By Professor Dr. Peter Ulmschneider, Professor Dr. Eric R. Priest (auth.), Professor Dr. Peter Ulmschneider, Professor Dr. Eric R. Priest, Professor Dr. Robert Rosner (eds.)

One of the nice difficulties of astrophysics is the unanswered query concerning the foundation and mechanism of chromospheric and coronal heating. simply how those outer stellar envelopes are heated is of primary significance, for the reason that all stars have sizzling chromospheric and coronal shells the place the temperature rises to thousands of levels, reminiscent of the temperatures within the stars' cores. right here for the 1st time is a finished stock of the proposed chromospheric and coronal heating theories. The proposed heating approaches are significantly in comparison, and the observational proof for some of the mechanisms is reviewed. this can be crucial examining for all these operating in such fields as stellar job, radio and XUV emission, rotation, and mass loss, for whom an in depth and constant presentation of our wisdom of chromospheric and coronal heating mechanisms is urgently needed.

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Additional resources for Mechanisms of Chromospheric and Coronal Heating: Proceedings of the International Conference, Heidelberg, 5–8 June 1990

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H. Roberts: I would like to comment on the question of producing small periodicities in coronal loops. Some years ago, Roberts, Edwin, and Benz (1984, Ap. J. 279, 857) lnvestigated the modes of oscillation of a cylindrical tube (loop) and showed that both long and short periods could arise, connected with the existence of slow and fast MHD waves. In particular, fast waves are ducted (guided) in regions of low Alfven speed (high gas density) and this ducting gives rise to a wave packet behavior.

360 is deeaying with a more eompaet leading spot of N polarity. On Oetober 31 this spot is alreadyon the invisible part of the disco Qualitative drawing of the eorresponding magnetie areh strueture, the loeation of a quiescent prominence at this position, and the polar map of the emission corona suggest that on Oetober 31 the slit of the speetrograph was plaeed at a position of maximum Fe XIV line emission at an acute angle across the arch. 58 nmjmm were taken at 20 s constant time illtervals between individual pietures and with exposure time of 6 s.

1987, in Theoretical Problems in High Resolution Solar Physics II (G. S. ) NASA Conf. Publ. : 1991, in Mechanisms of Chromospheric and Coronal Heating (P. : 1976, Solar Phys. : 1978, Solar Phys. : 1987, Astron. Astrophys. : 1982, Solar Phys. : 1987, Astron. Astrophys. : 1990, in Cool Stars, Stellar Systems, and the Sun (G. ) Astron. Soc. Pacific Conf. : 1986, Ap. J. : 1989, Astron. Astrophys. : 1990, in The Dynamic Sun (Proc. of the 6th European Meeting on Solar Physics), Debrecen, in press Discussion Z.

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