Abstract
We examine chromospheric oscillations in both a coronal hole (CH) and a quiet Sun (QS) region, by employing Transition Region and Coronal Explorer (TRACE) and Big Bear Solar Observatory (BBSO) data on September 14 and 16, 2004. For the CH, the average oscillation periods of network magnetic field and non-magnetic field (NMF) regions are 257 and 222 s, respectively, and the average period of network field is longer than that of NMF region by 15.8%. In the QS, the average oscillation period is the 225 s for network field and 212 s for the NMF region. The average period of the network field is also longer than that of the NMF region by 6.1%. For the network region, we find that the average period in the CH is longer than that in the QS by 14.2%. This difference between CH and QS is possibly caused by different magnetic configurations i.e. the open magnetic field in the CH and the close field in the QS.
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Supported by the National Natural Science Foundation of China (Grant Nos. G10873020, 10603008, 40890161, 10703020, 40674081, and 10703007), the CAS Project (Grant No. KJCX2-YW-T04), and the National Basic Research Program of China (Grant No. G2006CB806303)
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Song, Q., Zhang, J. Chromospheric oscillations observed with BBSO and TRACE. Sci. China Ser. G-Phys. Mech. Astron. 52, 1718–1722 (2009). https://doi.org/10.1007/s11433-009-0217-8
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DOI: https://doi.org/10.1007/s11433-009-0217-8