Presentation on theme: "ABSTRACT: On 17 January 2005 two ﬂare/CME events (CME 1 and CME 2 and the flares are referred to as stage 1 and 2 of a 3B/X3.8 flare), occurred in close."— Presentation transcript:
ABSTRACT: On 17 January 2005 two ﬂare/CME events (CME 1 and CME 2 and the flares are referred to as stage 1 and 2 of a 3B/X3.8 flare), occurred in close temporal succession in the same active region (NOAA AR 720, N15 ◦ W25 ◦ ). The CMEs had similar very high projected speed, above 2000 km/ s, but the second one was faster than the ﬁrst and eventually overtook it. The CMEs were associated with two successive ﬁlament eruptions and ﬂares in the same active region. The ﬂares were contiguous so that the CMEs probably resulted from the eruption of neighboring parts of the same overall magnetic conﬁguration. The soft X-ray characteristics of the two successive events were di ﬀ erent: a very slow rise to moderate peak ﬂux during stage 1 and a more impulsive rise to the X3.8 level during stage 2. Both events had a conspicuous microwave burst, but the ﬁrst one was stronger than the second, contrary to the soft X-rays. The second burst was also seen in hard X-rays by RHESSI, which was in the Earth’s shadow during the ﬁrst burst. The two events were accompanied by metre-to-kilometre type-III groups tracing energetic electrons escaping into the interplanetary space. Although the decametre-to-hectometre spectral signatures of the two type-III groups appeared similar, the metric radio emission reveals distinctive differences that corroborate evolving acceleration regions in the corona. Two decametre-to-hectometre type-II bursts detected on dynamic spectra were attributed to the shock waves driven by CME 1 and CME 2 respectively. A peculiar type- III burst was observed at the intersection, on the dynamic spectrum, of the two CME fronts (at ≈ 38 R SUN ) and it was, therefore, associated with the CME 1 -CME 2 interaction. The events under discussion were clearly related with enhanced fluxes of near-relativistic electrons at 1 AU, as observed by the ACE/EPAM experiment. The Sun to Earth transit-time estimation of the energetic electrons indicates two or three distinct injection episodes. This report provides evidence that a variety of acceleration regions contribute to energetic electrons escaping to interplanetary space. The role of shock acceleration is clearly established at low energies, by the type II radio emission. Our results favour acceleration in the course of magnetic reconnection for the escaping electron beams (type III bursts and in situ measurements). This work shows again that combined analyses of SEP and electromagnetic emission provide new insight into the solar origin of SEP events. THE 17 JANUARY 2005 COMPLEX SOLAR RADIO EVENT ASSOCIATED WITH INTERACTING FAST CORONAL MASS EJECTIONS THE 17 JANUARY 2005 COMPLEX SOLAR RADIO EVENT ASSOCIATED WITH INTERACTING FAST CORONAL MASS EJECTIONS Olga E. Malandraki 1, Alexander Hillaris 2, Karl-Ludwig Klein 3, Panagiota Preka-Papadema 2, Xenophon Moussas 2, Costas Bouratzis 2, Eleftheria Mitsakou 2, Panagiotis Tsitsipis 4, and Athanassios Kontogeorgos 4 1 Institute of Astronomy and Astrophysics, National Observatory of Athens, 11810- Athens, Greece 2 Section of Astrophysics, Astronomy and Mechanics, Department of Physics, University of Athens, Zografos- Athens, GR-15783 3 Observatoire de Paris, LESIA-CNRS UMR 8109, Univ. P & M Curie and Paris-Diderot, Observatoire de Meudon, F-92195, Meudon, France 4 Technological Educational Institute of Lamia, GR-35100, Lamia, Greece FIGURE 1: EIT  195 Ǻ images with overlaid NRH  contours in the 164-432 MHz range covering the time interval 09:00 to 10:00 UT. They show the NOAA 720 AR (N15 o W25 o ) where a 3B/X3.8 flare occured. The NRH contours indicate the movement of the radio sources in a north-west direction. This corresponds, approximately, to the movement of the main part of the two Halo CMEs (FIGURE 2).Solar north is at the top, west on the right. FIGURE 2: The two CMEs (CME 1 and CME 2 ) in close succession as recorded by the SOHO/LASCO . The most conspicuous features of both CMEs are seen above the north- western limb, though both were labelled halo CMEs in the LASCO CME catalogue. The linear fits to the trajectories of their fronts imply that the CME fronts intersect near 12:32 UT at a heliocentric distance of about 38 R SUN. In FIGURE 3 we present the FREQUENCY-TIME trajectories of CME 1 & CME 2 calculated from the Hybrid Coronal density Model . Top: Two frames of the 09:30:05 Halo CME1 with extrapolated lift of at 09:00:47 and plane-of-the-sky speed 2094 km/sec. Bottom: Two frames of the 09:54:05 Halo CME2 with extrapolated lift of at 09:38:25 and plane-of-the-sky speed 2547 km/sec. Solar north is at the top, west on the right. FIGURE 3: An overview of the complex radio event using combined ARTEMIS-IV/Wind/Waves (, ) di ﬀ erential spectrum, GOES SXR (blue) and RSTN  ﬂux 15400 MHz (Red) proﬁle and the frequency-time plots of CME 1 and CME 2 (black) calculated from the Hybrid Coronal density Model . The type IV continuum, the type III GG bursts (III 1 and III 2 ), the stages 1 and 2 of the SXR ﬂux rise, and the type III like burst (III 3 ) at the convergence of the fronts of CME 1 and CME 2 are duly annotated on the plot. Both SXR and microwave time histories indicate two successive events of energy release. GOES reports an X3.8 SXR ﬂare from 06:59 UT to 10:07 UT; it starts with a smooth increase until 09:05, followed by a slightly faster (stage 1) until 09:45 and an even faster rise (stage 2) until the peak. The gradual rise in stage 1 and the faster rise in stage 2 were each accompanied by strong microwave bursts. The type II bursts (II 1 and II 2 ) are aligned with the inferred frequency-time trajectory of the fronts of CME 1 and CME 2, therefore ascribe them to their respective bow shocks of the CMEs. The two type III groups occurred near the extrapolated lift off times of the two CMEs. FIGURE 4: ACE/EPAM  energetic electron enhancements in response to the January 17 solar activity. 1-min averaged deﬂected electron intensities for the interval 04:00-20:00 UT on January 17 of four magnetically deﬂected electron channels (38-315 keV) from the EPAM/CA60. The horizontal lines denote pre-event ambient intensity; the solid vertical line marks the arrival of an interplanetary forward shock (FS) at 07:12 UT at ACE . Inserts a and b present Pitch-Angle Distributions snapshots at the onset of the event at about 11:00 UT and at about 12:10 UT; normalized di ﬀ erential electron intensity is plotted versus the cosine of the pitch angle. The bottom right insert is an overview of the 20-min averaged di ﬀ erential intensities for the interval January 15-20, 2005. The first significant rise (>2σ) of the electron intensities occurs at 10:00 UT (The spiky increase at about 10:40 UT is probably due to X-ray contamination). We estimate a travel time of about 15 min, which indicates the electrons were released at ≈09:45 UT at the Sun (photon arrival at 09:53 UT). This electron release is, probably, related to III 1 and III 2 (FIGURE 3). Follows a significant and more abrupt rise at all energies. Extrapolation of this second rise to the pre-event background intensities indicates a start at ≈ 12:00 UT. The electron PADs (snapshot b) indicate stronger unidirectional anisotropies are observed in association with this electron enhancement, which indicate fresh injection of energetic electrons between the Sun and the spacecraft. This timing is consistent with the III 3 burst observed at ≈ 11:37 UT during the CME 1 -CME 2 interaction. RESULTS Type III 1 : The type III 1 bursts are most prominent at low frequencies, upstream of the inferred CME 1 front, while at higher frequencies more complex bursts are observed that mostly have a distinct low-frequency cut off. The low-frequency cut off of the decimetric bursts in the early phase of III 1 can be explained by interactions of the electron beams with the turbulence near the front of CME 1 because there is a distinct lack of (reverse-slope) RS type IIIs. This point to ﬂare-accelerated electrons at the origin of the first group of decametric-to-kilometric type III bursts. Type III 2 : Here the decimetric-metric counterpart is mostly reverse-slope bursts and an intense type IV continuum that gradually progresses toward lower frequencies. The type III emission starts at lower frequencies than during III 1. The change of sign of the drift rate suggests that in this group the accelerator is located above the dm-metre wave radio sources, and this is in agreement with the estimated position of the CME 2 front. The acceleration could be ascribed to the CME 2 shock but the type IV emission clearly does not follow the type II burst as it drifts towards lower frequency, yet it persists for tens of minutes or more. This suggests that the site of the electron acceleration stays increasingly behind the CME 2 front and its shock, and is consistent with an interpretation of the electron acceleration in terms of reconnection in the corona behind the CME 2. Type III 3 CME 1 -CME 2 interaction: The association of CME interaction with particle acceleration has been ascribed to acceleration by the shock of the second CME as it traverses the previous one (, ), although they also mention magnetic reconnection. But, in this case, the spectral nature of the radio emission shows that the accelerator must release the electron beams onto open solar wind-type field lines it, thus, favours magnetic reconnection, probably, in sheath regions with strong magnetic fields of interplanetary origin, draped around the CMEs. Near-relativistic electrons at 1 AU: The observations strongly suggest that successive intensity increases are first due to the coronal acceleration in the ﬂare/CME event, and then to an episode during the interaction of CME 1 -CME 2. The escape of these electrons to ACE confirms that the electrons cannot have been accelerated in the body of the first CME, even if a shock driven by the second one passed through it. Neither can they originate from reconnection between closed magnetic field lines of the two CMEs. The electrons must rather be accelerated in regions from where they have ready access to solar wind magnetic field lines. This is consistent with a common acceleration of the mildly relativistic electrons and the electron beams at lower energies that produce the type III emission. REFRENCES  Bougeret, J.L., Kaiser,M.L., Kellogg, et al. : 1995, Space Sci. Rev. 71, 231.  Brueckner, G.E., Howard, R.A., Koomen, et al.: 1995, Solar Phys. 162, 357.  Caroubalos, C., Maroulis, D., Patavalis, et al.: 2001, Exp. Astron. 11, 23.  Gold, R.E., Krimigis, S.M., Hawkins et al.: 1998, Space Sci. Rev. 86, 541.  Gopalswamy, N., Yashiro, S., Kaiser, et al.: 2001, Astrophys. J. Lett. 548, L91.  Gopalswamy, N., Yashiro, S., Kaiser, et al.: 2002, Geophys. Res. Lett. 29, 080000.  Guidice D.A., Cliver E.W., Barron W.R., Kahler S.: 1981, Bull. Amer. Astron. Soc., 13, 553.  Kontogeorgos, A., Tsitsipis, P., Caroubalos et al.: 2006, Exp. Astron. 21, 41.  Delaboudiniere, J.P., Artzner, G.E., Brunaud et al.: 1995, Solar Phys. 162, 291.  Kerdraon A., Delouis J.M.: 1997, In: Trottet, G. (ed.) Coronal Phys. from Radio and Space Observations, Berlin Springer Verlag, Lecture Notes in Phys., 483,192  Papaioannou, A., Malandraki, O., Belov, A., et al.: 2010, Solar Phys. 266, 181.  Vrsnak, B., Magdalenic, J., Zlobec, P.: 2004, Astron. Astrophys. 413, 753.