EDP Sciences
Free access
Volume 441, Number 3, October III 2005
Page(s) 1191 - 1194
Section The Sun
DOI http://dx.doi.org/10.1051/0004-6361:20052919

A&A 441, 1191-1194 (2005)
DOI: 10.1051/0004-6361:20052919

Coronal oscillation above a supergranular cell of the quiet Sun chromospheric network?

C. Gontikakis1, H. Peter2 and H. C. Dara1

1  Academy of Athens, Research Center of Astronomy and Applied Mathematics, Soranou Efessiou 4, 115 27 Athens, Greece
    e-mail: [cgontik;edara]@cc.uoa.gr
2  Kiepenheuer-Institut f $\rm\ddot u$r Sonnenphysik, Sch $\rm\ddot o$neckstr. 6, 79104 Freiburg, Germany
    e-mail: peter@kis.uni-freiburg.de

(Received 22 February 2005 / Accepted 24 June 2005)

We have detected an oscillation in the low corona, using a raster of the SUMER EUV spectrograph in the Ne VIII, 770 Å line formed at about 700 000 K. The oscillation was found in the Ne VIII Doppler map above the interior of a supergranular cell of the chromospheric network in the quiet Sun, while it is absent in line radiance. The photospheric magnetic field, extrapolated to coronal levels, was used to relate this phenomenon to the magnetic structure. This oscillation phenomenon, reported here for the first time, seems to occur only above the darkest cells of the chromospheric network. We interpret our findings as a collective non-compressible oscillation of the corona above the whole cell interior. This oscillation may originate at the chromosphere and the driving wave may undergo a mode conversion at the top chromosphere, where the magnetic pressure equals the gas pressure. Our interpretation cannot be definitive and should be verified with more data.

Key words: Sun: UV radiation -- Sun: corona

© ESO 2005