EDP Sciences
Free Access
Volume 425, Number 1, October I 2004
Page(s) 309 - 319
Section The Sun
DOI https://doi.org/10.1051/0004-6361:20041004
Published online 10 September 2004

A&A 425, 309-319 (2004)
DOI: 10.1051/0004-6361:20041004

AFS dynamic evolution during the emergence of an active region

D. Spadaro1, S. Billotta1, L. Contarino1, P. Romano2 and F. Zuccarello2

1  INAF - Osservatorio Astrofisico di Catania, Via S. Sofia 78, 95125 Catania, Italy
    e-mail: dspadaro@ct.astro.it
2  Dipartimento di Fisica e Astronomia - Sezione Astrofisica, Università di Catania, Via S. Sofia 78, 95125 Catania, Italy

(Received 1 April 2004 / Accepted 25 May 2004 )

Using data acquired during an observational campaign carried out at the THEMIS telescope in IPM mode, coordinated with other ground- and space-based instruments (IOACT, TRACE, EIT/SOHO, MDI/SOHO), we have analyzed the first evolutionary phases of a recurrent active region (NOAA 10050), in order to study the morphology and dynamics of its magnetic structures during their emergence and early development. The main result obtained from this analysis concerns the dynamic evolution of the arch filament system (AFS) crossing the polarity inversion line: the line of sight velocities determined from Doppler measurements confirm that the loops forming the AFS show an upward motion at their tops and a downward motion at their extremities, but also indicate that the upward motion decreases while the active region develops. Moreover, it has been found that, within the limits of the temporal cadence and spatial resolution of the instruments used, the first evidence of the active region formation is initially observed in the transition region and lower corona, and later on (i.e. after about 6 h) in the inner layers (chromosphere and photosphere). Another interesting result concerns the analysis of the magnetograms, indicating that the initial increase in the magnetic flux seems to be synchronous with the appearance od the active region appearance in the transition region and lower corona, and that the rate of increase of the magnetic flux during the formation of the active region is not constant, but is steeper at the beginning (i.e. during the first 150 h) than in the following period. All these results may indicate the presence of some mechanism that decelerates the magnetic flux emergence as more and more flux tubes rise towards higher atmospheric layers. Finally, we would like to stress the observed asymmetries between the preceding and the following sides of NOAA 10050: the p-side is more extented than the f-side, the p-side moves forward from the initial outbreak position much faster than the f-side recedes; the AFS f-side exhibits higher downflows than the p-side.

Key words: Sun: activity -- sunspots -- Sun: magnetic fields -- Sun: filaments

© ESO 2004

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