An ice‐cream cone model for coronal mass ejections

Xue, Xianghui; Wang, Chuanbing

doi:10.1029/2004ja010698

Cited by 90 publications

(113 citation statements)

References 23 publications

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“…This measurement shows that the projection effect was lowest for the SOHO view compared to other views from the STEREO satellites. We confirmed the above argument again by applying the ice cream cone model of CME (Xue et al 2005) to the LASCO CME data and found that the source longitude of the CME is E89. These results are consistent with the study by Gopalswamy et al (2009), who reported the expected source locations (E102, E81, and E58) of the CME deduced from the different views of SA, SOHO, and SB, respectively.…”

Section: -D Cme Kinematicssupporting

confidence: 68%

Relationship between multiple type II solar radio bursts and CME observed by STEREO/SECCHI

Cho

Bong

Moon

et al. 2011

A&A

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Aims. Two or more type II bursts are occasionally observed in close time sequence during solar eruptions, which are known as multiple type II bursts. The origin of the successive burst has been interpreted in terms of coronal mass ejections (CMEs) and/or flares. Detailed investigations of the relationship between CMEs and the bursts enable us to understand the nature of the multiple type II bursts. In this study, we examine multiple type II bursts and compare their kinematics with those of a CME occurring near the time of the bursts. Methods. To do this, we selected multiple type II bursts observed by the Culgoora radiospectrographs and a limb CME detected in the low corona field of view (1.4−4 R s ) of a STEREO/SECCHI instrument on December 31, 2007. To determine the 3D kinematics of the CME, we applied the stereoscopic technique to the STEREO/SECCHI data. Results. Our main results are as follows: (1) the multiple type II bursts occurred successively at ten minute intervals and displayed various emission structures and frequency drifting rates; (2) near the time of the bursts, the CME was observed by STEREO and SOHO simultaneously, but no evidence of other CMEs was detected; (3) inspection of the 3D kinematics of the CME using the stereoscopic observation by STEREO/SECCHI revealed that the CME propagated along the eastward radial direction as viewed from the Earth; (4) very close time and height associations were found between the CME nose and the first type II burst, and between CME-streamer interaction and the second type II burst. Conclusions. On the basis of these results, we suggest that a single shock in the leading edge of the CME could be the source of the multiple type II bursts and support the notion that the CME nose and the CME-streamer interaction are the two main mechanisms able to generate the bursts.

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Section: -D Cme Kinematicssupporting

confidence: 68%

Relationship between multiple type II solar radio bursts and CME observed by STEREO/SECCHI

Cho

Bong

Moon

et al. 2011

A&A

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“…By combining the ice cream cone model (Xue et al 2005) and CME deflection model , we find that besides the obvious factor of the source region location, the span angle and the deflection are also important in determining the probability of a CME impacting an object such as the Earth. The large span angles of some CMEs (e.g., the second, third, and possible fourth) account for the fact that they are observed by the Wind spacecraft (i.e., they hit the Earth), even though their source region locations are not close to the solar central meridian.…”

Section: Conclusion and Discussionmentioning

confidence: 99%

“…Thus, many researchers suggest that the geometrical properties of most CMEs could be inferred indirectly by a cone model (Howard et al 1982;Fisher & Munro 1984;Leblanc et al 2001;Zhao et al 2002;Michalek et al 2003;Xie et al 2004). Recently, an ice cream cone model was further developed by Xue et al (2005), whose work showed consistency between the fitted and observed speeds of CMEs.…”

Section: Ice Cream Cone Modelmentioning

confidence: 99%

“…Since there is a sufficient number of LASCO images for this CME, its projected speeds at all the given directions can be obtained by fitting the measured height-time curves with linear lines. Second, assuming that this CME originated from the associated flare location, we can use the equations listed in Table 1 of the Xue et al (2005) paper to fit the measured projected speeds with the ice cream cone model, in which the span angle is fitted as a parameter. The least-squares fit is applied to get the best solution, as shown in Figure 5.…”

Section: Ice Cream Cone Modelmentioning

confidence: 99%

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Impact of Major Coronal Mass Ejections on Geospace during 2005 September 7–13

Wang¹,

Xue²,

Shen³

et al. 2006

ApJ

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We have analyzed five major CMEs originating from NOAA active region (AR) 808 during the period of 2005 September 7-13, when the AR 808 rotated from the east limb to near solar meridian. Several factors that affect the probability of the CMEs' encounter with the Earth are demonstrated. The solar and interplanetary observations suggest that the second and third CMEs, originating from E67 and E47 , respectively, encountered the Earth, while the first CME originating from E77 missed the Earth, and the last two CMEs, although originating from E39 and E10 , respectively, probably only grazed the Earth. On the basis of our ice cream cone mode and CME deflection model, we find that the CME span angle and deflection are important for the probability of encountering Earth. The large span angles allowed the middle two CMEs to hit the Earth, even though their source locations were not close to the solar central meridian. The significant deflection made the first CME totally miss the Earth even though it also had wide span angle. The deflection may also have made the last CME nearly miss the Earth even though it originated close to the disk center. We suggest that, in order to effectively predict whether a CME will encounter the Earth, the factors of the CME source location, the span angle, and the interplanetary deflection should all be taken into account. Subject headingg s: solar-terrestrial relations -Sun: coronal mass ejections (CMEs)

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“…where φ/2 represents the cone half-angle expressed in radians, i.e., φ is the CME-cone angular width (for details of the cone model see Zhao et al 2002;Michałek et al 2003;Xie et al 2004;Schwenn et al 2005;Xue et al 2005). Below we assume that the width φ and the CME mass m do not change significantly beyond r = 20 r .…”

Section: The Modelmentioning

confidence: 99%

The role of aerodynamic drag in propagation of interplanetary coronal mass ejections

Vršnak

Žic

Falkenberg

et al. 2010

A&A

122

115

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Context. The propagation of interplanetary coronal mass ejections (ICMEs) and the forecast of their arrival on Earth is one of the central issues of space weather studies. Aims. We investigate to which degree various ICME parameters (mass, size, take-off speed) and the ambient solar-wind parameters (density and velocity) affect the ICME Sun-Earth transit time. Methods. We study solutions of a drag-based equation of motion by systematically varying the input parameters. The analysis is focused on ICME transit times and 1 AU velocities. Results. The model results reveal that wide ICMEs of low masses adjust to the solar-wind speed already close to the sun, so the transit time is determined primarily by the solar-wind speed. The shortest transit times and accordingly the highest 1 AU velocities are related to narrow and massive ICMEs (i.e. high-density eruptions) propagating in high-speed solar wind streams. We apply the model to the Sun-Earth event associated with the CME of 25 July 2004 and compare the results with the outcome of the numerical MHD modeling.

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An ice‐cream cone model for coronal mass ejections

Cited by 90 publications

References 23 publications

Relationship between multiple type II solar radio bursts and CME observed by STEREO/SECCHI

Relationship between multiple type II solar radio bursts and CME observed by STEREO/SECCHI

Impact of Major Coronal Mass Ejections on Geospace during 2005 September 7–13

The role of aerodynamic drag in propagation of interplanetary coronal mass ejections

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