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Stationary Parts of an EIT and Moreton Wave: a Topological Model

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Stationary Parts of an EIT and Moreton Wave: a Topological Model A&A 465, 603–612 (2007) Astronomy DOI: 10.1051/0004-6361:20065845 & c ESO 2007 Astrophysics Stationary parts of an EIT and Moreton wave: a topological model C. Delannée1, J.-F. Hochedez1, and G. Aulanier2 1 Royal Observatory of Belgium, Brussels, Belgium e-mail: [email protected] 2 LESIA, Meudon observatory, Meudon, France Received 16 June 2006 / Accepted 30 August 2006 ABSTRACT Context. EIT and Moreton waves came into focus in 1997, when a propagating disturbance on a large area of the solar disc was discovered. The process generating the EIT and Moreton waves has been frequently discussed. Aims. On May 2, 1998, a halo CME was observed related to an EIT wave, a Moreton wave, a X1 flare, radio emission sources, and dimmings. We studied this event to find the relation between all these structures. Methods. We use and co-align multi-wavelength observations and the online potential field source surface (pfss) package. Results. The observed EIT and Moreton waves present some brightenings that remain at the same location. We relate the connectivity of the coronal potential magnetic field to the stationary brightenings. We find that the areas where the magnetic field lines have drastic jumps of connectivity are cospatial to the stationary brightenings of the waves. Conclusions. We conclude that the EIT and Moreton waves may be due to Joule heating resulting from the generation of electric currents in the neighboring area of the drastic jumps of magnetic connectivity, while the magnetic field lines are opening during a CME. Key words. Sun: coronal mass ejections (CMEs) – Sun: magnetic fields – Sun: activity – Sun: flares – Sun: chromosphere – Sun: corona 1. Introduction to reproduce certain properties of the observed wave-like struc- tures. In this context, EIT waves could be used as proxies for Three wave-like structures with the length scale of the solar coronal seismology, so as to derive the coronal physical parame- radius can be observed in three different spectral band passes. ters, which are important in terms of space weather applications First, the Moreton waves are large arch-shaped brightenings (Ballai et al. 2005). α propagating through the sun observed in H (Dodson 1949). However, to our knowledge only four observed waves are They originate close to a flare that occurred few tens of seconds almost full circles (the ones reported in Thompson 1998, 1999, earlier (Warmuth et al. 2004a). 2000a). The circles of these four events are not complete: they Second, the EIT waves are mainly observed with the present gaps of brightness. Apart from these rare cases, the Extreme ultra-violet Imaging Telescope (EIT, Delaboudinière waves are always observed with a quite narrow width: from 50 to et al. 1995) with the filter centered on 195 Å and comprising 150 degrees in all studied spectral wavelengths (Warmuth et al. the Fe XII emission line. Thompson et al. (1998) first reported 2004a). A magnetosonic wave should almost always be a full an arch-shaped bright structure traveling across the sun that was circle even if the observed circle is dotted and deformed by the named EIT wave. The morphologies and kinematics of this wave irregular medium in which it is propagating, as presented in the made the author suggest that it was very likely the Moreton simulations (Wu et al. 2001, 2005; Wang et al. 2000). Moreover wave. Thomspon et al. (1999) showed that the EIT and Moreton Delannée (2000) showed in four cases that some parts of the waves are quite cospatial when the two waves are observed in a bright front of EIT waves can remain at the same location for 1 h, same event. which does not seem in accordance with a propagating wave. Finally, X-ray waves were reported recently by Warmuth Delannée & Aulanier (1999) and Cliver et al. (2005) showed et al. (2005). X-ray waves also seem to originate from a flare, and that nearly 100% of EIT waves are related to a CME. On the are rather cospatial with EIT and Moreton waves. The fact that contrary, only 6% of flares are related to an EIT wave (Delannée so many coronal and chromospheric waves are cospatial leads & Aulanier 1999), 1% of B-class flares are related to EIT waves the authors to conclude that they are part of the same “decelerat- (Cliver et al. 2005). Recently Chen (2006) claimed that none of ing disturbance”. 14 non-CME associated energetic flares are related to an EIT All the waves reported in the articles mentioned above are wave. Moreover the EIT waves are systematically associated in each related to a flare, and seem to originate from them. So, precise configuration with dimmed regions of the solar surface in the waves are interpreted as a magnetosonic wave initiated in 195 Å (Delannée 2000). Harra & Sterling (2001) showed that the a pressure pulse associated with the flare. Uchida (1968), Wu dimmings occurring during a CME are due to density decrease et al. (2001, 2005), and Wang et al. (2000) performed numerical and matter ejection. So, the EIT waves seem more related to simulations of magnetosonic waves initiated by a pressure pulse CMEs than to flares. Therefore, EIT waves cannot be blast waves Article published by EDP Sciences and available at http://www.aanda.org or http://dx.doi.org/10.1051/0004-6361:20065845 604 C. Delannée et al.: Stationary EIT and Moreton wave driven by a pressure pulse (Warmuth 2006). The Moreton waves Since the physical nature of EIT waves is still strongly de- are observed in red shift followed by blue shift in the wings of bated, the objective of this paper was to test the relative strengths the Hα line (Warmuth et al. 2004b). The blue shift has a long and weaknesses of each interpretation through the revisiting of a lifetime so that it seems more related to matter ejection than to well documented event, already analyzed by several groups. We the oscillation of the matter in the wave. Thus, the Moreton wave thus chose an event that occurred on May 2, 1998 and that com- is also closely associated with a CME. Since CMEs are strong prised a X1 flare, an EIT wave, a Moreton wave, radio sources, drivers of space weather and since EIT waves appear to be an and a halo CME. To our knowledge, 6 articles have already been observational signature of their early development in the corona, published analyzing the relations of the different structures ap- understanding their physical properties has strong implications pearing during the event. Their results are summarized in Sect. 2. in terms of space weather predictions. In the present study we re-analyze the same data, but using so- called “derotated base difference images” (DBDI). In these im- CMEs are believed to result from the fast expansion of previ- ages, we then took special care to identify and study stationary ously stressed magnetic fields, driven by ideal or resistive MHD brightenings that appear along the path of the EIT and Moreton instabilities (see, e.g., the models of Amari et al. 1996; and waves. We overlaid the DBDI images on coronal field lines in- Antiochos et al. 1999). When CMEs are launched, their expan- tegrated from a potential field extrapolation. We found that the sion velocities quickly reach a significant fraction of the Alfvén stationary brightenings are located in a region of drastic jumps speed. So CMEs lead to strong magnetic perturbations in the in the magnetic field lines connectivity. This study first leads us corona. The latter must naturally result in large-amplitude fast- to address the following question: observationally, are the sta- mode magnetosonic waves. While they propagate, such strong tionary parts of the front of EIT waves a rare and peculiar class MHD waves can produce significant mass flows and pressure among all EIT wave related events (as advocated by Warmuth variations. These processes are clearly presented in 2.5D MHD et al. 2004a) or are they generic and typical, so that the EIT calculations where the magnetic perturbation that is applied is waves really moving, that are detected with the EIT time cadence modeled in the form of strong field line shearing motions (Wu of image, are rather exceptional instead? We argue for the latter et al. 1983). In the same context of CME related waves, Warmuth case. In this context, we suggest that the succession of station- (2006) suggested a second possible process: EIT waves could be ary brightenings must result from the formation and dissipation piston-driven waves as well as the CME shock fronts observed of current sheets, progressively generated in large-scale quasi- ahead of the CME as type II emission in radio wavelengths. In separatrix layers, as the magnetic flux expands above the flare such cases, the expanding magnetic field would compress the site and pushes up the overlaying transequatorial field lines. plasma in the legs of the CME producing the bright EIT wave front. Based on the morphological properties of these waves ob- served in EUV in the low corona, Delannée & Aulanier (1999) 2. Summary of past studies also conjectured that EIT waves could be due to the opening of magnetic field lines. However, it was shown that the EIT wave Among the six papers that studied the May 2, 1998 event, five brightenings were stationary, and co-spatial with the footpoints analyzed the observed waves. They all interpreted them as mag- of a separatrix surface, which is by definition a discontinuity in netosonic waves. The sixth paper addressed the issue of the the field line connectivity. This first led to conjecture that the large-scale dimmings developing in the corona during the whole fast expansion of magnetic field lines, which should naturally event.
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