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Признаки стационарного магнитного пересоединения в солнечном ветре

Признаки стационарного магнитного пересоединения в солнечном ветре. Ю. Л. Сасунов, В. С. Семенов С С. Петербургский университет. Thanks to N. Erkaev, M. Heyn, H. Biernat and I. Kubyshkin. Sites for reconnection in magnetosphere. “ Standard Model ” of Flares.

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Признаки стационарного магнитного пересоединения в солнечном ветре

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  1. Признаки стационарного магнитного пересоединения в солнечном ветре Ю. Л. Сасунов, В. С. Семенов СС. Петербургский университет Thanks to N. Erkaev, M. Heyn, H. Biernat and I. Kubyshkin

  2. Sites for reconnection in magnetosphere

  3. “Standard Model” of Flares

  4. Reconnection at the Leading Edge of an ICME After J. Gosling

  5. Results from Study of Initial 49 Exhausts Identified in the ACE 64-s Data (~1.3 events/month) Most of the exhausts were associated with relatively large field shear angles. Typical exhaust crossing times were 10 minutes - exhaust widths ~ 2.4 x 105 km. After J. Gosling

  6. Reconnection event 31.08 – 1.09.2001 This is the largest exhaust yet identified in the solar wind and demonstrates prolonged reconnection at an extended and continuous X-line. Gosling et al., GRL 2007

  7. Normal coordinates LMN

  8. Riemann problem for reconnection Heyn, Biernat, Rijnbeek, and Semenov, The Structure of Reconnection Layers, J. Plasma Phys., 1988.

  9. Decay of discontinuity

  10. Structure of reconnection layer 2-D projection 3-D view

  11. Alfven discontinuity • Shock wave

  12. Wind ACE Geotail

  13. Reconnection event on 31 Aug – 1 Sep 2001 (WIND)

  14. Reconnection event on 31 Aug – 1 Sep 2001 (GEOTAIL)

  15. Reconnection event on 31 Aug – 1 Sep 2001 (ACE)

  16. Interaction of solar wind with ICME With reconnection after Erkaev N. V.

  17. Interaction of solar wind with ICME No reconnection after Erkaev N. V. Pudovkin and Bogdanova, Geomag. Aeronomy, 2002

  18. Reconnection in the solar wind: Occurs at thin current sheets that separate distinctly different plasma states (tangential discontinuities). Commonly is quasi-stationary and typically occurs at extended X-lines (~390 Re Phan et al. 2006, ~600 Re Gosling et al. 2007) Produces Petschek-type exhausts of roughly Alfvenic jetting plasma bounded by rotational discontinuity-slow shock structure that bifurcate the original thin current sheet. Slows down ICMEs with low magnetic shear and accelerates ICMEs with high shear.

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