Evolution and Signatures of Helical Magnetic Fields
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1 Evolution and Signatures of Helical Magnetic Fields Tina Kahniashvili McWilliams Center for Cosmology Carnegie Mellon University & Abastumani Astrophysical Observatory Ilia State University NORDITA June
2 Based On Kahniashvili, Maravin, Lavrelashvili, Kosowsky PRD 2014 Kahniashvili, Tevzadze, Brandenburg, Neronov, PRD 2013 Tevzadze, Kisslinger, Brandenburg, Kahniashvili, ApJ 2013 Ongoing Collaboration (papers in preparation) Axel Brandenburg, Ruth Durrer, Victoria Merten, Alexander Tevzadze, Tanmay Vachaspati, Winston Yin
3 Earth MF Cosmic Magnetic Fields Interstellar MF Galaxy MF Sun MF
4 How do we observe cosmic magnetic fields? Electromagnetic waves & Effects induced by magnetic fields
5 Magnetic Helicity Solar activity: Sunspots Solar flares Coronal mass ejection Solar wind Magnetic helicity reflects mirror symmetry (parity) breaking DIFFICULT TO DETECT cosmic rays: Kahniashvili & Vachaspati 2006 gamma-rays: Tashiro and Vachaspati 2011
6 Gamma Rays vs Magnetic Helicity Tashiro and Vachaspati 2015 Tashiro, Chen, Francesc, Vachaspati 2014 Chen, Chowdhury, Francesc, Tashiro, Vachaspati 2014
7 Primordial Magnetic Field Hypothesis F. Hoyle in Proc. La structure et l evolution de l Universe (1958) Inflation Phase transitions Supersymmetry String Cosmology Topological defects Springel Millenium simulations
8 Inflation Magnetogenesis (Turner & Widrow 1988, Ratra 1992) The correlation length larger than horizon Scale invariant spectrum Well agree with the lower bounds Diffuculties Backreaction Symmetries violation Phase Transitions (Harrisonl 1970, Vachaspati 1991) Bubble collisions first order phase transitions QCDPT EWPT Causal fields Limitation of the correlation length Smoothed and effective fields approaches
9 Cosmological vs. Astrophysical Magnetogenesis MHD Simulations by Donnert et al Ejection Primordial Z=4 Z=4 Z=0 Z=0
10 Cosmological Magnetic Fields (Obvious Limits) BBN limits: 10% of additional relativistic component microgauss (comoving value) Grasso and Rubistein 2000 Yamazaki and Kusakabe 2012 Kawasaki and Kusakabe 2012 Faraday Rotation Measure At z~2-3 microgauss Bernet et al Kronberg et al. 2008
11 Magnetized CMB Perturbations Faraday rotation does not depend on magnetic helicity Density perturbations - scalar mode Fast and slow magnetosound waves Adams et al Jedamzik, Katalinic, Olinto, 1996 Vorticity perturbations - vector mode Alfven waves Subramanian and Baroow, 1998 Durrer, Kahniashvili, and Yates, 1998 Gravitational waves - tensor Mode Deryagin et al Durrer, Ferreira, Kahniashvili 2000
12 Modeling Helical Magnetic Field Kahniashvili, Kosowsky, Lavrelashvili, Maravin, 2014
13 Magnetic Helicity Effects on CMB Parity-even fluctuations Temperature - Temperature Temperature - E polarization E-polarization E-polarization B-polarization B-polarization Parity-odd fluctuations Temperature B-polarization E-polarization B-polarization Pogosian, Vachaspati, and Winitski 2000, Caprini, Durrer, and Kahniashvili, 2003, Kahniashvili and Ratra 2005, Kunze 2012, Kahniashvili, et al. 2014, Balardini, Finelli, and Paoletti, 2014
14 Magnetic Helicity vs. WMAP 9 years data Kahniashvili, Kosowsky, Lavrelashvili, Maravin, 2014
15 Magnetic Helicity Effects
16 Magnetic Helicity Limits Kahniashvili, Kosowsky, Lavrelashvili, Maravin, 2014
17 Phenomenology If the magnetic field has been generated through a causal process in the early universe it s correlation length could not exceed the Hubble horizon at the moment of the generation
18 MHD Modeling Coupling of the magnetic field with primordial plasma Injection of the magnetic energy at a given scale (phase transition bubble) Brandenburg, Kahniashvili, Tevzadze 2014
19 Modeling Magnetic Field smoothed vs. effective magnetic field one-scale (delta function) magnetic field Kahniashvili, Tevzadze, Brandenburg, Neronov 2013
20 Phase Transitions Generated Magnetic Field Phenomenology Non-helical field Helical field Helicity conservation law
21 Kahniashvili, Tevzadze, Brandenburg, Neronov 2013
22 Kahniashvili, Tevzadze, Brandenburg, Neronov 2013
23 Magnetic field from QCD Phase Transitions Tevzadze, Kisslinger, Brandenburg, Kahniashvili 2012 Our analysis show that in the most optimistic scenario the magnetic correlation length in the comoving frame can reach 10 kpc with the amplitude of the effective magnetic field being ng. We demonstrate that the considered model of magneto-genesis can provide the seed magnetic field for galaxies and clusters.
24 Magnetic Helicity Growth Tevzadze, Kisslinger, Brandenburg, Kahniashvili 2012 The correlation length should satisfy: Fractional magnetic helicity grows until it reaches its maximal value
25 Helical Magnetic Fields Decay Brandenburg, Kahniashvili, Tevzadze 2015 Causal fields correlation length limitation n B =2 or n B =0 Inverse Cascade
26 Helical Magnetic Fields Decay Vachaspati 2001
27 Helical Magnetic Field Brandenburg, Kahniashvili, Tevzadze 2015
28 Inflationary Magnetic Helicity Magnetic field correlation length might be as large as the Hubble horizon today or even larger (infinity) Can we see the imprints of an a-causal field? Kahniashvili, Brandenburg, Durrer, Tevzadze, Yin, 2015
29 Inflation Generated Helical Magnetic Field Kahniashvili, Brandenburgh, Durrer, Tevzadze, Yin 2015 The absence of inverse cascade for Inflation generated magnetic fields
30 Helical Magnetic Fields Scaling Laws Brandenburg, Kahniashvili, Tevzadze 2015
31 Conclusion The lower bound of the extragalactic magnetic field favors a primordial magnetogenesis approach (in particular, helical magnetic fields) The primordial magnetic field might be a plausible explanation for the galaxy magnetic field Cosmological magnetic field order of 0.1 nanogauss can be detectable by the nearest future CMB polarization and LSS measurements On the other hand, if the field is significantly smaller it would satisfy the LOWER limit bound but would not been observable through cosmological observations
32
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