Linking two consecutive non-merging magnetic clouds with their solar sources
| Autor: | Dasso, S., Mandrini, C.H., Schmieder, B., Cremades, H., Cid Tortuero, Consuelo, Cerrato Montalbán, Yolanda, Saiz Villanueva, María Elena, Démoulin, P., Zhukov, A.N., Rodriguez, L., Aran, A., Menvielle, M., Poedts, S. |
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| Přispěvatelé: | Universidad de Alcalá. Departamento de Física y Matemáticas |
| Rok vydání: | 2009 |
| Předmět: |
Ciencia
Ciencias Físicas Physics ASTROPHYSICS AND ASTRONOMY: RADIO EMISSIONS [SOLAR PHYSICS] INTERPLANETARY MAGNETIC FIELDS [INTERPLANETARY PHYSICS] Física EJECTA DRIVER GASES AND MAGNETIC CLOUDS [INTERPLANETARY PHYSICS] CORONAL MASS EJECTIONS [INTERPLANETARY PHYSICS] purl.org/becyt/ford/1.3 [https] Space Physics Astronomía purl.org/becyt/ford/1 [https] CIENCIA Solar and Stellar Astrophysics ASTROPHYSICS AND ASTRONOMY: CORONAL MASS EJECTIONS [SOLAR PHYSICS] CIENCIAS NATURALES Y EXACTAS |
| Zdroj: | e_Buah Biblioteca Digital Universidad de Alcalá instname CONICET Digital (CONICET) Consejo Nacional de Investigaciones Científicas y Técnicas instacron:CONICET |
| Popis: | On 15 May 2005, a huge interplanetary coronal mass ejection (ICME) was observed near Earth. It triggered one of the most intense geomagnetic storms of solar cycle 23 (Dst peak = -263 nT). This structure has been associated with the two-ribbon flare, filament eruption, and coronal mass ejection originating in active region 10759 (NOAA number). We analyze here the sequence of events, from solar wind measurements (at 1 AU) and back to the Sun, to understand the origin and evolution of this geoeffective ICME. From a detailed observational study of in situ magnetic field observations and plasma parameters in the interplanetary (IP) medium and the use of appropriate models we propose an alternative interpretation of the IP observations, different to those discussed in previous studies. In our view, the IP structure is formed by two extremely close consecutive magnetic clouds (MCs) that preserve their identity during their propagation through the interplanetary medium. Consequently, we identify two solar events in H{\alpha} and EUV which occurred in the source region of the MCs. The timing between solar and IP events, as well as the orientation of the MC axes and their associated solar arcades are in good agreement. Additionally, interplanetary radio type II observations allow the tracking of the multiple structures through inner heliosphere and pin down the interaction region to be located midway between the Sun and the Earth. The chain of observations from the photosphere to interplanetary space is in agreement with this scenario. Our analysis allows the detection of the solar sources of the transients and explains the extremely fast changes of the solar wind due to the transport of two attached (though nonmerging) MCs which affect the magnetosphere. Comisión Interministerial de Ciencia y Tecnología-CICYT Ministerio de Educación y Ciencia |
| Databáze: | OpenAIRE |
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