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Orientations of Halo CMEs and Magnetic Clouds
V. Yurchyshyn, Q. Hu, R.P. Lepping, B. Lynch, J. Krall BBSO, UC Riverside, GSFC, Univ. Mich., NRL
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Introduction CMEs observed near the earth often exhibit a magnetic structure that can be described as complex ejecta, magnetic clouds, plasmoids or shocks. Well defined MCs are associated with 30-50% of CMEs MC, in turn, have magnetically organized geometry that is thought to correspond to a curved flux rope (Bothemer & Schwenn 1998) 9/16/2018 2006 SPD Meeting, Durham, NH
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Three part structure of CMEs
White light morphology of CMEs seems to bear information on their magnetic structure: they are organized in the axial direction, which corresponds to the axis of the underlying erupting flux rope (Cremades & Bothmer, 2004) 9/16/2018 2006 SPD Meeting, Durham, NH
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Halo CMEs Halo CMEs are 2D projection of a 3D structure and they often exhibit various sizes and shapes. Many of them can be enveloped by an ellipse and fitted with a cone model (Zhao, Plunkett & Liu 2002, Xie Ofman & Lawrence 2004; Zhao 2005) 9/16/2018 2006 SPD Meeting, Durham, NH
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Halo CMEs and Erupting Flux Rope Modeling
In this study we assume that halo elongation indicates the orientation of an erupting flux rope sun Solid – ACE Dashed – Model Model halo CME top view earth 9/16/2018 2006 SPD Meeting, Durham, NH
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Oct 28 and Nov Events Nov Elongation of a halo CME closely matches the orientation of the erupting flux rope Oct 9/16/2018 2006 SPD Meeting, Durham, NH
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Data & Analysis Selected 25 halo CME -- MC events
Determined the orientation of CMEs Determined the clock angle of MCs: Grad-Shafranov MC reconstruction by Q. Hu MC fitting by Lepping et al. (2006) MC fitting by Lynch et al. (2005) MC fitting with the EFR model (J. Krall & V. Yurchyshyn) 9/16/2018 2006 SPD Meeting, Durham, NH
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Orientation of 25 halo CMEs
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Results Ovals – CMEs, lines – MCs.
Short lines are used when the difference between CME and MC orientations, , exceeds 45 deg. Black dotted line – mean MC orientation angle Green boxes: 15 events (60%) < 45 deg Red boxes: 8 events (32%) > 45 deg Blue boxes: 2 events (8%) ? 9/16/2018 2006 SPD Meeting, Durham, NH
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What Does This Result Mean?
For 60% of events (“green”) the CME elongation agrees with MC orientations What about the “red” events? Was our initial assumption wrong? Or is there something that affects a coronal ejecta? Is there any systematic difference between the CMEs and MCs? Can MCs be deflected and their orientation changed during the propagation toward the Earth? 9/16/2018 2006 SPD Meeting, Durham, NH
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CMEs & Heliospheric Current Sheet
CMEs disrupt heliospheric magnetic fields (Zhao & Hoeksema 1996) Fast moving CMEs interact w/ upstream plasma, shock formation (Gosling et al., 1994; Howard & Tappin 2006) CMEs may “displace” and “push” the heliospheric magnetic fields (Smith 2001) Most CMEs may be associated with HCS, which is considered to be a conduit for CMEs (Crooker et al., 1993) Does the heliosphere affects CMEs? 9/16/2018 2006 SPD Meeting, Durham, NH
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Comparison between CMEs, HCS and MCs
Wilcox Solar Observatory Coronal Field Map at 2.5R 9/16/2018 2006 SPD Meeting, Durham, NH
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Results of the Comparison
13 events CME,MC<45 deg and MC agrees w/HCS 7 events CME,MC>45 deg, while MC agrees w/HCS 2 events CME,MC<45 deg, however MC HCS (V>2000km/s) 1 event CME,MC>45 deg, MC is to HCS 2 events – uncertain 9/16/2018 2006 SPD Meeting, Durham, NH
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Orientations of CMEs, HCS and MCs are similar
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Do CMEs rotate to align w/HCS?
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Are Fast CMEs not affected by HCS?
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Conclusions For about 60% of events the halo elongation and the MC orientation correspond to the local tilt of the HCS For majority of solar ejecta (80%), the underlying erupting flux rope at 1AU (i.e. MC) aligns itself with the HCS It seem that very fast (V>2000km/s, 2 events) CMEs maintain their orientation constant There is an indication that the degree of CME rotation , if indeed occurs, might depend on the speed of a CME: faster CMEs are less affected by the HCS (shorter interaction time? stronger CMEs?) The data seem to support our initial assumption although the results should be tested on a larger data set 9/16/2018 2006 SPD Meeting, Durham, NH
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Conclusions The data seem to support original assumption that the CME elongation represent the axis of an erupting flux rope 9/16/2018 2006 SPD Meeting, Durham, NH
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