1 / 15

Sakai, J. I., Nishi, K., and Sokolov, I. V. ApJ, 2002, 576, 1018

Heating of coronal loop footpoints by slingshot magnetic reconnection during two loop interactions driven by a moving solitary magnetic kink. Sakai, J. I., Nishi, K., and Sokolov, I. V. ApJ, 2002, 576, 1018. Background-theories. Possible coronal heating mechanism:

argyle
Télécharger la présentation

Sakai, J. I., Nishi, K., and Sokolov, I. V. ApJ, 2002, 576, 1018

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. Heating of coronal loop footpoints by slingshot magnetic reconnection during two loop interactions driven by a moving solitary magnetic kink Sakai, J. I., Nishi, K., and Sokolov, I. V. ApJ, 2002, 576, 1018

  2. Background-theories • Possible coronal heating mechanism: • MHD waves propagate and dissipate (e.g., Steiner et al. 1994, Ofman, et al. 1998, Sakurai, 1985) • Current sheets heating at the topologic interface (e.g., Parker 1972, Glencross 1975, Rosner et al. 1978, Sturrock and Uchida 1981, Demoulin and Priest 1997)---- but it is hard to detect the existence of current in the corona at present

  3. Background-observations • TRACE EUV observations (Lenz et al. 1999;Aschwanden et al. 2000, 2001)  near-isothermal loop T structure, multithreads, heated near the footpoints for some EUV loops • TRACE EUV observations (Schrijver 1999, Qiu et al. 1999) •  existence of up- and downflows in active region loops

  4. Sakai’s previous main results • Collision of magnetic flux tubes  shock formation and upflows (2000a) • Collision between the shock waves and the loops  surface Alfven waves (2000b) • Nonlinear MHD wave propagation  upward torsional and compressional waves (2000c, 2001a) • Surface Alfven waves and upward plasma  magnetic reconnection  Chromospheric loop heating model (2001b)

  5. The present work • To investigate reconnection between a vertical loop and a low-lying loop driven by the ‘moving solitary magnetic kink’ (MoSMak)  Coronal loop heating ?

  6. Formation of a MoSMaK • Head-on collision process of two dense plasma blobs in a twisted magnetic flux tube (the plasma blobs can be driven by the flux tube collisions near the photosphere) Iso-surface of |B|=0.32 A=2a/VA, a=20

  7. Velocity structure of the MoSMaK Vx-Vy Bx-By (1) (2) (3) Iso-surface of |v|=0.2

  8. Time evolution of the head-on collision process of two MoSMaKs Iso-surface of |B|=0.19 Horizontal loop Strong expanding toroidal flux

  9. Time evolution of the iso-surface of |B|=0.19 Vertical loop Sling-shot reconnection appears

  10. Time evolution of the iso-surface of |B|=0.31 with different view

  11. Time evolution of By-Bz (x=100) Time evolution of Bx-Bz (y=100)

  12. Time evolution of the iso-surface of |V|=0.15 Time evolution of Vy-Vz (x=100)

  13. Velocity distribution on Z=200 at t=28

  14. Vertical loop heating

  15. conclusion • A new local heating model of loop footpoints in the chromosphere is proposed • Non-uniform heating by slingshot reconnection, driven by the MoSMaKs • The loop interaction results in the formation of both helical up- and downflows

More Related