Chromospheric oscillations observed with BBSO and TRACE

  • Qiao Song
  • Jun Zhang


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.


chromosphere oscillations UV radiation magnetic fields quiet Sun coronal hole 


  1. 1.
    Narain U, Ulmschneider P. Chromospheric and coronal heating mechanisms II. Space Sci Rev, 1996, 75: 453–509CrossRefADSGoogle Scholar
  2. 2.
    Wikstøl \( \mathbb{O} \), Hansteen V H, Carlsson M, et al. Chromospheric and transition region internetwork oscillations: A signature of upward-propagating waves. Astrophys J, 2000, 531: 1150–1160CrossRefADSGoogle Scholar
  3. 3.
    Krijger J M, Rutten R J, Lites B W, et al. Dynamics of the solar chromosphere. III. Ultraviolet brightness oscillations from TRACE. Astron Astrophys, 2001, 379: 1052–1082CrossRefADSGoogle Scholar
  4. 4.
    Zhang J, Lin G H, Wang J X, et al. Lifetime of intranetwork magnetic elements. Sol Phys, 1998, 178: 245–250CrossRefADSGoogle Scholar
  5. 5.
    Zhang J, Lin G H, Wang J X, et al. The evolution of intranetwork magnetic elements. Astron Astrophys, 1998, 338: 322–328ADSGoogle Scholar
  6. 6.
    Zhang J, Wang J X, Wang H M, et al. The motion patterns of intranetwork magnetic elements. Astron Astrophys, 1998, 355: 341–350ADSGoogle Scholar
  7. 7.
    McAteer R T J, Gallagher P T, Bloomfield D S, et al. Ultraviolet oscillations in the chromosphere of the quiet Sun. Astrophys J, 2004, 602: 436–445CrossRefADSGoogle Scholar
  8. 8.
    McIntosh S W, Fleck B, Judge P G. Investigating the role of plasma topography on chromospheric oscillations observed by TRACE. Astron Astrophys, 2003, 405: 769–777CrossRefADSGoogle Scholar
  9. 9.
    Vecchio A, Cauzzi G, Reardon K P, et al. Solar atmospheric oscillations and the chromospheric magnetic topology. Astron Astrophys, 2007, 461: L1–L4CrossRefADSGoogle Scholar
  10. 10.
    Handy B N, Acton LW, Kankelborg C C, et al. The transition region and coronal explorer. Sol Phys, 1999, 187: 229–260CrossRefADSGoogle Scholar
  11. 11.
    Zhang J, Ma J, Wang H M. Comparison of magnetic flux distribution between a coronal hole and a quiet Sun region. Astrophys J, 2006, 649: 464–469CrossRefADSGoogle Scholar
  12. 12.
    Ireland J, Walsh R W, Harrison R A, et al. A wavelet analysis of active region oscillations. Astron Astrophys, 1999, 347: 335–365ADSGoogle Scholar

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© Science in China Press and Springer Berlin Heidelberg 2009

Authors and Affiliations

  1. 1.Key Laboratory of Solar ActivityNational Astronomical Observatories, Chinese Academy of SciencesBeijingChina

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