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B", volume = "281", year = "1992", pages = "300-302", doi = "10.1016/0370-2693(92)91144-X", reportNumber = "NBI-HE-92-13", SLACcitation = "%%CITATION = PHLTA,B281,300;%%" } @inproceedings{Enqvist:1994dq, author = "Enqvist, Kari", title = "{On primordial magnetic fields}", booktitle = "{1st International Conference on Strong and Electroweak Matter (SEWM 1994) Sintra, Portugal, March 23-25, 1994}", year = "1994", pages = "143-154", eprint = "hep-ph/9405315", archivePrefix = "arXiv", primaryClass = "hep-ph", reportNumber = "NORDITA-94-6-P-A", SLACcitation = "%%CITATION = HEP-PH/9405315;%%" } @article{Enqvist:1993np, author = "Enqvist, K. and Olesen, P.", title = "{On primordial magnetic fields of electroweak origin}", journal = "Phys. Lett. B", volume = "319", year = "1993", pages = "178-185", doi = "10.1016/0370-2693(93)90799-N", eprint = "hep-ph/9308270", archivePrefix = "arXiv", primaryClass = "hep-ph", reportNumber = "NBI-HE-93-33", SLACcitation = "%%CITATION = HEP-PH/9308270;%%" } @ARTICLE{Caprini:2009pr, author = {Caprini, Chiara and Durrer, Ruth and Fenu, Elisa}, title = {{Can the observed large scale magnetic fields be seeded by helical primordial fields?}}, journal = {JCAP}, year = {2009}, volume = {0911}, pages = {001}, abstrct = {Gravitational wave production induces a strong constraint on the amplitude of a primordial magnetic field. It has been shown that the nucleosynthesis bound for a stochastic gravitational wave background implies that causally generated fields cannot have enough power on large scales to provide the seeds necessary for the observed magnetic fields in galaxies and clusters, even by the most optimistic dynamo amplification. Magnetic fields generated at inflation can have high enough amplitude only if their spectrum is very red. Here we show that helicity, which leads to an inverse cascade, can mitigate these limits. In particular, we find that helical fields generated at the QCD phase transition or at inflation with red spectrum are possible seeds for the dynamo. Helical fields generated at the electroweak phase transition are instead excluded as seeds at large scales. We also calculate the spectrum of gravitational waves generated by helical magnetic fields. }, archiveprefix = {arXiv}, doi = {10.1088/1475-7516/2009/11/001}, eprint = {0906.4976}, primaryclass = {astro-ph.CO}, slaccitation = {%%CITATION = 0906.4976;%%} } @ARTICLE{Durrer:2003ja, author = {Durrer, Ruth and Caprini, Chiara}, title = {{Primordial Magnetic Fields and Causality}}, journal = {JCAP}, year = {2003}, volume = {0311}, pages = {010}, abstract = {We discuss the implications of causality on a primordial magnetic field. We show that the residual field on large scales is much more suppressed than usually assumed and that a helical component is even more reduced. Due to this strong suppression, even maximal primordial fields generated at the electroweak phase transition can just marginally seed the fields in clusters, but they cannot leave any detectable imprint on the cosmic microwave background.}, archiveprefix ={arXiv}, doi = {10.1088/1475-7516/2003/11/010}, eprint = {astro-ph/0305059}, slaccitation = {%%CITATION = ASTRO-PH/0305059;%%} } @ARTICLE{Saveliev:2012ea, author = {Saveliev, Andrey and Jedamzik, Karsten and Sigl, Gunter}, title = {{Time Evolution of the Large-Scale Tail of Non-Helical Primordial Magnetic Fields with Back-Reaction of the Turbulent Medium}}, journal = {Phys. Rev. D}, year = {2012}, volume = {86}, pages = {103010}, abstract = { We present a derivation of the time evolution equations for the energy content of nonhelical magnetic fields and the accompanying turbulent flows from first principles of incompressible magnetohydrodynamics in the general framework of homogeneous and isotropic turbulence. This is then applied to the early Universe, i.e., the evolution of primordial magnetic fields. Numerically integrating the equations, we find that most of the energy is concentrated at an integral wavenumber scale k_I where the turbulence turn over time equals the Hubble time. At larger length scales L, i.e., smaller wavenumbers q = 2 \pi / L << k_I, independent of the assumed turbulent flow power spectrum, mode-mode coupling tends to develop a small q magnetic field tail with a Batchelor spectrum proportional to the fourth inverse power of L and therefore a scaling for the magnetic field of B ~ L^(-5/2). }, archiveprefix = {arXiv}, doi = {10.1103/PhysRevD.86.103010}, eprint = {1208.0444}, primaryclass = {astro-ph.CO}, reportnumber = {DESY-12-131}, slaccitation = {%%CITATION = ARXIV:1208.0444;%%}, texkey = {Saveliev:2012ea} } @ARTICLE{Tavecchio:10, author = {Tavecchio, F. and others}, title = {{The intergalactic magnetic field constrained by Fermi/LAT observations of the TeV blazar 1ES 0229+200}}, journal = {\mnras}, year = {2010}, volume = {406}, pages = {L70-L74}, abstract = {TeV photons from blazars at relatively large distances, interacting with the optical-IR cosmic background, are efficiently converted into electron-positron pairs. The produced pairs are extremely relativistic (Lorentz factors of the order of 1e6 1e7 and promptly loose their energy through inverse Compton scatterings with the photons of the microwave cosmic background, producing emission in the GeV band. The spectrum and the flux level of this reprocessed emission is critically dependent on the intensity of the intergalactic magnetic field, B, that can deflect the pairs diluting the intrinsic emission over a large solid angle. We derive a simple relation for the reprocessed spectrum expected from a steady source. We apply this treatment to the blazar 1ES 0229+200, whose intrinsic very hard TeV spectrum is expected to be approximately steady. Comparing the predicted reprocessed emission with the upper limits measured by the Fermi/Large Area Telescope, we constrain the value of the intergalactic magnetic field to be larger than $B \simeq 5\times 10^{-15}$ Gauss, depending on the model of extragalactic background light.}, archiveprefix ={arXiv}, doi = {10.1111/j.1745-3933.2010.00884.x}, eprint = {1004.1329}, primaryclass = {astro-ph.CO}, slaccitation = {%%CITATION = 1004.1329;%%} } @ARTICLE{Dolag:10, author = {K. Dolag and M. Kachelriess and S. Ostapchenko and R. Tomas}, title = {{Lower limit on the strength and filling factor of extragalactic magnetic fields}}, journal = {\apj}, year = {2011}, volume = {727}, pages = {L4}, month = sep, __markedentry = {[ruchay]}, abstract = {High energy photons from blazars can initiate electromagnetic pair cascades interacting with the extragalactic photon background. The charged component of such cascades is deflected and delayed by extragalactic magnetic fields (EGMF), reducing thereby the observed point-like flux and leading potentially to multi degree images in the GeV energy range. We calculate the fluence of 1ES 0229+200 as seen by Fermi-LAT for different EGMF profiles using a Monte Carlo simulation for the cascade development. The non-observation of 1ES 0229+200 by Fermi-LAT suggests that the EGMF fills at least 60% of space with fields stronger than {\cal O}(10^{-16}-10^{-15})G for life times of TeV activity of {\cal O}(10^2-10^4)yr. Thus the (non-) observation of GeV extensions around TeV blazars probes the EGMF in voids and puts strong constraints on the origin of EGMFs: Either EGMFs were generated in a space filling manner (e.g. primordially) or EGMFs produced locally (e.g. by galaxies) have to be efficiently transported to fill a significant volume fraction, as e.g. by galactic outflows.}, comments = {5 pages, 5 eps figures; v2: added discussion of time delays}, eprint = {1009.1782}, oai2identifier = {1009.1782}, owner = {ruchay}, slaccitation = {%%CITATION = 1009.1782;%%}, timestamp = {2011-01-25} } @article{Semikoz:2012ka, author = "Semikoz, V.B. and Sokoloff, D.D. and Valle, J.W.F.", title = "{Lepton asymmetries and primordial hypermagnetic helicity evolution}", journal = "JCAP", volume = "1206", pages = "008", doi = "10.1088/1475-7516/2012/06/008", year = "2012", eprint = "1205.3607", archivePrefix ="arXiv", primaryClass = "astro-ph.CO", reportNumber = "IFIC-12-33", texkey = "Semikoz:2012ka", SLACcitation = "%%CITATION = ARXIV:1205.3607;%%", } @ARTICLE{Giovannini:1997eg, author = {Giovannini, Massimo and Shaposhnikov, M. E.}, title = {{Primordial hypermagnetic fields and triangle anomaly}}, journal = {Phys. Rev. D}, year = {1998}, volume = {57}, pages = {2186-2206}, archiveprefix ={arXiv}, doi = {10.1103/PhysRevD.57.2186}, eprint = {hep-ph/9710234}, slaccitation = {%%CITATION = HEP-PH/9710234;%%} } @article{PRPLM99, author = {J. A. Pons and S. Reddy and M. Prakash and J. M. Lattimer and J. A. Miralles}, title = {Evolution of Proto-Neutron Stars}, journal = {ApJ}, volume = {513}, number = {2}, pages = {780}, url = {http://stacks.iop.org/0004-637X/513/i=2/a=780}, year = {1999}, abstract = {We study the thermal and chemical evolution during the Kelvin-Helmholtz phase of the birth of a neutron star, employing neutrino opacities that are consistently calculated with the underlying equation of state (EOS). Expressions for the diffusion coefficients appropriate for general relativistic neutrino transport in the equilibrium diffusion approximation are derived. The diffusion coefficients are evaluated using a field-theoretical finite-temperature EOS that includes the possible presence of hyperons. The variation of the diffusion coefficients is studied as a function of EOS and compositional parameters. We present results from numerical simulations of proto-neutron star cooling for internal stellar properties as well as emitted neutrino energies and luminosities. We discuss the influence of the initial stellar model, the total mass, the underlying EOS, and the addition of hyperons on the evolution of the proto-neutron star and on the expected signal in terrestrial detectors. We find that the differences in predicted luminosities and emitted neutrino energies do not depend much upon the details of the initial models or the underlying high-density EOS for early times ( t <10 s), provided that opacities are calculated consistently with the EOS. The same holds true for models that allow for the presence of hyperons, except when the initial mass is significantly larger than the maximum mass for cold, catalyzed matter. For times larger than about 10 s, and prior to the occurrence of neutrino transparency, the neutrino luminosities decay exponentially with a time constant that is sensitive to the high-density properties of matter. We also find the average emitted neutrino energy increases during the first 5 s of evolution and then decreases nearly linearly with time. In general, increasing the proto-neutron star mass increases the average energy and the luminosity of neutrinos, as well as the overall evolutionary timescale. The influence of hyperons or variations in the dense matter EOS is increasingly important at later times. Metastable stars, those with hyperons that are unstable to collapse upon deleptonization, have relatively long evolution times, which increase the nearer the mass is to the maximum mass supportable by a cold, deleptonized star.} } @article{Prakash:1996xs, author = "Prakash, Madappa and Bombaci, Ignazio and Prakash, Manju and Ellis, Paul J. and Lattimer, James M. and Knorren, Roland", title = "{Composition and structure of protoneutron stars}", journal = "Phys. Rept.", volume = "280", year = "1997", pages = "1-77", doi = "10.1016/S0370-1573(96)00023-3", eprint = "nucl-th/9603042", archivePrefix ="arXiv", primaryClass = "nucl-th", reportNumber = "SUNY-NTG-96-11, NUC-MINN-93-23-T", SLACcitation = "%%CITATION = NUCL-TH/9603042;%%" } @article{Yamamoto:2015gzz, author = "Yamamoto, Naoki", title = "{Chiral transport of neutrinos in supernovae: Neutrino-induced fluid helicity and helical plasma instability}", journal = "Phys. Rev. D", volume = "93", year = "2016", number = "6", pages = "065017", doi = "10.1103/PhysRevD.93.065017", eprint = "1511.00933", archivePrefix ="arXiv", primaryClass = "astro-ph.HE", SLACcitation = "%%CITATION = ARXIV:1511.00933;%%" } @article{Ohnishi:2014uea, author = "Ohnishi, Akira and Yamamoto, Naoki", title = "{Magnetars and the Chiral Plasma Instabilities}", year = "2014", eprint = "1402.4760", archivePrefix = "arXiv", primaryClass = "astro-ph.HE", reportNumber = "YITP-14-14", SLACcitation = "%%CITATION = ARXIV:1402.4760;%%" } @article{Boyarsky:2012ex, author = "Boyarsky, Alexey and Ruchayskiy, Oleg and Shaposhnikov, Mikhail", title = "{Long-range magnetic fields in the ground state of the Standard Model plasma}", journal = "Phys. Rev. Lett.", volume = "109", year = "2012", pages = "111602", doi = "10.1103/PhysRevLett.109.111602", eprint = "1204.3604", archivePrefix ="arXiv", primaryClass = "hep-ph", reportNumber = "CERN-PH-TH-2012-112", SLACcitation = "%%CITATION = ARXIV:1204.3604;%%" } @article{Charbonneau:2009ax, author = "Charbonneau, James and Zhitnitsky, Ariel", title = "{Topological Currents in Neutron Stars: Kicks, Precession, Toroidal Fields, and Magnetic Helicity}", journal = "JCAP", volume = "1008", pages = "010", doi = "10.1088/1475-7516/2010/08/010", year = "2010", eprint = "0903.4450", archivePrefix ="arXiv", primaryClass = "astro-ph.HE", SLACcitation = "%%CITATION = ARXIV:0903.4450;%%", } %% @Article{ Dvornikov:2015lea, author = {{Dvornikov}, M. and {Semikoz}, V.~B.}, title = "{Generation of the magnetic helicity in a neutron star driven by the electroweak electron-nucleon interaction}", journal = "JCAP", number = "05", volume = "1505", pages = "032", doi = "10.1088/1475-7516/2015/05/032", year = "2015", eprint = "1503.04162", archiveprefix ="arXiv", primaryclass = "astro-ph.HE", slaccitation = "%%CITATION = ARXIV:1503.04162;%%" } @Article{ Sigl:2015xva, author = {Sigl, G\"unter and Leite, Natacha}, title = "{Chiral Magnetic Effect in Protoneutron Stars and Magnetic Field Spectral Evolution}", journal = "JCAP", volume = "1601", year = "2016", number = "01", pages = "025", doi = "10.1088/1475-7516/2016/01/025", eprint = "1507.04983", archiveprefix = "arXiv", primaryclass = "astro-ph.HE", slaccitation = "%%CITATION = ARXIV:1507.04983;%%" } @Article{ Dvornikov:2016cmz, author = "Dvornikov, Maxim", title = "{Magnetic fields in turbulent quark matter and magnetar bursts}", year = "2016", eprint = "1612.06540", archiveprefix = "arXiv", primaryclass = "astro-ph.HE", slaccitation = "%%CITATION = ARXIV:1612.06540;%%" } @ARTICLE{Haensel:95, author = {{Haensel}, P.}, title = "{URCA Processes in Dense Matter and Neutron Star Cooling}", journal = {\ssr}, keywords = {dense matter, neutron stars}, year = 1995, month = nov, volume = 74, pages = {427-436}, doi = {10.1007/BF00751429}, adsurl = {http://adsabs.harvard.edu/abs/1995SSRv...74..427H}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} } @article{Urpin:2003wg, author = "Urpin, V. and Gil, J.", title = "{Convection in protoneutron stars and the structure of surface magnetic fields in pulsars}", journal = {\aap}, volume = "415", year = "2004", pages = "305-311", doi = "10.1051/0004-6361:20034447", eprint = "astro-ph/0311181", archivePrefix ="arXiv", primaryClass = "astro-ph", SLACcitation = "%%CITATION = ASTRO-PH/0311181;%%" } @ARTICLE{BPP69, author = {{Baym}, G. and {Pethick}, C. and {Pikes}, D.}, title = "{Electrical Conductivity of Neutron Star Matter}", journal = {\nat}, year = 1969, month = nov, volume = 224, pages = {674-675}, doi = {10.1038/224674a0}, adsurl = {http://adsabs.harvard.edu/abs/1969Natur.224..674B}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} } @ARTICLE{Zra14, author = {{Zrake}, J.}, title = "{Inverse Cascade of Nonhelical Magnetic Turbulence in a Relativistic Fluid}", journal = {\apjl}, archivePrefix = "arXiv", eprint = {1407.5626}, primaryClass = "astro-ph.HE", keywords = {gamma-ray burst: general, magnetic fields, magnetohydrodynamics: MHD, turbulence}, year = 2014, month = oct, volume = 794, eid = {L26}, pages = {L26}, doi = {10.1088/2041-8205/794/2/L26}, adsurl = {http://esoads.eso.org/abs/2014ApJ...794L..26Z}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} } @ARTICLE{BKT15, author = {{Brandenburg}, A. and {Kahniashvili}, T. and {Tevzadze}, A.~G. }, title = "{Nonhelical inverse transfer of a decaying turbulent magnetic field}", journal = {Phys. Rev. Lett.}, archivePrefix = "arXiv", eprint = {1404.2238}, keywords = {Turbulence, MHD waves, plasma waves turbulence}, year = 2015, month = feb, volume = 114, number = 7, eid = {075001}, pages = {075001}, doi = {10.1103/PhysRevLett.114.075001}, adsurl = {http://esoads.eso.org/abs/2015PhRvL.114g5001B}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} } @ARTICLE{BKMPTV17, author = {{Brandenburg}, A. and {Kahniashvili}, T. and {Mandal}, S. and {Pol}, A.~R. and {Tevzadze}, A.~G. and {Vachaspati}, T.}, title = "{Evolution of hydromagnetic turbulence from the electroweak phase transition}", journal = {\prd}, archivePrefix = "arXiv", eprint = {1711.03804}, year = 2017, month = dec, volume = 96, number = 12, eid = {123528}, pages = {123528}, doi = {10.1103/PhysRevD.96.123528}, adsurl = {http://esoads.eso.org/abs/2017PhRvD..96l3528B}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} } @ARTICLE{TD93, author = {{Thompson}, C. and {Duncan}, R.~C.}, title = "{Neutron star dynamos and the origins of pulsar magnetism}", journal = {\apj}, keywords = {Dynamo Theory, Neutron Stars, Pulsars, Stellar Convection, Stellar Magnetic Fields, Stellar Physics, Gamma Ray Bursts, Stellar Interiors, Supernovae}, year = 1993, month = may, volume = 408, pages = {194-217}, doi = {10.1086/172580}, adsurl = {http://adsabs.harvard.edu/abs/1993ApJ...408..194T}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} } @article{Kharzeev:07, author = {Kharzeev, Dmitri E. and McLerran, Larry D. and Warringa, Harmen J.}, journal = {Nucl. Phys.}, pages = {227}, title = {{The Effects of topological charge change in heavy ion collisions: 'Event by event P and CP violation'}}, volume = {A803}, year = {2008}, abstract = {Quantum chromodynamics (QCD) contains field configurations which can be characterized by a topological invariant, the winding number Q_w. Configurations with nonzero Q_w break the charge-parity CP symmetry of QCD. We consider a novel mechanism by which these configurations can separate charge in the presence of a background magnetic field - the "Chiral Magnetic Effect". We argue that sufficiently large magnetic fields are created in heavy ion collisions so that the Chiral Magnetic Effect causes preferential emission of charged particles along the direction of angular momentum. Since separation of charge is CP-odd, any observation of the Chiral Magnetic Effect could provide a clear demonstration of the topological nature of the QCD vacuum. We give an estimate of the effect and conclude that it might be observed experimentally.}, doi = {10.1016/j.nuclphysa.2008.02.298}, } @article{Hirono:2015rla, author = "Hirono, Yuji and Kharzeev, Dmitri and Yin, Yi", title = "{Self-similar inverse cascade of magnetic helicity driven by the chiral anomaly}", journal = "Phys. Rev. D", volume = "92", year = "2015", number = "12", pages = "125031", doi = "10.1103/PhysRevD.92.125031", eprint = "1509.07790", archivePrefix ="arXiv", primaryClass = "hep-th", abstract = { For systems with charged chiral fermions, the imbalance of chirality in the presence of magnetic field generates an electric current - this is the Chiral Magnetic Effect (CME). We study the dynamical real-time evolution of electromagnetic fields coupled by the anomaly to the chiral charge density and the CME current by solving the Maxwell-Chern-Simons equations. We find that the CME induces the inverse cascade of magnetic helicity towards the large distances, and that at late times this cascade becomes self-similar, with universal exponents. We also find that in terms of gauge field topology the inverse cascade represents the transition from linked electric and magnetic fields (Hopfions) to the knotted configuration of magnetic field (Chandrasekhar-Kendall states). The magnetic reconnections are accompanied by the pulses of the CME current directed along the magnetic field lines. We devise an experimental signature of these phenomena in heavy ion collisions, and speculate about implications for condensed matter systems. }, SLACcitation = "%%CITATION = ARXIV:1509.07790;%%" } @ARTICLE{Vilenkin:79, author = {Vilenkin, A.}, title = {{Macroscopic parity violating effects: neutrino fluxes from rotating black holes and in rotating thermal radiation}}, journal = {Phys. Rev. D}, year = {1979}, volume = {20}, pages = {1807-1812}, abstract = {Two macroscopic effects of parity nonconservation are considered. (i) Particle emission by rotating black holes is shown to be asymmetric. In particular, neutrinos are emitted preferentially in the direction opposite to the hole's angular momentum. (ii) It is shown that in a rotating thermal radiation there exist equilibrium neutrino and antineutrino currents parallel to the angular velocity vector.}, doi = {10.1103/PhysRevD.20.1807}, texkey = {Vilenkin:1979ui} } @ARTICLE{Wil80, author = {{Williamson}, J.~H.}, title = "{Low-storage Runge-Kutta schemes}", journal = {J. Comp. Phys.}, year = 1980, volume = 35, pages = {48} } % doi = {10.1016/0021-9991(80)90033-9} @ARTICLE{Jur11, author = {{Jur{\v c}i{\v s}inov{\'a}}, E. and {Jur{\v c}i{\v s}in}, M. and {Remeck{\'y}}, R.}, title = "{Turbulent magnetic Prandtl number in kinematic magnetohydrodynamic turbulence: Two-loop approximation}", journal = {\pre}, keywords = {Navier-Stokes equations, Field-theoretic formulations and renormalization, Turbulent diffusion, Magnetohydrodynamics and electrohydrodynamics}, year = 2011, month = oct, volume = 84, number = 4, eid = {046311}, pages = {046311}, doi = {10.1103/PhysRevE.84.046311}, adsurl = {http://adsabs.harvard.edu/abs/2011PhRvE..84d6311J}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} } @ARTICLE{YBR03, author = {{Yousef}, T.~A. and {Brandenburg}, A. and {R{\"u}diger}, G.}, title = "{Turbulent magnetic Prandtl number and magnetic diffusivity quenching from simulations}", journal = {\aap}, eprint = {astro-ph/0302425}, keywords = {magnetohydrodynamics (MHD), turbulence}, year = 2003, month = dec, volume = 411, pages = {321-327}, doi = {10.1051/0004-6361:20031371}, adsurl = {http://adsabs.harvard.edu/abs/2003A%26A...411..321Y}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }