ESTIMATING THE ARRIVAL TIME OF EARTH-DIRECTED CORONAL MASS EJECTIONS AT IN SITU SPACECRAFT USING COR AND HI OBSERVATIONS FROM<i>STEREO</i>

Mishra, Wageesh; Srivastava, Nandita

doi:10.1088/0004-637x/772/1/70

Cited by 53 publications

(85 citation statements)

References 82 publications

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“…In this case, what is seen by a spacecraft is the segment tangent to the line of sight. The triangulation concept has proven to be a useful tool for determining CME Sun-to-Earth kinematics and connecting imaging observations with in situ signatures (e.g., Liu et al 2010aLiu et al ,b, 2011Mishra and Srivastava 2013). Details of when, where, and how CMEs accelerate/decelerate in interplanetary space can be quantified using the kinematics derived with the triangulation method.…”

Section: A Brief Overview Of Cme Kinematicsmentioning

confidence: 99%

The Physical Processes of CME/ICME Evolution

et al. 2017

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As observed in Thomson-scattered white light, coronal mass ejections (CMEs) are manifest as large-scale expulsions of plasma magnetically driven from the corona in the most energetic eruptions from the Sun. It remains a tantalizing mystery as to how these erupting magnetic fields evolve to form the complex structures we observe in the solar wind at Earth. Here, we strive to provide a fresh perspective on the post-eruption and interplanetary evolution of CMEs, focusing on the physical processes that define the many complex interactions of the ejected plasma with its surroundings as it departs the corona and propagates through the heliosphere. We summarize the ways CMEs and their interplanetary CMEs (ICMEs) are rotated, reconfigured, deformed, deflected, decelerated and disguised during their journey through the solar wind. This study then leads to consideration of how structures originating in coronal eruptions can be connected to their far removed interplanetary counterparts. Given that ICMEs are the drivers of most geomagnetic storms (and the sole driver of extreme storms), this work provides a guide to the processes that must be considered in making space weather forecasts from remote observations of the corona.

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Section: A Brief Overview Of Cme Kinematicsmentioning

confidence: 99%

The Physical Processes of CME/ICME Evolution

et al. 2017

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“…We determine the kinematics of the CME leading front with a triangulation technique 18,19 . This technique has no free parameters and has had success in tracking interplanetary propagation of various CMEs [20][21][22][23][24][25][26] . STEREO B and SOHO provide the best elongation measurements owing to their vantage points, as shown in Fig.…”

Section: Multi-point Imaging Observationsmentioning

confidence: 99%

Observations of an extreme storm in interplanetary space caused by successive coronal mass ejections

et al. 2014

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Space weather refers to dynamic conditions on the Sun and in the space environment of the Earth, which are often driven by solar eruptions and their subsequent interplanetary disturbances. It has been unclear how an extreme space weather storm forms and how severe it can be. Here we report and investigate an extreme event with multi-point remote-sensing and in situ observations. The formation of the extreme storm showed striking novel features. We suggest that the in-transit interaction between two closely launched coronal mass ejections resulted in the extreme enhancement of the ejecta magnetic field observed near 1 AU at STEREO A. The fast transit to STEREO A (in only 18.6 h), or the unusually weak deceleration of the event, was caused by the preconditioning of the upstream solar wind by an earlier solar eruption. These results provide a new view crucial to solar physics and space weather as to how an extreme space weather event can arise from a combination of solar eruptions.

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“…To track and estimate the arrival times of the CMEs in the heliosphere using HI1 & 2 images, we constructed J-maps based on the method developed by Sheeley et al (1999); Davies et al (2009) and derived the variation of elongation of selected features with time. The details about extraction of strip of constant position angle, selection of bin size and adopted procedure for construction of J-maps and derivation of elongation angle from it has been described in section 3.1.1 of Mishra and Srivastava (2013). The positively inclined bright features in the J-maps (Figure 4) correspond to enhanced density structure of the CMEs.…”

Section: Tracking Of Cmes In Hi Field-of-viewmentioning

confidence: 99%

“…Vršnak et al (2013) have shown that drag parameter lies in the range of (0.2 -2.0) × 10 −7 km −1 . Using these values of the drag parameter in the DBM, the arrival time of CME at L1 can be predicted with a reasonably good accuracy (Vršnak et al, 2013;Mishra and Srivastava, 2013). The estimated speed, time and distance (v 0 , t 0 and R ) of LE of CME1 (green track in J-map) are used as inputs in the DBM, corresponding to extreme range of drag parameter, to predict its arrival time and transit speed at L1.…”

Section: Arrival Time Of Tracked Featuresmentioning

confidence: 99%

“…Various techniques based on stereoscopic observations which estimate the 3D kinematics of CMEs in the heliosphere have been developed (Mierla et al, 2008;Thernisien, Vourlidas, and Howard, 2009;Thompson, 2009;Liu et al, 2010a;Lugaz et al, 2010;Davies et al, 2013). Using these techniques, association of remote observations of CMEs with in situ observations has been carried out by Liu et al (2010b); ; Kilpua et al (2012); Möstl et al (2012); Mishra and Srivastava (2013); . Also, several models have been developed for predicting the arrival time of CMEs at 1 AU (Gopalswamy et al, 2000;Vršnak et al, 2013).…”

Section: Introductionmentioning

confidence: 99%

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Evolution and Consequences of Interacting CMEs of 9 – 10 November 2012 Using STEREO/SECCHI and In Situ Observations

2014

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Understanding of the kinematic evolution of Coronal Mass Ejections (CMEs) in the heliosphere is important to estimate their arrival time at the Earth. It is found that kinematics of CMEs can change when they interact or collide with each other as they propagate in the heliosphere. In this paper, we analyze the collision and post-interaction characteristics of two Earth-directed CMEs, launched successively on 2012 November 9 and 10, using white light imaging observations from STEREO/SECCHI and in situ observations taken from WIND spacecraft. We tracked two density enhanced features associated with leading and trailing edge of November 9 CME and one density enhanced feature associated with leading edge of November 10 CME by constructing J-maps. We found that the leading edge of November 10 CME interacted with the trailing edge of November 9 CME. We also estimated the kinematics of these features of the CMEs and found a significant change in their dynamics after interaction. In in situ observations, we identified distinct structures associated with interacted CMEs and also noticed their heating and compression as signatures of CME-CME interaction. Our analysis shows an improvement in arrival time prediction of CMEs using their post-collision dynamics than using pre-collision dynamics. Estimating the true masses and speeds of these colliding CMEs, we investigated the nature of observed collision which is found to be close to perfectly inelastic. The investigation also places in perspective the geomagnetic consequences of the two CMEs and their interaction in terms of occurrence of geomagnetic storm and triggering of magnetospheric substorms.

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ESTIMATING THE ARRIVAL TIME OF EARTH-DIRECTED CORONAL MASS EJECTIONS AT IN SITU SPACECRAFT USING COR AND HI OBSERVATIONS FROMSTEREO

Cited by 53 publications

References 82 publications

The Physical Processes of CME/ICME Evolution

The Physical Processes of CME/ICME Evolution

Observations of an extreme storm in interplanetary space caused by successive coronal mass ejections

Evolution and Consequences of Interacting CMEs of 9 – 10 November 2012 Using STEREO/SECCHI and In Situ Observations

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