• Published : 2008.04.30


Spectral line profiles of filaments/prominences to be observed by the Fast Imaging Solar Spectrograph (FISS) are studied. The main spectral lines of interests are $H{\alpha}$, Ca II 8542, and Ca II K. FISS has a high spectral resolving power of $2{\times}10^5$, and supports simultaneous dual-band recording. This instrument will be installed at the 1.6m New Solar Telescope (NST) of Big Bear Solar Observatory, which has a high spatial resolution of 0.065" at 500nm. Adopting the cloud model of radiative transfer and using the model parameters inferred from pre-existing observations, we have simulated a set of spectral profiles of the lines that are emitted by a filament on the disk or a prominence at the limb. Taking into account the parameters of the instrument, we have estimated the photon count to be recorded by the CCD cameras, the signal-to-noise ratios, and so on. We have also found that FISS is suitable for the study of multi-velocity threads in filaments if the spectral profiles of Ca II lines are recorded together with $H{\alpha}$ lines.


  1. Beckers, J. M., 1964, Ph.D. Thesis, University of Utrecht (AFCRL-Environmental Research Paper, No.49)
  2. Denker, C., Goode, P. R., Ren, D., Saadeghvaziri, M. A., Verdoni, A. P., Wang, H., Yang, G., Abramenko, V., Cao, W., Coulter, R., Fear, R., Nenow, J., Shoumko, S., Spirock, T. J., Varsik, J. R., Chae, J., Kuhn, J. R., Moon, Y., Park, Y. D., & Tritschler, A., 2006, Progress on the 1.6-meter New Solar Telescope at Big Bear Solar Observatory, SPIE, 6267, 10
  3. Engvold, O., Malville, J. M., & Livingston, W., 1978, The Fine Structure of Prominences, SoPh, 60, 57
  4. Choi, S., Kim, Y.-H., Moon, Y.-J., Cho, K.-S., Park, Y.-D., Jang, B.-H., Kim, S.-J., & Kim, K.-S., 2005, Component-Based Development of Observational Software for KASI Solar Imaging Spectrograph, JKAS, 38, 463
  5. Mein, P. & Mein, N., 1991, Dynamical Fine Structure of a Quiescent Prominence, SoPh, 136, 317
  6. Molowny-Horas, R., Heinzel. P., Mein, P., & Mein, N., 1999, A non-LTE Inversion Procedure for Chromospheric Cloud-like Features, A&A, 345, 618
  7. Schmieder, B., 1992, Structural Elements of Filaments, SoPh, 141, 275
  8. Kubota, J., 1980, The Optical Thickness of Quiescent Prominences in the Ca II K Lines and the Centeral Reversal in the Spectral Lines, PASJ, 32, 359
  9. Lin, Y., Engvold, O., van der Voort, L. R., Wiik, J. E., & Berger, T. E., 2005, Thin Threads of Solar filaments, SoPh, 226, 239
  10. Goode, P. R., Denker, C. J., Didkovsky, L. I., Kuhn, J. R., & Wang, H., 2003, 1.6 M Solar Telescope in Big Bear - The NST, JKAS, 36,S1, S125
  11. Gouttebroze, P., Vial, J.-C., & Heinzel, P., 1997, Formation of Ca II Lines in Solar Prominences, SoPh, 172, 125
  12. Heinzel, P., Gouttebroze, P., & Vial, J.-C., 1994, Theoretical Correlations between Prominence Plasma Parameters and the Emitted Radiation, A&A, 292, 656
  13. Tziotziou, K., Heinzel, P., Mein, P., & Mein, N., 2001, Non-LTE Inversion of Chromospheric Ca II Cloudlike Features, A&A, 366, 686
  14. Tziotziou, K., 2007, Chromospheric Cloud-Model Inversion Techniques, ASPC, 368, 217
  15. Stellmacher, G. & Wiehr, E., 2000, Two-dimensional Photometric Analysis of Emission Lines in Quiescent Prominences, SoPh, 196, 357
  16. Tandberg-Hanssen, E., 1995, The Nature of Solar Prominences, Kluwer Academic publishers
  17. Zhang, Q. Z. & Fang, C., 1987, Semi-empirical Models of a Quiescent Prominence, A&A, 175, 277
  18. Wang, H., Chae, J., Gurman, J. B., & Kucera, T. A., 1998, Comparison of Prominences in $H\alpha$ and He II $304\AA$, SoPh, 183, 91
  19. Wallace, L., Hinkle, K., & Livingston, W. C., 1993, An Atlas of the Photospheric Spectrum from 8900 to 13600 cm(-1) (7350 to 11230 [angstroms]), National Solar Observatory
  20. Wallace, L., Hinkle, K., & Livingston, W., 1998, An Atlas of the Spectrum of the Solar Photosphere from 13,500 to 28,000 cm-1 (3570 to 7405 A), National Optical Astronomy Observatories
  21. Engvold, O., Jensen, E., Zhang, Y., & Brynildsen, N., 1989, Distribution of Velocities in the Pre-Eruptive Phase of a Quiscent Prominence, HvaOB, 13, 205
  22. Zirker, J. B. & Koutchmy, S., 1990, Prominence Fine Structure. II - Diagnostics, SoPh, 131, 107
  23. Chae, J., Park, H.-M., & Park, Y.-D., 2007, $H\alpha$ Spectral Properties of Velocity Threads Constituting a Quiescent Solar Filament, JKAS, 40, 67
  24. Heinzel, P. & Anzer, U., 2006, On the Fine Structure of Solar Filaments, ApJ, 643, L65
  25. Stellmacher, G. & Wiehr, E., 1973, Observation of an Instability in a 'Quiescent' Prominence, A&A, 24, 321
  26. Thomas, R. N., 1957, The Source Function in a Nonequilibrium Atmosphere. I. The Resonance Lines, ApJ, 125, 260
  27. Vardavas, I. M. & Cram, L. E., 1974, Partially Coherent Scattering Models for the Formation of the Chromospheric Ca II K Line, SoPh, 38, 367
  28. Zhang, Q. Z., Livingston, W. C., Hu, J., & Fang, C., 1987, Spectral Analysis and the Two-dimensional Dstribution of Physical Parameters in a Quiescent Prominence, SoPh, 114, 245
  29. Zirker, J. B. & Koutchmy, S., 1990, Prominence Fine Structure, SoPh, 127, 109

Cited by

  1. Connection Between Chromospheric Events and Photospheric Dynamics vol.288, pp.1, 2013,
  2. Fast Imaging Solar Spectrograph of the 1.6 Meter New Solar Telescope at Big Bear Solar Observatory vol.288, pp.1, 2013,
  3. FISS Observations of Vertical Motion of Plasma in Tiny Pores vol.288, pp.1, 2013,