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Intermittency of the magnetic fields on the Sun: Indroduction

Intermittency of the magnetic fields on the Sun: Indroduction. V.I. Abramenko Big Bear Solar Observatory, NJIT Crimean Astrophysical Observatory, Ukraine Email: avi@bbso.njit.edu. November 2, 2007 BBSO. y. [ ]. (y-m) 2. 1. P(y)= —. — exp. ——. 2  2. (). x. P(y). y.

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Intermittency of the magnetic fields on the Sun: Indroduction

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  1. Intermittency of the magnetic fields on the Sun: Indroduction V.I. Abramenko Big Bear Solar Observatory, NJIT Crimean Astrophysical Observatory, Ukraine Email: avi@bbso.njit.edu November 2, 2007 BBSO

  2. y [ ] (y-m)2 1 P(y)= — — exp —— 22 () x P(y) y y P(y) x y Introduction: what is the intermittency? m <y1> yi  N 2 <y2> (yi - m )2 / N m <y1> = yP(y)dy <yk > =(y-m)kP(y)dy

  3. [ ] (y-m)2 1 P(y)= — — exp —— 22 () P(y) y P(y) y Introduction: what is the intermittency? y m <y1> yi  N 2 <y2> (yi - m )2 / N x m= <y1> = yP(y)dy <yk > =(y-m)kP(y)dy x

  4. [ ] (y-m)2 1 P(y)= — — exp —— 22 () P(y) y P(y) y Introduction: what is the intermittency? y m <y1> yi  N 2 <y2> (yi - m )2 / N x m= <y1> = yP(y)dy <yk > =(y-m)kP(y)dy x

  5. Introduction: what is the intermittency?

  6. Photosphere Turbulent plasma motions Magnetic field Sunspots We are here

  7. Continuous turbulent motions of magnetic elements in the photosphere Photospheric plasma is in a state of turbulence. The magnetic field, as a subject of turbulence, is highly intermittent. The measure of intermittency is the quantitative characteristic of the complexity of the magnetic field.

  8. Magnetic field, Gauss Intermittent process Increase of the number of discontinuities of the magnetic field Appearance or/and reinforcement of strong small-scale magnetic flux tubes What is the physical meaning of increase of intermittency of the magnetic field?

  9. Consequences of magnetic field discontinuities: Magnetic reconnection process High magnetic energy Lower magnetic energy The X – point, or a magnetic discontinuity magnetic energy dissipation

  10. The avalanche model of a solar flare (Parker,1983,1988) A flare is the collective energy released by an avalancheof reconnection events on the magnetic field discontinuities Corona Magnetic field lines discontinuities Photosphere Sunspots

  11. Conclusion Intermittencyof the magnetic field reflects the complexity of the field. Namely, the strength of magnetic discontinuities, the presence of rare super-strong flux tubes of various sizes, the burst-like behavior of the field. That is why intermittency can bear information of the flaring productivity of solar active regions, and therefore, deserves our attention. Methods to analyze intermittency will be discussed in details in our future lectures.

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