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Astron. Astrophys. 363, 279-288 (2000)

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5. Network bright points (high brightness)

These structures have two components: the first one is the quiet sun network formed by the complicated statistical processes of frequent collisions and coalescence and rapid replacement of flux from the flux bank provided by the ephemeral active regions described by Martin (1990) and modelled by Schrijver et al. (1997), and the second one consists of the familiar coarse mottles (De Jager, 1959) which are the fragmented remnants from decaying or decayed active regions, patterned and added to the network boundaries by the flows on the solar surface. It is vital to know how far the quiet sun network and the coarse mottles differ in terms of the long-period oscillations exhibited by the "network bright points" (Kalkofen, 1997) or any other observable properties. Also, it might be important to know whether the quiet sun network elements originating from the ephemeral active regions and those from the merger of intranetwork fields (which are also typical features of the quiet sun) have identical or different properties. It would be worthwhile to know how do these properties manifest themselves and how far the brightness - magnetic field relationship for the quiet sun network (cf. Skumanich et al., 1975; Stenflo & Harvey, 1985; Nindos & Zirin, 1998) might apply to these different quiet sun network structures.

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© European Southern Observatory (ESO) 2000

Online publication: December 5, 2000
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