Linking two consecutive non-merging magnetic clouds with their solar sources
Identifiers
Permanent link (URI): http://hdl.handle.net/10017/29099DOI: 10.1029/2008JA013102
ISSN: 0148-0227
Date
2009-02-28Funders
Comisión Interministerial de Ciencia y Tecnología-CICYT
Ministerio de Educación y Ciencia
Bibliographic citation
Journal of Geophysical Research, 2009, n. 114, p. 1-17
Keywords
Solar and Stellar Astrophysics
Space Physics
Project
info:eu-repo/grantAgreement/CICYT//ESP2005-07290-C02-01/ES/Solar Orbiter, meteorología espacial e instrumentación
info:eu-repo/grantAgreement/CICYT//ESP2006-08459/Minería de datos de Soho
info:eu-repo/grantAgreement/MEC//AYA 2004-0322/ES
info:eu-repo/grantAgreement/MEC//AYA2007-60724/ES/PARTICULAS ENERGETICAS SOLARES: ANALISIS DE DATOS Y MODELOS. SOLPENCO2/
Document type
info:eu-repo/semantics/article
Version
info:eu-repo/semantics/publishedVersion
Publisher's version
http://dx.doi.org/10.1029/2008JA013102Rights
Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
© American Geophysical Union, 2009
Access rights
info:eu-repo/semantics/openAccess
Abstract
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.
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Linking_Saiz_JournalGeophysica ... | 8.610Mb |
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