Abstract
Two large stable solar filaments were used as test tracers to determine the apparent synodic rotation rate as a function of the central meridian distance for several filaments' segments at different heights. An analytic fitting procedure was applied to determine simultaneously the real synodic rotation rate and the height of the traced filament segments. The determined heights were compared with the values obtained from the widths of filament contours on the solar disk and with the values obtained by direct measurements at the solar limb. Furthermore, the obtained rotation rates and heights of the filaments' segments close to the filaments' pivot points were compared with the values obtained using two successive central meridian passages. Finally, sources and scales of errors were investigated and possible implications on the previous studies of the solar differential rotation were considered.
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References
Adams, W. M. and Tang, F.: 1977, Solar Phys. 55, 499.
Aschwanden, M. J. and Bastian, T. S.: 1994a, Astrophys. J. 426, 425.
Aschwanden, M. J. and Bastian, T. S.: 1994b, Astrophys. J. 426, 434.
Aschwanden, M. J., Lim, J., Gary, D. E., and Klimchuk, J. A.: 1995, Astrophys. J. 454, 512.
Balthasar, H. and Wöhl, H.: 1983, Solar Phys. 88, 71.
Balthasar, H. Vázquez, M. and Wöhl, H.: 1986, Astron. Astrophys. 155, 87.
Brajša, R., Vršnak, B., Ruždjak, V., Schroll, A., Pohjolainen, S., Urpo, S., and Teräsranta, H.: 1991, Solar Phys. 133, 195.
Brajša, R., Ruždjak, V., Vršnak, B., Pohjolainen, S., Urpo, S., Schroll, A. and Wöhl, H.: 1997a, Solar Phys. 171, 1.
Brajša, R., Ruždjak, V., Vršnak, B., Pohjolainen, S., Urpo, S., and Wöhl, H.: 1997b, Hvar Obs. Bull. 21, 67.
Bruzek, A.: 1961, Z. Astrophys. 51, 75.
d'Azambuja, M. and d'Azambuja, L.: 1948, Ann. Obs. Paris-Meudon VI, Fasc. VII.
Dumitrache, C.: 1994, in A.v. Alvensleben (ed.), JOSO Annual Report 1993, p. 134.
Förster, M.: 1979, Staatsexamensarbeit, Univ. of Göttingen.
Liu, S.-Y. and Kundu, M. R.: 1976, Solar Phys. 46, 15.
Mouradian, Z., Martres, M. J., Soru-Escaut, I., and Gesztelyi, L.: 1987, Astron. Astrophys. 183, 129.
Roša, D.: 1996, Hvar Obs. Bull. 20, 41.
Roša, D., Vršnak, B. and Božíc, H.: 1995, Hvar Obs. Bull. 19, 23.
Roša, D., Vršnak, B., Božíc, H., Brajša, H., Ruždjak, V., Schroll, A., and Wöhl, H.: 1998, Solar Phys. 179, 237(Paper I).
Schröter, E.-H.: 1985, Solar Phys. 100, 141.
Schröter, E.-H. and Wöhl, H.: 1975, Solar Phys. 42, 3.
Schröter, E.-H. and Wöhl, H.: 1976, Solar Phys. 49, 19.
Snodgrass, H. B.: 1992, in K. L. Harvey (ed.), 'The Solar Cycle', 12th Sac. Peak Summer Workshop, ASP Conf. Ser. 27, 205.
Solonsky, Yu. A. and Makarova, V. V.: 1992, Solar Phys. 139, 233.
Teräsranta, H.: 1982, inS. Urpo (ed.), Proc. XVI Finnish Astronomer's Days, Helsinki Univ. Tech., Radio Lab. Report S 129, p.29.
Urpo, S., Pohjolainen, S., Teräsranta, H., Vršnak, B., Ruždjak, V., Brajša, R. and Schroll, A.: 1989, in V. Ruždjak and E. Tandberg-Hanssen (eds.), 'Dynamics of Quiescent Prominences', IAU Colloq. 117, Hvar Obs. Bull. 13, 437.
Wöhl, H.: 1990, in L. Dezsö (ed.), 'The Dynamic Sun', 6th European Meeting on Solar Physics, Publ. Debrecen Obs. 7, 19.
Wright, C. S.: 1991, Catalogue of Solar Filament Disappearances 1964–1980, Electronics Research Laboratory, Defence Science and Technology Organisation, Salisbury, Australia.
Zebedin, C., Schroll, A., and Haupt, H.: 1994, in A.v. Alvensleben (ed.), JOSO Annual Report 1993, p. 133.
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Vršnak, B., Roša, D., Božić, H. et al. Height of Tracers and the Correction of the Measured Solar Synodic Rotation Rate: Demonstration of the Method. Solar Physics 185, 207–225 (1999). https://doi.org/10.1023/A:1005107424355
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DOI: https://doi.org/10.1023/A:1005107424355