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Astrophysical and Laboratory Plasmas: A Festschrift for by Allan J. Willis, Thomas W. Hartquist (auth.), A. J. Willis,

By Allan J. Willis, Thomas W. Hartquist (auth.), A. J. Willis, T. W. Hartquist (eds.)

All through his profession Sir Robert Wilson has validated that advances in a large choice of fields in astrophysics and laboratory physics are plausible in the course of the program of basic plasma spectroscopy. His paintings has integrated: optical reviews that probed the character of interstellar dirt and primary printed the life of O big name winds; vacuum ultraviolet and X-ray analysis of fusion plasmas; rocket ultraviolet and X-ray observations of the sunlight; and the belief, improvement and use of the foreign Ultraviolet Explorer (IUE) satellite tv for pc which has contributed enormously to stellar, interstellar and extragalactic astrophysics. This quantity includes reports honouring Sir Robert and reflecting his pursuits.

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Figure 7 shows how the corona has evolved during four years of observations by the SXT. The overall soft x-ray luminosity has decreased by a factor of twenty in that time and the large-scale structure, representing the evolved magnetic field of large active regions, has been replaced by the weaker, less organized field structure of the numerous x-ray bright points. 5. Future Observations With the launch of the Solar and Heliospheric Observatory (SoHO) by ESA and NASA at the end of 1995, a major new observational capability is added to the solar arsenal.

Magnetic flux is seen to emerge from the solar interior, rising and breaking through the surface in the form of bipolar regions. Here 'bipolar' indicates that the magnetic field is re-entrant to the solar surface - field of one polarity emerges and field of the opposite polarity re-enters, usually at a nearby location. The overall appearance is roughly that of the field from a magnetic dipole lying horizontally just below the surface. Corresponding to this magnetic structure, the hot coronal plasma is seen to form loop-shaped structures which appear to trace the magnetic topology.

Thus the spine and the fan form the skeleton of the field lines near the null. 2) and E+v x B = 0. 4) where c and k are constants describing a field line. 1 follow. This approach has been applied to a single null, a pair of nulls and fields without nulls, as follows. CORONAL HEATING BY MAGNETIC RECONNECTION 55 z X Fig. 5. The structure of a 3D null point First of all, let us consider a 3D null point and ask what is the nature of reconnection near such a point? How do magnetic flux surfaces reconnect?

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