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    188宝金博页面版: temporal evolution of magnetic elements

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    内容提示： arXiv:0712.0234v1 [astro-ph] 3 Dec 2007**FULL TITLE**ASP Conference Series, Vol. **VOLUME**, **YEAR OF PUBLICATION****NAMES OF EDITORS**Temporal evolution of magnetic elementsR. Rezaei1, R. Schlichenmaier1, W. Schmidt1and C. Beck1,21-Kiepenheuer-Institut f¨ ur Sonnenphysik, 79104 Freiburg, Germany2-Instituto de Astrof? ?sica de Canarias (IAC), E 38205, La Laguna,SpainAbstract.the quiet Sun by investigating weak spectro-polarimetric signals. To this end,we observed a quiet region close to the disk cent...

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    arXiv:0712.0234v1 [astro-ph] 3 Dec 2007**FULL TITLE**ASP Conference Series, Vol. **VOLUME**, **YEAR OF PUBLICATION****NAMES OF EDITORS**Temporal evolution of magnetic elementsR. Rezaei1, R. Schlichenmaier1, W. Schmidt1and C. Beck1,21-Kiepenheuer-Institut f¨ ur Sonnenphysik, 79104 Freiburg, Germany2-Instituto de Astrof´ ?sica de Canarias (IAC), E 38205, La Laguna,SpainAbstract.the quiet Sun by investigating weak spectro-polarimetric signals. To this end,we observed a quiet region close to the disk center with the German VTT inTenerife, July 07, 2006. We recorded 38 scans of the same area. Each scanwas eight arcsec wide and observed within about 100 seconds. We used PO-LIS to simultaneously observe Stokes profiles of the neutral iron lines at 630.15and 630.25nm, the Stokes-I profile of the Ca iiH line at 396.8nm, and a con-tinuum speckle channel at 500nm. We witness two examples of magnetic fluxcancellation of small-scale opposite-polarity patches, followed by an enhancedchromospheric emission. In each case, the two opposite-polarity patches grad-ually became smaller and, within a few minutes, the smaller one completelydisappeared. The larger patch also diminished significantly. We provide evi-dence for a cancellation scenario in the photosphere which leaves minor tracesat the chromospheric level.We study the structure and evolution of the magnetic field of1.IntroductionObservations indicate that most of the magnetic flux passing through the photo-sphere is concentrated in magnetic elements, i.e., patches of high field strengththat are embedded in relatively field-free plasma (Solanki 1993). The field linesof the magnetic elements are nearly vertical to the surface because of buoyancyforces. In the hierarchy of the magnetic structures, the magnetic elements takethe position between dark and bright structures, i.e., between pores and networkbright points (Zwaan 1987, Stenflo 1994). While the magnetic elements are notvisible in continuum or line wing, they appear bright in the core of the chro-mospheric Ca iiH and K lines. The convective motion associated with the pho-tospheric granulation sweeps the magnetic flux toward the intergranular lanes.Due to the geometry of these lanes, the magnetic flux is arranged there either inchains of individual flux tubes or elongated sheets. This behavior is seen in high-resolution observations (Berger et al.2004; Rouppe van der Voort et al. 2005)as well as in numerical simulations (Steiner 2005, V¨ ogler et al.2005).Magnetic flux cancellations are common events in the solar atmosphere.There are examples in which it leads to a clear enhancement in the chromo-spheric intensity (Bellot Rubio & Beck 2005; Beck, Bellot Rubio & Nagata 2005).Magnetic reconnection at the photospheric level was also studied by Litvinenko(1999) and Takeuchi & Shibata (2001). Rezaei et al.(2007b) presented Stokes-Vprofiles of the Fe i630nm line pair, where the two lines show opposite polaritiesin a single spectrum (OP profile). They suggested that it may be understood as1

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