Analisis Multi-Panjang Gelombang Erupsi Filamen 29 September 2013
Keywords:
Filament Eruption, Quiescent Filament, CME, Flux Rope, Magnetic CloudAbstract
Geomagnetic disturbances in Earth's environment can be caused by Coronal Mass Ejections (CMEs) that reconnect with Earth's magnetic field. CMEs originate from the Sun, carrying magnetic fields from their source. There is a strong correlation between the magnetic flux ropes (FRs) of solar filaments and CMEs that lead to these terrestrial disturbances. CMEs can be initiated by either solar flares or quiescent filament eruptions. Key characteristics of filaments linked to CMEs include magnetic chirality patterns, flux rope (FR) configurations, sigmoid orientations, double ribbon flares, and post-eruptive arcades (PEAs). When a CME carries a flux rope (FR) into Earth's environment as an interplanetary CME (ICME) containing a magnetic cloud, it may subsequently trigger geomagnetic storms. Therefore, this study aims to analyze multi-wavelength filament eruption events to identify filament characteristics associated with geoeffective CMEs and geomagnetic storms. This study aims to analyze the filament eruption using multi-wavelength observations to identify filament properties linked to a geoeffective CME and subsequent geomagnetic storm. A quiet-Sun filament eruption on 29 September 2013 was examined. Automated identification of the filament’s chirality and tilt angle was conducted using H-alpha chromospheric images. The flux rope configuration, sigmoid structure, and PEA were analyzed using extreme ultraviolet (EUV) solar images, while the CME geometry was reconstructed using the Graduated Cylindrical Shell (GCS) fitting method. The filament detection results indicate a dextral chirality with a left-handed helical flux rope, showing a tilt angle of 71.1° consistent with the CME geometry. Examination of solar wind parameters reveals that the filament eruption, carried by a fast CME flux rope, generated a shock upon arrival at Earth. No magnetic cloud signatures were detected in the near-Earth environment. but the CME was geoeffective and triggered a moderate geomagnetic storm with Dst -72nT.
Downloads
References
Bernasconi, P. N., Rust, D. M., dan Hakim, D. (2005): Advanced automated solar filament detection and characterization code: description, performance, and results. Solar Physics, 228, 97-117.
Bothmer dan Schwenn, 1998 Bothmer, V., dan Schwenn, R. (1997): The structure and Origin of Magnetic Clouds in the Solar Wind. In Annales Geophysicae (Vol. 16, No. 1, pp. 1-24). Berlin/Heidelberg: Springer-Verlag.
Brueckner, G. E., Howard, R. A., Koomen, M. J., Korendyke, C. M., Michels, D. J., Moses, J. D. (1995). The large angle spectroscopic coronagraph (LASCO) visible light coronal imaging and spectroscopy. Solar Physics, 162(1), 357-402.
Burlaga, L., Sittler, E., Mariani, F., dan Schwenn, A. R. (1981): Magnetic loop behind an interplanetary shock: Voyager, Helios, and IMP 8 observations. Journal of Geophysical Research: Space Physics, 86(A8), 6673-6684.
Burlaga, L. F. (1988): Magnetic clouds and force‐free fields with constant alpha. Journal of Geophysical Research: Space Physics, 93(A7), 7217-7224.
Dai, J., Zhentong Li, Ya Wang, Zhe Xu, Yanjie Zhang, Leping Li, Qingmin Zhang, Yingna Su, and Haisheng Ji.. (2022). A partial filament eruption in three steps induced by external magnetic reconnection. The Astrophysical Journal, 929(1), 85.
Démoulin, P. (2008, October). A review of the quantitative links between CMEs and magnetic clouds. In Annales Geophysicae (Vol. 26, No. 10, pp. 3113-3125). Copernicus GmbH.
Chae, J. (2000). The magnetic helicity sign of filament chirality. The Astrophysical Journal, 540(2), L115.
Chen, Y., Cheng, X., Chen, J., Dai, Y., & Ding, M. (2023). Observations of a failed solar filament eruption involving external reconnection. The Astrophysical Journal, 959(2), 67.
Gilbert, H. R., Holzer, T. E., Burkepile, J. T., & Hundhausen, A. J. (2000). Active and Eruptive Prominences and TheirRelationship to Coronal MassEjections. The Astrophysical Journal, 537(1), 503.
Gopalswamy, N., Yashiro, S., Michalek, G., Stenborg, G., Vourlidas, A., Freeland, S., & Howard, R. (2009). The soho/lasco cme catalog. Earth, Moon, and Planets, 104(1), 295-313.
Gopalswamy, N., Michałek, G., Yashiro, S., Mäkelä, P., Akiyama, S., Xie, H., & Vourlidas, A. (2024). The SOHO LASCO CME Catalog--Version 2. arXiv preprint arXiv:2407.04165.
Kilpua, E., Koskinen, H. E., & Pulkkinen, T. I. (2017). Coronal mass ejections and their sheath regions in interplanetary space. Living Reviews in Solar Physics, 14(1), 5.
Li, L., Song, H., Hou, Y., Zhou, G., Tan, B., Ji, K., Xiang, Y., Hou, Z., Guo, Y., Qiu, Y. and Su, Y. (2025). Failure of a solar filament eruption caused by magnetic reconnection with overlying coronal loops. The Astrophysical Journal, 979(2), 113.
Martin, S. F. (1998): Filament chirality: A link between fine-scale and global patterns. In International Astronomical Union Colloquium (Vol. 167, pp. 419-429). Cambridge University Press.
Müller, D., Nicula, B., Felix, S., Verstringe, F., Bourgoignie, B., Csillaghy, A., Berghmans, D., Jiggens, P., García-Ortiz, J. P., Ireland, J., Zahniy, S. & Fleck, B. (2017). JHelioviewer-Time-dependent 3D visualisation of solar and heliospheric data. Astronomy & Astrophysics, 606, A10.Lepping et al. 1990.
Nitta, N. V., & Mulligan, T. (2017). Earth-affecting coronal mass ejections without obvious low coronal signatures. Solar Physics, 292(9), 125.
Pal, S., Kilpua, E., Good, S., Pomoell, J., & Price, D. J. (2021). Uncovering erosion effects on magnetic flux rope twist. Astronomy & Astrophysics, 650, A176.
Palmerio, E., Kilpua, E.K., Möstl, C., Bothmer, V., James, A.W., Green, L.M., Isavnin, A., Davies, J.A. and Harrison, R.A., 2018. Coronal magnetic structure of earthbound CMEs and in situ comparison. Space Weather, 16(5), pp.442-460.
Pinzon-Cortes, S., Gómez-Pérez, N., & Vargas Domínguez, S. (2025). Ring current local time dependence during geomagnetic storms using equatorial Dst-proxies. Acta Geodaetica et Geophysica, 60(1), 97-114.
Thernisien, A. (2011). Implementation of the graduated cylindrical shell model for the three-dimensional reconstruction of coronal mass ejections. The Astrophysical Journal Supplement Series, 194(2), 33.
Seki, D., Otsuji, K., Ishii, T. T., Asai, A., & Ichimoto, K. (2021). Relationship between three-dimensional velocity of filament eruptions and CME association. Earth, Planets and Space, 73(1), 58.
Sinha, S., Srivastava, N., & Nandy, D. (2019). Solar filament eruptions as precursors to flare–CME events: Establishing the temporal connection. The Astrophysical Journal, 880(2), 84.
Song, H., Li, L., & Chen, Y. (2022). Toward a unified explanation for the three-part structure of solar coronal mass ejections. The Astrophysical Journal, 933(1), 68.
Török, T., & Kliem, B. (2005). Confined and ejective eruptions of kink-unstable flux ropes. The Astrophysical Journal, 630(1), L97.
van Ballegooijen, A. A., & Martens, P. C. H. (1989). Formation and eruption of solar prominences. Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 343, Aug. 15, 1989, p. 971-984., 343, 971-984.
Vršnak, B., & Žic, T. (2007). Transit times of interplanetary coronal mass ejections and the solar wind speed. Astronomy & Astrophysics, 472(3), 937-943.
Vršnak, B., T. Žic, D. Vrbanec, M. Temmer, T. Rollett, C. Möstl, A. Veronig, J. Čalogović, M. Dumbović, S. Lulić, Y.-J. Moon & A. Shanmugaraju (2013). Propagation of interplanetary coronal mass ejections: The drag-based model. Solar physics, 285(1), 295-315.
Wang, J., Zhao, Y., Feng, H., Liu, Q., Tian, Z., Li, H. & Zhao, G. (2019). Comparison of counterstreaming suprathermal electron signatures of ICMEs with and without magnetic cloud: are all ICMEs flux ropes?. Astronomy & Astrophysics, 632, A129.
Xie, H., N. Gopalswamy, S. Akiyama, S. Yashiro, P. Makela (2023): Magnetic flux rope structures associated with filament channels: Two case studies, Journal of Atmospheric and Solar-Terrestrial Physics,Volume 252.
Zhang, Q. M., Z. J. Ning, Y. Guo, T. H. Zhou, X. Cheng, H. S. Ji, L. Feng, and T. Wiegelmann. (2015). Multiwavelength observations of a partially eruptive filament on 2011 September 8. The Astrophysical Journal, 805(1), 4.
Zhang, Y., Zhang, Q., Dai, J. et al. (2022) Multiwavelength Observations of a Partial Filament Eruption on 13 June 2011. Sol Phys 297, 138.
Zurbuchen, T.H., dan Richardson, I.G. (2006) Space Sciences Series of ISSI, vol 21. Springer, New York.
Downloads
Published
Data Availability Statement
All relevant data supporting the findings of this study are available within the article
