1 / 17

Spatio-Temporal Dynamics of Magnetic Fields and Flaring Productivity of Active Regions

Spatio-Temporal Dynamics of Magnetic Fields and Flaring Productivity of Active Regions. Valentina I. Abramenko Big Bear Solar Observatory of NJIT Email: avi@bbso.njit.edu http://www.bbso.njit.edu/~avi/. Introduction.

forbes
Download Presentation

Spatio-Temporal Dynamics of Magnetic Fields and Flaring Productivity of Active Regions

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Spatio-Temporal Dynamics ofMagnetic Fields and Flaring Productivity of Active Regions Valentina I. Abramenko Big Bear Solar Observatory of NJIT Email: avi@bbso.njit.edu http://www.bbso.njit.edu/~avi/

  2. Introduction The 2005 Joint Assembly / AGU,SEG, NABS and SPD/AAS, May 23-27, 2005, New Orleans, LA, USA

  3. Introduction Essential properties of the photospheric plasma: Magnetized plasma in a turbulent state (Parker 1979), very intermittent (or, in other words, multifractal) medium (Lawrence et al. 1993, Abramenko et al. 2002), where the magnetic helicity may have an inverse cascade (Biskamp 1993)

  4. Introduction Situation in the photosphere – flaring in the corona: Magnetic helicity transport in the photosphere (Rust & LaBonte 2003; Georgoulis – present meeting; Chae2001; Romano 2005 ). Statistical properties of electric currents, current helecity, magnetic flux, etc., derived from vector-magnetograms (Leka & Barnes 2004). Fractal dimensions of the photospheric magnetic fields (Tarbell et al. 1990; Balke et al. 1993; Meunier 1999; McAteer, Gallagher & Ireland 2005).

  5. Introduction Situation in the photosphere – flaring in the corona: we propose to analyze 1. Distribution functions of the magnetic flux in elements of the magnetic field in active regions (Abramenko & Longcope, ApJ, 2005) 2. Multifractality (intermittency) of the photospheric magnetic fields – poster SP41B-04 (Abramenko, Yurchyshyn, Wang, Goode, ApJ 577, 2002). 3. Turbulence state of the photospheric magnetic field as derived from magnetic power spectrum – present talk.

  6. Observational Data:SoHO/MDI high resolution magnetograms http://www.bbso.njit.edu/~avi/PowerSp.pdf

  7. For example, during 13 days an active region launched flares: X5.2 , M1.2 , C6.0 A=(520 + 12 + 6.0) / 13 = 41.4 -6 -2 (in units 10 W m ) Soft X-ray Flare Index http://www.bbso.njit.edu/~avi/PowerSp.pdf

  8. Magnetic Power Spectrum Flaring active region 9077 (A=120) Flare-quiet active region 0061 (A=2.6) http://www.bbso.njit.edu/~avi/PowerSp.pdf

  9. Magnetic Power Spectrum:time-variations of the power index Flare-quiet active region 0061: Flaring active region 9077: http://www.bbso.njit.edu/~avi/PowerSp.pdf

  10. Magnetic Power Spectrum:emerging active region http://www.bbso.njit.edu/~avi/PowerSp.pdf

  11. Soft X-ray Flare Indexversus Magnetic power index http://www.bbso.njit.edu/~avi/PowerSp.pdf

  12. http://www.bbso.njit.edu/~avi/PowerSp.pdf

  13. Magnetic Power Spectrum:calculations k y k x http://www.bbso.njit.edu/~avi/PowerSp.pdf

  14. Table 2: Emerging Active Regions http://www.bbso.njit.edu/~avi/PowerSp.pdf

  15. Table 1: Active Regions http://www.bbso.njit.edu/~avi/PowerSp.pdf

  16. Emerging of a Flare-quiet Active Region NOAA 9851 http://www.bbso.njit.edu/~avi/PowerSp.pdf

  17. Emergence of a Flaring Active Region NOAA 0365 http://www.bbso.njit.edu/~avi/PowerSp.pdf

More Related