scholarly journals Ensemble CME Modeling Constrained by Heliospheric Imager Observations

AGU Advances ◽  
2020 ◽  
Vol 1 (3) ◽  
Author(s):  
L. Barnard ◽  
M. J. Owens ◽  
C. J. Scott ◽  
C. A. Koning
Keyword(s):  
Heliospheric Imager

scholarly journals Validation of a priori CME arrival predictions made using real‐time heliospheric imager observations

Space Weather ◽  
2015 ◽  
Vol 13 (1) ◽  
pp. 35-48 ◽  
Author(s):  
Kimberley Tucker‐Hood ◽  
Chris Scott ◽  
Mathew Owens ◽  
David Jackson ◽  
Luke Barnard ◽  
...  
Keyword(s):  
Real Time ◽  
A Priori ◽  
Heliospheric Imager

scholarly journals Using Ghost Fronts Within STEREO Heliospheric Imager Data to Infer the Evolution in Longitudinal Structure of a Coronal Mass Ejection

Space Weather ◽  
2019 ◽  
Vol 17 (4) ◽  
pp. 539-552 ◽  
Author(s):  
C. J. Scott ◽  
M. J. Owens ◽  
C. A. Koning ◽  
L. A. Barnard ◽  
S. R. Jones ◽  
...  
Keyword(s):  
Coronal Mass Ejection ◽  
Longitudinal Structure ◽  
Mass Ejection ◽  
Heliospheric Imager

scholarly journals On the autonomous detection of coronal mass ejections in heliospheric imager data

2012 ◽  
Vol 117 (A5) ◽  
pp. n/a-n/a ◽  
Author(s):  
S. J. Tappin ◽  
T. A. Howard ◽  
M. M. Hampson ◽  
R. N. Thompson ◽  
C. E. Burns
Keyword(s):  
Coronal Mass Ejections ◽  
Autonomous Detection ◽  
Heliospheric Imager

scholarly journals Oscillations of cometary tails: a vortex shedding phenomenon?

2018 ◽  
Vol 615 ◽  
pp. A143 ◽  
Author(s):  
G. Nisticò ◽  
V. Vladimirov ◽  
V. M. Nakariakov ◽  
K. Battams ◽  
V. Bothmer
Keyword(s):  
Solar Wind ◽  
Vortex Shedding ◽  
Optical Instruments ◽  
Physical Conditions ◽  
Stereo Mission ◽  
Mhd Instability ◽  
Solar Wind Flow ◽  
Local Medium ◽  
Observed Behaviour ◽  
Heliospheric Imager

Context. During their journey to perihelion, comets may appear in the field of view of space-borne optical instruments, showing in some cases a nicely developed plasma tail extending from their coma and exhibiting an oscillatory behaviour. Aims. The oscillations of cometary tails may be explained in terms of vortex shedding because of the interaction of the comet with the solar wind streams. Therefore, it is possible to exploit these oscillations in order to infer the value of the Strouhal number S t, which quantifies the vortex shedding phenomenon, and the physical properties of the local medium. Methods. We used the Heliospheric Imager (HI) data of the Solar TErrestrial Relations Observatory (STEREO) mission to study the oscillations of the tails of comets 2P/Encke and C/2012 S1 (ISON) during their perihelion in Nov 2013. We determined the corresponding Strouhal numbers from the estimates of the halo size, the relative speed of the solar wind flow, and the period of the oscillations. Results. We found that the estimated Strouhal numbers are very small, and the typical value of S t ~ 0.2 would be extrapolated for size of the halo larger than ~106 km. Conclusions. Although the vortex shedding phenomenon has not been unambiguously revealed, the findings suggest that some kind of magnetohydrodynamic (MHD) instability process is responsible for the observed behaviour of cometary tails, which can be exploited for probing the physical conditions of the near-Sun region.

scholarly journals Design of the Heliospheric Imager for the STEREO mission

2001 ◽  
Author(s):  
Jean-Marc Defise ◽  
Jean-Philippe Halain ◽  
Emmanuel Mazy ◽  
Pierre P. Rochus ◽  
Russell A. Howard ◽  
...  
Keyword(s):  
Stereo Mission ◽  
Heliospheric Imager

The solar and heliospheric imager (SoloHI) instrument for the solar orbiter mission

2013 ◽  
Author(s):  
Russell A. Howard ◽  
Angelos Vourlidas ◽  
Clarence M. Korendyke ◽  
Simon P. Plunkett ◽  
Michael T. Carter ◽  
...  
Keyword(s):  
Orbiter Mission ◽  
Heliospheric Imager

Using STEREO-HI beacon data to predict CME arrival time and speed with the ELEvoHI model

2020 ◽  
Author(s):  
Maike Bauer ◽  
Tanja Amerstorfer ◽  
Jürgen Hinterreiter ◽  
Christian Möstl ◽  
Jackie A. Davies ◽  
...  
Keyword(s):  
Real Time ◽  
Coronal Mass Ejections ◽  
Arrival Time ◽  
Geomagnetic Storms ◽  
Leading Edge ◽  
Science Data ◽  
Electrical Devices ◽  
Using Data ◽  
Heliospheric Imager

<div> <div> <div> <div> <p>Coronal mass ejections (CMEs) may induce strong geomagnetic storms which have a significant impact on satellites in orbit as well as electrical devices on Earth’s surface. If we want to be able to mitigate the potentially devastating consequences which strong CMEs might have on Earth, developing models which accurately predict their arrival time is an integral step. The Ellipse Evolution model based on Heliospheric Imager observations (ELEvoHl) predicts the arrival of coronal mass ejections using data from STEREO’s HI instruments. HI data is available as high-resolution science data, which is downlinked every few days and low-resolution beacon data, which is downlinked in near real-time. Therefore, to allow for real time predictions of CME arrivals, beacon data must be used. We study different data reduction procedures to improve the quality of the measurements and compile the resulting images into time-elongation plots (J-plots). We track the leading edge of each selected CME event by hand, resulting in a series of time-elongation points which function as input for the ELEvoHI model. We compare the resulting predictions to those obtained using science data in terms of accuracy and errors of the predicted arrival time and speed.</p> </div> </div> </div> </div>

scholarly journals Design and performances of the heliospheric imager for the STEREO mission

2005 ◽  
Author(s):  
Emmanuel Mazy ◽  
Jean-Philippe Halain ◽  
Jean-Marc Defise ◽  
Philippe Ronchain ◽  
Russell A. Howard ◽  
...  
Keyword(s):  
Stereo Mission ◽  
Heliospheric Imager

scholarly journals The radial width of a Coronal Mass Ejection between 0.1 and 0.4 AU estimated from the Heliospheric Imager on STEREO

2009 ◽  
Vol 27 (11) ◽  
pp. 4349-4358 ◽  
Author(s):  
N. P. Savani ◽  
A. P. Rouillard ◽  
J. A. Davies ◽  
M. J. Owens ◽  
R. J. Forsyth ◽  
...  
Keyword(s):  
Cross Section ◽  
Heliocentric Distance ◽  
Circular Cross Section ◽  
Flux Rope ◽  
Field Of View ◽  
Statistical Surveys ◽  
Mass Ejection ◽  
Best Fit ◽  
Heliospheric Imager

Abstract. On 15–17 February 2008, a CME with an approximately circular cross section was tracked through successive images obtained by the Heliospheric Imager (HI) instrument onboard the STEREO-A spacecraft. Reasoning that an idealised flux rope is cylindrical in shape with a circular cross-section, best fit circles are used to determine the radial width of the CME. As part of the process the radial velocity and longitude of propagation are determined by fits to elongation-time maps as 252±5 km/s and 70±5° respectively. With the longitude known, the radial size is calculated from the images, taking projection effects into account. The radial width of the CME, S (AU), obeys a power law with heliocentric distance, R, as the CME travels between 0.1 and 0.4 AU, such that S=0.26 R0.6±0.1. The exponent value obtained is compared to published studies based on statistical surveys of in situ spacecraft observations of ICMEs between 0.3 and 1.0 AU, and general agreement is found. This paper demonstrates the new opportunities provided by HI to track the radial width of CMEs through the previously unobservable zone between the LASCO field of view and Helios in situ measurements.

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