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Поляризационный эффект в плазме ранней Вселенной и Черн-Саймонс аномалия в гипермагнитном поле

Поляризационный эффект в плазме ранней Вселенной и Черн-Саймонс аномалия в гипермагнитном поле. В.Б. Семикоз (ИЗМИРАН) [ по работам совместно с Хосе Валле и Д.Д. Соколовым ]. Magnetic field evolution after EWPT. Summary 1. • The right electron asymmetry ( ξ eR ) rises soon

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Поляризационный эффект в плазме ранней Вселенной и Черн-Саймонс аномалия в гипермагнитном поле

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  1. Поляризационный эффект в плазме ранней Вселенной и Черн-Саймонс аномалия в гипермагнитном поле В.Б. Семикоз (ИЗМИРАН) [по работам совместно с Хосе Валле и Д.Д. Соколовым]

  2. Magnetic field evolution after EWPT

  3. Summary 1 • The right electron asymmetry (ξeR) rises soon down to TEW from a negligible initial value at T» TEW up to ξeR~10 – 4 at T≤TEW . This happens due to the Abelian anomaly. • This provides both the α2 dynamo for BY and baryon asymmetry growth since fermion number sits in hypercharge fields. • The initial Maxwellian field B=BYcos θW can be a seed field field for galactic magnetic fields.

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