Hostname: page-component-586b7cd67f-rdxmf Total loading time: 0 Render date: 2024-11-26T07:37:06.718Z Has data issue: false hasContentIssue false

“Ambipolar diffusion” and magnetic reconnection

Published online by Cambridge University Press:  08 June 2011

Yuriy T. Tsap
Affiliation:
Crimean Astrophysical Observatory, Nauchny, Crimea, 98409, Ukraine email: [email protected]
Alexander V. Stepanov
Affiliation:
Central (Pulkovo) Astronomical Observatory, St. Petersburg, 196140, Russia email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Based on the three-fluid approximation the influence of the neutral component of hydrogen plasma on Joule dissipation of electric currents are considered. As distinguished from Mestel & Spitzer (1956) and Parker (1963) it has been shown that the magnetic flux may be not conserved in the case of the “ambipolar diffusion” due to collisions between ions and neutrals. This is explained by the ion acceleration under the action of Ampere's force. Joule dissipation is determined by electron and ion collisions in a partially ionized plasma. Plasma evacuation from current sheets is the effective mechanism of its cooling. Thickness of a current sheet can achieve up to hundreds of kilometers in the solar chromosphere. The origin of the solar chromospheric jets observed with the Hinode satellite are discussed.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2011

References

Cowling, T. G. 1957, Magnetohydrodynamics, Interscience, New YorkGoogle Scholar
De Pontieu, B., McIntosh, S., Hansteen, V. H. et al. . 2007, PASJ, 59, 655CrossRefGoogle Scholar
Mestel, L., & Spitzer, L. Jr. 1956, MNRAS, 116, 503CrossRefGoogle Scholar
Nakano, T., Nishi, R., & Umebayashi, T. 2002, ApJ, 573, 199CrossRefGoogle Scholar
Ni, L., Yang, Zh., & Wang, H. 2007, ApSS, 312, 139Google Scholar
Parker, E. N. 1963, ApJS, 8, 177CrossRefGoogle Scholar
Piddington, J. H. 1954, MNRAS, 114, 551Google Scholar
Shibata, K., Nakamura, T., Matsumoto, T. et al. . 2007, Science, 318, 1591CrossRefGoogle Scholar
Shu, F. H., Adams, F. C., & Lizano, S., 1987, ARA&A, 25, 23Google Scholar
Spitzer, L. Jr. 1978, Physical Processes in the Interstellar Medium, J. Wiley & Sons, New YorkGoogle Scholar
Tsap, Y. T. 1994, Astron. Lett., 20, 127Google Scholar
Vishniac, E. T., & Lazarian, A. 1999, ApJ, 511, 193CrossRefGoogle Scholar
Zaitsev, V. V., & Stepanov, A. V. 1992, Solar Phys., 139, 343CrossRefGoogle Scholar
Zweibel, E. G. 1989, ApJ, 340, 550CrossRefGoogle Scholar
Zweibel, E. G., & Brandenburg, A. 1997, ApJ, 478, 563CrossRefGoogle Scholar