Spatial and temporal relations between magnetic elements and bright points in the photospheric network

Details Spatial and temporal relations between magnetic elements and bright points in the photospheric network Spatial and temporal relations between magnetic elements and bright points in the photospheric network

Jul 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000a%26a...359..373m&link_type=abstract

Astronomy and Astrophysics, v.359, p.373-380 (2000)

Astronomy and Astrophysics

Astrophysics

19

Sun: Granulation, Sun: Magnetic Fields, Sun: Photosphere

Scientific paper

28 min time series of high resolution magnetograms, continuum filtergrams and line core filtergrams have been obtained in the line FeI 6173, with the 50 cm refractor of the Pic du Midi Observatory, in a quiet area near the solar disk center. Their comparison shows that every bright point of the photospheric network coincides better than 0"5 with a magnetic element of small size (smaller than 1"). The maximum of magnetic field strength of a magnetic element does not necessarily occur at the same time as the maximum of brightness. Such spatial and temporal relations cannot be explained by static models of flux tubes, but they can be by a dynamic flux tube model, as computed by Steiner et al. (1996). The observations also show that a magnetic element present in the network becomes bright and forms a bright point when it is compressed by the surrounding granules as they converge. This is an indication that the dynamics of granulation plays a major role in the concentration of the magnetic field into thin flux tubes, near the surface of the Sun.

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