Three-Dimensional Evolution of Erupted Flux Ropes from the Sun (2 – 20 R⊙) to 1 AU

@article{Isavnin2013ThreeDimensionalEO,
  title={Three-Dimensional Evolution of Erupted Flux Ropes from the Sun (2 – 20 R⊙) to 1 AU},
  author={Alexey Isavnin and Angelos Vourlidas and Emilia K. J. Kilpua},
  journal={Solar Physics},
  year={2013},
  volume={284},
  pages={203-215}
}
Studying the evolution of magnetic clouds entrained in coronal mass ejections using in-situ data is a difficult task, since only a limited number of observational points is available at large heliocentric distances. Remote sensing observations can, however, provide important information for events close to the Sun. In this work we estimate the flux rope orientation first in the close vicinity of the Sun (2 – 20 R⊙) using forward modeling of STEREO/SECCHI and SOHO/LASCO coronagraph images of… 

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References

SHOWING 1-10 OF 40 REFERENCES

Grad–Shafranov Reconstruction of Magnetic Clouds: Overview and Improvements

The Grad–Shafranov reconstruction is a method of estimating the orientation (invariant axis) and cross section of magnetic flux ropes using the data from a single spacecraft. It can be applied to

ROTATION OF WHITE-LIGHT CORONAL MASS EJECTION STRUCTURES AS INFERRED FROM LASCO CORONAGRAPH

Understanding the connection between the magnetic configurations of a coronal mass ejection (CME) and their counterpart in the interplanetary medium is very important in terms of space weather

A statistical study on the geoeffectiveness of Earth‐directed coronal mass ejections from March 1997 to December 2000

[1] We have identified 132 Earth-directed coronal mass ejections (CMEs) based on the observations of the Large Angle Spectroscopic Coronagraph (LASCO) and Extreme Ultraviolet Imaging Telescope (EIT)

Reconstruction of magnetic clouds in the solar wind: Orientations and configurations

[1] We develop a new approach for determining the orientation of the axis (z) of finite-β magnetic flux ropes from single-spacecraft data. It consists of an optimization procedure based on

ROTATION OF CORONAL MASS EJECTIONS DURING ERUPTION

Understanding the connection between coronal mass ejections (CMEs) and their interplanetary counterparts (ICMEs) is one of the most important problems in solar-terrestrial physics. We calculate the

Linking Remote-Sensing and In Situ Observations of Coronal Mass Ejections Using STEREO

The twin STEREO spacecraft have been observing the Sun since 2006. Even though STEREO has only been active during solar minimum conditions so far, an important number of coronal mass ejections (CMEs)

Properties of Interplanetary Coronal Mass Ejections at One AU During 1995 – 2004

We present a comprehensive survey of 230 interplanetary CMEs (ICMEs) during 1995 – 2004 using Wind and ACE in situ observations near one AU, and examine the solar-cycle variation of the occurrence

Deflection of coronal mass ejection in the interplanetary medium

A solar coronal mass ejection (CME) is a large-scale eruption of plasma and magnetic fields from the Sun. It is believed to be the main source of strong interplanetary disturbances that may cause

STEREO observations of interplanetary coronal mass ejections and prominence deflection during solar minimum period

In this paper we study the occurrence rate and so- lar origin of interplanetary coronal mass ejections (ICMEs) using data from the two Solar TErrestrial RElation Obser- vatory (STEREO) and the Wind