by design. What it does well is organize the standard picture of cosmic magnetism in roughly ten pages: measurement techniques, stellar and compact objects, ISM/star formation, galaxies, clusters, the IGM, and early-universe generation mechanisms. A newcomer would come away with a serviceable map of the field circa 2006, and the references point to the main reviews. On those terms it earns its keep.

The soft spots are mostly in the quantitative claims. The stress-test note is right: the cluster and IGM field strengths come from Faraday rotation measures and carry degeneracies among B, n_e, path length, and field geometry, and the review quotes them as if they were firm. The IGM value is explicitly an upper limit, but the text later refers to the 'inferred IGM magnetic field' and builds the primordial discussion on it. A referee should ask for a caveat sentence. Relatedly, the Battaner & Florido suggestion that magnetic fields can explain flat rotation curves without dark matter is mentioned without noting that this is a minority view with serious objections. A review can include heterodox ideas, but it should flag their status.

There are also a couple of outright factual slips: the Milky Way is not a member of the Virgo Cluster, and a typical cluster diameter is about 1-10 Mpc, not 100 Mpc. Those should be fixed. Several numerical values appear with missing units or superscripts (e.g., 'B 30-50 G' presumably microgauss; 'BQCD = 108G' likely 10^8 G), which is partly an encoding artifact but worth cleaning up.

The central qualitative claim, that magnetic fields are dynamically important across many scales, is sound and well supported by the more robust Zeeman and synchrotron observations in stellar and galactic contexts. The Faraday-rotation concern weakens some specific numbers, not the broad synthesis.

Bottom line: this paper is for readers who want a quick orientation in cosmic magnetism, not for specialists seeking new results. It deserves a serious referee only in the sense that a careful editor would have it fact-checked before publication; the errors above are all catchable. I would not desk-reject it, but I would send it for light-touch review focused on accuracy.

Referee report

Major objections (2)

[Magnetic Fields in Clusters of Galaxies and the IGM and Magnetic Fields in the Early Universe] The cluster and IGM field strengths quoted in these sections are derived from Faraday rotation measures and depend on the assumed thermal electron density, path length, and coherence length, as well as on the field geometry; none of these systematic uncertainties is described. The IGM value is introduced as an upper limit ('BIGM ≤ 10-9 G, assuming a coherent length ... L≈ 1 Mpc'), but later in the same section and in the Early Universe section the text refers to 'the inferred IGM magnetic field' and compares model predictions to it (e.g., 'Bo(100 kpc) ≈ 10-9 G which is of the order of the predicted IGM field'). Since a change in the assumed coherence length by an order of magnitude would shift a random-field Faraday rotation estimate of B by a factor of about sqrt(10) ∼ 3, and comparable changes can arise from electron-density clumping, the current wording overstates the security of these numbers. Please either add an explicit systematic-error caveat when quoting these field strengths or consistently label them as upper limits/order-of-magnitude estimates, and avoid the phrase 'inferred IGM magnetic field' without qualification.
[Magnetic Fields in the Milky Way and Other Galaxies] The sentence citing Battaner & Florido (2000) that magnetic field forces 'are a competitive candidate to explain the observed flatness of rotation curves without the necessity of invoking the presence of dark matter' presents a non-mainstream suggestion without any caveat. This claim is not representative of the current consensus, is severely constrained by other observations, and is not needed for the section's main point about the importance of magnetic fields. The authors should either attribute it explicitly as a minority proposal with a brief discussion of the objections, or remove it, to avoid misleading readers of a review paper.

Minor objections (6)

[Magnetic Fields in the ISM and Star Formation Regions] The section on the ISM refers to 'Cructcher 2005'; the correct spelling is 'Crutcher'.
[Magnetic Fields in Clusters of Galaxies and the IGM] The cluster section mentions 'Abel clusters'; this should be 'Abell clusters'.
[Magnetic Fields in the Milky Way and Other Galaxies] The starburst galaxy referred to as 'NGC1067' in the section on galaxies is likely 'NGC1068', which should be verified.
[Magnetic Fields in the Early Universe] In the Early Universe section, the phrase 'hugh computational domains' should read 'huge computational domains.'
[Magnetic Fields in the Early Universe] Several mathematical quantities appear to be missing superscript formatting in the plain text (e.g., 'BQCD = 108G' and '10-9 G'); the published version should ensure these are properly rendered.
[References] The reference list entry for Totani is incomplete (it has only an arXiv ID); it should include a title and a journal reference (or be formatted consistently with the other entries).

How Pith checks papers → · Full audit of this paper →

The paper

The paper claims

Cosmic magnetic fields are active players at every scale, from stellar flares to galaxies and intergalactic space.

The reading

This invited review argues that most visible matter in the universe is magnetized plasma, and that magnetic fields are dynamically important from stellar surfaces to galaxy clusters and the intergalactic medium. It assembles the observational evidence from Zeeman splitting, synchrotron polarization, optical polarization, and Faraday rotation to give field strengths of roughly $9\,\mu$G in spiral galaxies, $30$–$50\,\mu$G in starbursts, a few $\mu$G in clusters, and at most about $10^{-9}$ G in the diffuse intergalactic medium. Theoretically, it argues that flux freezing makes cosmic fields long-lived once created, and that dynamo action plus seed mechanisms such as the Biermann battery and the Harrison effect can explain their origin, with primordial fields constrained by the cosmic microwave background and big-bang nucleosynthesis. If the synthesis is correct, magnetism must be included in models of star formation, jet launching, cosmic-ray transport, and galaxy and cluster evolution.

What carries the argument

The carrying object is the magnetic induction equation, written in the paper as $\partial \mathbf{B}/\partial t = \nabla\times(\mathbf{v}\times\mathbf{B})$ plus a diffusion term; in most cosmic plasmas the diffusion time is far longer than dynamical times, so flux freezing makes fields persist once created. The second workhorse is the dynamo mechanism, which converts the kinetic energy of turbulent or differentially rotating flows into magnetic energy through the $\alpha$ and omega effects, and the observational diagnostics (Zeeman splitting, synchrotron polarization, optical polarization by aligned dust, and Faraday rotation) that convert measured radiation into field strengths.

Extended reading notes

Core claim

The paper's central claim is that magnetic fields are not passive tracers but active dynamical agents across the cosmos. The author gathers measurements showing coherent fields of roughly $100\,\mu$G to a few mG in molecular cloud cores, average fields near $9\,\mu$G across 74 spiral galaxies, $30$–$50\,\mu$G in starburst galaxies, $2$–$30\,\mu$G in galaxy clusters, and an upper limit near $10^{-9}$ G for the intergalactic medium. Alongside these numbers, the review invokes the magnetic induction equation to argue that flux freezing makes magnetic fields extremely difficult to destroy in astrophysical plasmas, and that dynamo mechanisms can amplify weak seeds to observed strengths; it also catalogs proposed seed-field sources, from the Biermann battery and Harrison vortices to the QCD phase transition and inflation, with CMBR and BBN upper limits bounding any primordial component. The paper thus aims to establish a unified picture in which magnetic fields matter for star formation, solar and stellar activity, pulsars, accretion disks, jets, cosmic rays, and galactic-disk stability.

Load-bearing premise

The whole quantitative picture rests on the assumption that Faraday rotation and the other standard diagnostics measure the true ambient field without systematic bias, which requires assuming electron densities and path lengths that, if wrong, would change every inferred field strength.

Editorial extensions

If this is right

Magnetic fields must be included in models of star formation: molecular cloud cores are magnetically supported, with gravitational collapse driven by ambipolar diffusion and angular momentum removed by magnetic braking.
The flat outer rotation curves of some disk galaxies could be explained by magnetic forces, offering a partial alternative to dark matter in those systems.
Galactic and cluster magnetic fields can be understood as dynamo-amplified products of weak seed fields, so a primordial field is not required even though it is not excluded.
Reconnection episodes in accretion disks, analogous to solar flares, may power the observed X-ray and radio flares and relativistic ejections in jet sources.
Higher-resolution polarization maps and a much larger sample of pulsar rotation measures will settle whether the Milky Way's multiple large-scale field reversals are real or local distortions.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

A testable extension is that if magnetic braking truly regulates protogalactic collapse, observed magnetic-field strengths in high-redshift galaxies should scale with star-formation rate, a correlation the next-generation radio arrays could test.
The review leaves implicit that the solar-flare to accretion-disk-flare analogy implies a common reconnection mechanism whose occurrence rate should scale predictably with disk magnetization; comparing flare statistics across stellar and supermassive-black-hole systems would test it.
The intergalactic upper limit near $10^{-9}$ G is a constraint rather than a detection; future gamma-ray or low-frequency radio observations could either confirm a floor or push the limit lower, changing which seed mechanisms remain viable.

Original abstract

Most of the visible matter in the Universe is in a plasma state, or more specifically is composed of ionized or partially ionized gas permeated by magnetic fields. Thanks to recent advances on the theory and detection of cosmic magnetic fields there has been a worldwide growing interest in the study of their role on the formation of astrophysical sources and the structuring of the Universe. In this lecture, I will briefly review the importance of the cosmic magnetic fields both from a theoretical and from an observational perspective, particularly focusing on stellar and compact objects, the interstellar medium and star formation regions, and on galaxies, clusters of galaxies, and the primordial Universe.

The compiled record

The paper's own sentences, arranged, kept beside the review and separate from it. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.

Compiled by classifier-1.13.0 via TypeSafe API, question bank abstract-p1-20260923, 2026-09-23: 1 request, 3,042 input tokens.

What the abstract itself states, as probabilities: claims first 0.02 · states limitation 0.12 · human participants 0.02 · controlled comparison 0.01 · randomized assignment 0.01 · states quantitative result 0.02 · compares with prior results 0.03 · mentions code or data availability 0.02.

The abstract, sentence by sentence

arXiv listing abstract v1. Results and the main claim are underlined; show every role.

Most of the visible matter in the Universe is in a plasma state, or more specifically is composed of ionized or partially ionized gas permeated by magnetic fields. Thanks to recent advances on the theory and detection of cosmic magnetic fields there has been a worldwide growing interest in the study of their role on the formation of astrophysical sources and the structuring of the Universe. In this lecture, I will briefly review the importance of the cosmic magnetic fields both from a theoretical and from an observational perspective, particularly focusing on stellar and compact objects, the interstellar medium and star formation regions, and on galaxies, clusters of galaxies, and the primordial Universe.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#	sentence	role	the authors' own work	states the main conclusion	strength
s0	Most of the visible matter in the Universe is in a plasma state, or more specifically is composed of ionized or partially ionized gas permeated by magnetic fields.	background 1.00	0.04	0.05	asserted 1.00
s1	Thanks to recent advances on the theory and detection of cosmic magnetic fields there has been a worldwide growing interest in the study of their role on the formation of astrophysical sources and the structuring of the Universe.	background 1.00	0.04	0.05	asserted 1.00
s2	In this lecture, I will briefly review the importance of the cosmic magnetic fields both from a theoretical and from an observational perspective, particularly focusing on stellar and compact objects, the interstellar medium and star formation regions, and on galaxies, clusters of galaxies, and the primordial Universe.	contribution 0.95	0.20	0.07	asserted 0.57

What kind of paper the classifier reports this is: review 1.00 · evidence from literature 0.95.

What was examined, and what was not

sources read

arXiv listing abstract v1

not examined

full text
figures and tables
references and citing sentences
relations to other papers

levels run

P abstract

not run

S sections
T body sentences
C citations
R cross-paper relations

Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

References

Works cited (36)

[1]

F. Bacciotti, T. P. Ray, R. Mundt, J. Eislöffel, and J. Solf, , ApJ, 2002, 576, 222

View on Pith 2002
[2]

E. Battaner, and E. Florido, Fundamentals of Cosmic Fields, 2000, 21, 1-154

View on Pith 2000
[3]

R. Beck, in Magnetic Fields in the Universe: from Laboratory and Stars to Primordial Structures, edited by E. M. de Gouveia Dal Pino, G. Lugones and A. Lazarian, AIP Conference Proceedings 784, American Institute of Physics, Melville, NY, 2005a, pp. 453-355

View on Pith
[4]

R. Beck, in Magnetic Fields in the Universe: from Laboratory and Stars to Primordial Structures, edited by E. M. de Gouveia Dal Pino, G. Lugones and A. Lazarian, AIP Conference Proceedings 784, American Institute of Physics, Melville, NY, 2005b, pp. 343-353

View on Pith
[5]

Blandford, R.D. & Payne, D.G. MNRAS, 1982, 199

View on Pith 1982
[6]

H. Carmichael, in Proc. of AAS-NASA Symp. on the Physics of Solar Flares, Edited by W. N. Hess, NASA-SP 50, p. 451

View on Pith
[7]

R. M. Crutcher, in Magnetic Fields in the Universe: from Laboratory and Stars to Primordial Structures, edited by E. M. de Gouveia Dal Pino, G. Lugones and A. Lazarian, AIP Conference Proceedings 784, American Institute of Physics, Melville, NY, 2005, pp. 129-139

View on Pith 2005
[8]

E. M. de Gouveia Dal Pino, in Magnetic Fields in the Universe: from Laboratory and Stars to Primordial Structures, edited by E. M. de Gouveia Dal Pino, G. Lugones and A. Lazarian, AIP Conference Proceedings 784, American Institute of Physics, Melville, NY, 2005a, pp. 183-194

View on Pith
[9]

E. M. de Gouveia Dal Pino, Advances in Space Research, 2005b, 35, 908-924

View on Pith
[10]

E. M. de Gouveia Dal Pino, 2006a, Braz. J. Phys. (in press)

View on Pith
[11]

E. M. de Gouveia Dal Pino, in Cosmic Magnetic Fields, edited by R. Beck et al., 2006b, Astron. Nachr, 2006 (in press)

View on Pith 2006
[12]

E. M. de Gouveia Dal Pino and A. Lazarian, A&A, 2005, 441, 845-853

View on Pith 2005
[13]

R.-J. Dettmar, in Magnetic Fields in the Universe: from Laboratory and Stars to Primordial Structures, edited by E. M. de Gouveia Dal Pino, G. Lugones and A. Lazarian, AIP Conference Proceedings 784, American Institute of Physics, Melville, NY, 2005a, pp. 354-361

View on Pith
[14]

T. A. Ensslin, C. Vogt, and C. Pfrommer, in The Magnetized Plasma in Galaxy Evolution, edited by K. T. Chyzy et al., Jagiellonian University, Krakow, 2005, 231-238

View on Pith 2005
[15]

F. Govoni et al., in Cosmic Magnetic Fields, edited by R. Beck et al., 2006, Astron. Nachr, 2006 (in press)

View on Pith 2006
[16]

D. Grasso, and H.R. Rubinstein, Physics Reports, 2001, 348, 163-266

View on Pith 2001
[17]

D. Grasso, in Cosmic Magnetic Fields, edited by R. Beck et al., 2006, Astron. Nachr, 2006 (in press)

View on Pith 2006
[18]

G. A. Guerrero and E. M. de Gouveia Dal Pino, 2006 (in prep.)

View on Pith 2006
[19]

E.R. Harrison, Mon. Not. R. Astron. Soc., 1970, 147, 279

View on Pith 1970
[20]

Y. Kato, S., Mineshige, and K. Shibata, ApJ, 2004, 605, 307

View on Pith 2004
[21]

J. Kim et al., in Cosmic Magnetic Fields, edited by R. Beck et al., 2006, Astron. Nachr, 2006 (in press)

View on Pith 2006
[22]

A. Königl, A., and R. Pudritz, in Protostars and Planets IV, (Book - Tucson: University of Arizona Press); edited by Mannings, V., Boss, A.P., Russell, S. S., 2000, p. 759

View on Pith 2000
[23]

P. P. Kronberg, in in The Magnetized Plasma in Galaxy Evolution, edited by K. T. Chyzy et al., Jagiellonian University, Krakow, 2005, 239-246

View on Pith 2005
[24]

P. P. Kronberg, H. Lesch and U. Hopp, ApJ, 1999, 511, 56

View on Pith 1999
[25]

Zhi-Yun, Li, and F. H. Shu, ApJ, 1996, 468, 261

View on Pith 1996
[26]

A. M. Magalhães et al., in Magnetic Fields in the Universe: from Laboratory and Stars to Primordial Structures, edited by E. M. de Gouveia Dal Pino, G. Lugones and A. Lazarian, AIP Conference Proceedings 784, American Institute of Physics, Melville, NY, 2005, pp. 715-720

View on Pith 2005
[27]

C. Melioli, E.M. de Gouveia Dal Pino, and A. Raga, A&A, A&A, 2005, 443, 495-508

View on Pith 2005
[28]

C. Melioli, A. D’Ercoli, E.M. de Gouveia Dal Pino, F. Brighentti, and A. Raga, 2006 (in prep.)

View on Pith 2006
[29]

M. Rees, in Cosmic Magnetic Fields, edited by R. Beck et al., 2006, Astron. Nachr, 2006 (in press)

View on Pith 2006
[30]

M. Shaposhnikov, in Magnetic Fields in the Universe: from Laboratory and Stars to Primordial Structures, edited by E. M. de Gouveia Dal Pino, G. Lugones and A. Lazarian, AIP Conference Proceedings 784, American Institute of Physics, Melville, NY, 2005, pp. 423-433

View on Pith 2005
[31]

K. Shibata, in Magnetic Fields in the Universe: from Laboratory and Stars to Primordial Structures, edited by E. M. de Gouveia Dal Pino, G. Lugones and A. Lazarian, AIP Conference Proceedings 784, American Institute of Physics, Melville, NY, 2005, pp. 153-163

View on Pith 2005
[32]

G. Sigl,A. Olinto, K. Jedamzik, Phys. Rev. D 55 (1997) 4582

View on Pith 1997
[33]

A. V. R. Silva, in Magnetic Fields in the Universe: from Laboratory and Stars to Primordial Structures, edited by E. M. de Gouveia Dal Pino, G. Lugones and A. Lazarian, AIP Conference Proceedings 784, American Institute of Physics, Melville, NY, 2005, pp. 90-102

View on Pith 2005
[34]

K. Subramanian, MNRAS, 1998, 294, 718

View on Pith 1998
[35]

T. Totani,[astro-ph/9904042]

View on Pith Pith review arXiv
[36]

M. S. Turner and L. M. Widrow, Phys. Rev. D, 1988, 37, 2743

View on Pith 1988

How the literature uses it

1 arXiv paper cite this in 1 sentence

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

Discussion

Disagree with the review, or know something it missed? Leave a comment, highlight any passage above to comment on it, or challenge this review formally.

[1] [1]

F. Bacciotti, T. P. Ray, R. Mundt, J. Eislöffel, and J. Solf, , ApJ, 2002, 576, 222

View on Pith 2002

[2] [2]

E. Battaner, and E. Florido, Fundamentals of Cosmic Fields, 2000, 21, 1-154

View on Pith 2000

[3] [3]

R. Beck, in Magnetic Fields in the Universe: from Laboratory and Stars to Primordial Structures, edited by E. M. de Gouveia Dal Pino, G. Lugones and A. Lazarian, AIP Conference Proceedings 784, American Institute of Physics, Melville, NY, 2005a, pp. 453-355

View on Pith

[4] [4]

R. Beck, in Magnetic Fields in the Universe: from Laboratory and Stars to Primordial Structures, edited by E. M. de Gouveia Dal Pino, G. Lugones and A. Lazarian, AIP Conference Proceedings 784, American Institute of Physics, Melville, NY, 2005b, pp. 343-353

View on Pith

[5] [5]

Blandford, R.D. & Payne, D.G. MNRAS, 1982, 199

View on Pith 1982

[6] [6]

H. Carmichael, in Proc. of AAS-NASA Symp. on the Physics of Solar Flares, Edited by W. N. Hess, NASA-SP 50, p. 451

View on Pith

[7] [7]

R. M. Crutcher, in Magnetic Fields in the Universe: from Laboratory and Stars to Primordial Structures, edited by E. M. de Gouveia Dal Pino, G. Lugones and A. Lazarian, AIP Conference Proceedings 784, American Institute of Physics, Melville, NY, 2005, pp. 129-139

View on Pith 2005

[8] [8]

E. M. de Gouveia Dal Pino, in Magnetic Fields in the Universe: from Laboratory and Stars to Primordial Structures, edited by E. M. de Gouveia Dal Pino, G. Lugones and A. Lazarian, AIP Conference Proceedings 784, American Institute of Physics, Melville, NY, 2005a, pp. 183-194

View on Pith

[9] [9]

E. M. de Gouveia Dal Pino, Advances in Space Research, 2005b, 35, 908-924

View on Pith

[10] [10]

E. M. de Gouveia Dal Pino, 2006a, Braz. J. Phys. (in press)

View on Pith

[11] [11]

E. M. de Gouveia Dal Pino, in Cosmic Magnetic Fields, edited by R. Beck et al., 2006b, Astron. Nachr, 2006 (in press)

View on Pith 2006

[12] [12]

E. M. de Gouveia Dal Pino and A. Lazarian, A&A, 2005, 441, 845-853

View on Pith 2005

[13] [13]

R.-J. Dettmar, in Magnetic Fields in the Universe: from Laboratory and Stars to Primordial Structures, edited by E. M. de Gouveia Dal Pino, G. Lugones and A. Lazarian, AIP Conference Proceedings 784, American Institute of Physics, Melville, NY, 2005a, pp. 354-361

View on Pith

[14] [14]

T. A. Ensslin, C. Vogt, and C. Pfrommer, in The Magnetized Plasma in Galaxy Evolution, edited by K. T. Chyzy et al., Jagiellonian University, Krakow, 2005, 231-238

View on Pith 2005

[15] [15]

F. Govoni et al., in Cosmic Magnetic Fields, edited by R. Beck et al., 2006, Astron. Nachr, 2006 (in press)

View on Pith 2006

[16] [16]

D. Grasso, and H.R. Rubinstein, Physics Reports, 2001, 348, 163-266

View on Pith 2001

[17] [17]

D. Grasso, in Cosmic Magnetic Fields, edited by R. Beck et al., 2006, Astron. Nachr, 2006 (in press)

View on Pith 2006

[18] [18]

G. A. Guerrero and E. M. de Gouveia Dal Pino, 2006 (in prep.)

View on Pith 2006

[19] [19]

E.R. Harrison, Mon. Not. R. Astron. Soc., 1970, 147, 279

View on Pith 1970

[20] [20]

Y. Kato, S., Mineshige, and K. Shibata, ApJ, 2004, 605, 307

View on Pith 2004

[21] [21]

J. Kim et al., in Cosmic Magnetic Fields, edited by R. Beck et al., 2006, Astron. Nachr, 2006 (in press)

View on Pith 2006

[22] [22]

A. Königl, A., and R. Pudritz, in Protostars and Planets IV, (Book - Tucson: University of Arizona Press); edited by Mannings, V., Boss, A.P., Russell, S. S., 2000, p. 759

View on Pith 2000

[23] [23]

P. P. Kronberg, in in The Magnetized Plasma in Galaxy Evolution, edited by K. T. Chyzy et al., Jagiellonian University, Krakow, 2005, 239-246

View on Pith 2005

[24] [24]

P. P. Kronberg, H. Lesch and U. Hopp, ApJ, 1999, 511, 56

View on Pith 1999

[25] [25]

Zhi-Yun, Li, and F. H. Shu, ApJ, 1996, 468, 261

View on Pith 1996

[26] [26]

A. M. Magalhães et al., in Magnetic Fields in the Universe: from Laboratory and Stars to Primordial Structures, edited by E. M. de Gouveia Dal Pino, G. Lugones and A. Lazarian, AIP Conference Proceedings 784, American Institute of Physics, Melville, NY, 2005, pp. 715-720

View on Pith 2005

[27] [27]

C. Melioli, E.M. de Gouveia Dal Pino, and A. Raga, A&A, A&A, 2005, 443, 495-508

View on Pith 2005

[28] [28]

C. Melioli, A. D’Ercoli, E.M. de Gouveia Dal Pino, F. Brighentti, and A. Raga, 2006 (in prep.)

View on Pith 2006

[29] [29]

M. Rees, in Cosmic Magnetic Fields, edited by R. Beck et al., 2006, Astron. Nachr, 2006 (in press)

View on Pith 2006

[30] [30]

M. Shaposhnikov, in Magnetic Fields in the Universe: from Laboratory and Stars to Primordial Structures, edited by E. M. de Gouveia Dal Pino, G. Lugones and A. Lazarian, AIP Conference Proceedings 784, American Institute of Physics, Melville, NY, 2005, pp. 423-433

View on Pith 2005

[31] [31]

K. Shibata, in Magnetic Fields in the Universe: from Laboratory and Stars to Primordial Structures, edited by E. M. de Gouveia Dal Pino, G. Lugones and A. Lazarian, AIP Conference Proceedings 784, American Institute of Physics, Melville, NY, 2005, pp. 153-163

View on Pith 2005

[32] [32]

G. Sigl,A. Olinto, K. Jedamzik, Phys. Rev. D 55 (1997) 4582

View on Pith 1997

[33] [33]

A. V. R. Silva, in Magnetic Fields in the Universe: from Laboratory and Stars to Primordial Structures, edited by E. M. de Gouveia Dal Pino, G. Lugones and A. Lazarian, AIP Conference Proceedings 784, American Institute of Physics, Melville, NY, 2005, pp. 90-102

View on Pith 2005

[34] [34]

K. Subramanian, MNRAS, 1998, 294, 718

View on Pith 1998

[35] [35]

T. Totani,[astro-ph/9904042]

View on Pith Pith review arXiv

[36] [36]

M. S. Turner and L. M. Widrow, Phys. Rev. D, 1988, 37, 2743

View on Pith 1988