The magnetic structure of the extended solar corona varies with the changing photospheric field during the solar cycle. A simple potential model of the corona using solar surface observations from 1976 to the present shows how the large-scale coronal field evolves over more than a solar activity cycle. These predictions match well with large stable structures inferred from measurements of coronal electron density and the IMF, though dynamic changes are poorly modeled. The sun's polar field was about 25 stronger at solar minimum in 1986 than in 1976; the heliospheric current sheet was also flatter. In Cycle 21 the coronal and photospheric large-scale long-lived field patterns rotated every 26.9 days in the northern hemisphere; the southern field rotated every 28 days. Similar periods have been present in the IMF and in the occurrence of solar flares during the last several solar cycles.


    Zugriff

    Zugriff über TIB

    Verfügbarkeit in meiner Bibliothek prüfen


    Exportieren, teilen und zitieren



    Titel :

    Large-scale solar and heliospheric magnetic fields


    Beteiligte:

    Erschienen in:

    Erscheinungsdatum :

    1991-01-01



    Medientyp :

    Sonstige


    Format :

    Keine Angabe


    Sprache :

    Englisch


    Schlagwörter :


    Large-scale solar and heliospheric magnetic fields

    Todd Hoeksema, J. | Elsevier | 1991




    Solar and heliospheric space missions

    Kuznetsov, V.D | Online Contents | 2015


    Solar and heliospheric space missions

    Kuznetsov, V.D. | Elsevier | 2014