Tracking a major interplanetary disturbance with SMEI

2004 ◽  
Vol 31 (2) ◽  
Author(s):  
S. J. Tappin ◽  
A. Buffington ◽  
M. P. Cooke ◽  
C. J. Eyles ◽  
P. P. Hick ◽  
...  
Keyword(s):  
Interplanetary Disturbance

Solar wind temperature–velocity relationship over the last five solar cycles and Forbush decreases associated with different types of interplanetary disturbance

2020 ◽  
Vol 500 (3) ◽  
pp. 2786-2797
Author(s):  
A A Melkumyan ◽  
A V Belov ◽  
M A Abunina ◽  
A A Abunin ◽  
E A Eroshenko ◽  
...  
Keyword(s):  
Solar Wind ◽  
High Speed ◽  
Coronal Holes ◽  
Cosmic Ray ◽  
Magnetic Clouds ◽  
Solar Cycles ◽  
Forbush Decreases ◽  
Proton Temperature ◽  
Interaction Regions ◽  
Interplanetary Disturbance

ABSTRACT The behaviour of the solar wind (SW) proton temperature and velocity and their relationship during Forbush decreases (FDs) associated with various types of solar source – coronal mass ejections (CMEs) and coronal holes (CHs) – have been studied. Analysis of cosmic ray variations, SW temperature, velocity, density, plasma beta, and magnetic field (from 1965–2019) is carried out using three databases: the OMNI database, Variations of Cosmic Rays database (IZMIRAN) and Forbush Effects & Interplanetary Disturbances database (IZMIRAN). Comparison of the observed SW temperature (T) and velocity (V) for the undisturbed SW allows us to derive a formula for the expected SW temperature (Texp, the temperature given by a T–V formula, if V is the observed SW speed). The results reveal a power-law T–V dependence with a steeper slope for low speeds (V < 425 km s−1, exponent = 3.29 ± 0.02) and flatter slope for high speeds (V > 425 km s−1, exponent = 2.25 ± 0.02). A study of changes in the T–V dependence over the last five solar cycles finds that this dependence varies with solar activity. The calculated temperature index KT = T/Texp can be used as an indicator of interplanetary and solar sources of FDs. It usually has abnormally large values in interaction regions of different-speed SW streams and abnormally low values inside magnetic clouds (MCs). The results obtained help us to identify the different kinds of interplanetary disturbance: interplanetary CMEs, sheaths, MCs, corotating interaction regions, high-speed streams from CHs, and mixed events.

scholarly journals Formation of a strong southward IMF near the solar maximum of cycle 23

2004 ◽  
Vol 22 (2) ◽  
pp. 673-687 ◽  
Author(s):  
S. Watari ◽  
M. Vandas ◽  
T. Watanabe
Keyword(s):  
Solar Wind ◽  
Magnetic Fields ◽  
Geomagnetic Storms ◽  
Solar Maximum ◽  
Interplanetary Shocks ◽  
Physical Processes ◽  
Interplanetary Magnetic Fields ◽  
Interplanetary Physics ◽  
Solar Wind Parameters ◽  
Interplanetary Disturbance

Abstract. We analyzed observations of the solar activities and the solar wind parameters associated with large geomagnetic storms near the maximum of solar cycle 23. This analysis showed that strong southward interplanetary magnetic fields (IMFs), formed through interaction between an interplanetary disturbance, and background solar wind or between interplanetary disturbances are an important factor in the occurrence of intense geomagnetic storms. Based on our analysis, we seek to improve our understanding of the physical processes in which large negative Bz's are created which will lead to improving predictions of space weather. Key words. Interplanetary physics (Flare and stream dynamics; Interplanetary magnetic fields; Interplanetary shocks)

Tracking a major interplanetary disturbance

1983 ◽  
Vol 31 (10) ◽  
pp. 1171-1176 ◽  
Author(s):  
S.J. Tappin ◽  
A. Hewish ◽  
G.R. Gapper
Keyword(s):  
Interplanetary Disturbance

Powerful non-geoeffective interplanetary disturbance of July 2012 observed by muon hodoscope URAGAN

2015 ◽  
Vol 56 (12) ◽  
pp. 2833-2838 ◽  
Author(s):  
I.I. Astapov ◽  
N.S. Barbashina ◽  
A.A. Petrukhin ◽  
V.V. Shutenko ◽  
I.S. Veselovsky
Keyword(s):  
Muon Hodoscope ◽  
Interplanetary Disturbance

The source and propagation of the interplanetary disturbance associated with the full-halo coronal mass ejection on 28 October 2003

2007 ◽  
Vol 112 (A5) ◽  
pp. n/a-n/a ◽  
Author(s):  
Munetoshi Tokumaru ◽  
Masayoshi Kojima ◽  
Ken’ichi Fujiki ◽  
Masahiro Yamashita ◽  
Bernard V. Jackson
Keyword(s):  
Coronal Mass Ejection ◽  
Halo Coronal Mass Ejection ◽  
Mass Ejection ◽  
Interplanetary Disturbance

scholarly journals Coronal Mass Ejections travel time

2016 ◽  
Vol 12 (S328) ◽  
pp. 218-220
Author(s):  
Carlos Roberto Braga ◽  
Rafael Rodrigues Souza de Mendonça ◽  
Alisson Dal Lago ◽  
Ezequiel Echer
Keyword(s):  
Travel Time ◽  
Coronal Mass Ejections ◽  
Geomagnetic Storms ◽  
Time Of Arrival ◽  
Lagrangian Point ◽  
Expansion Speed ◽  
Interplanetary Disturbance

AbstractCoronal mass ejections (CMEs) are the main source of intense geomagnetic storms when they are earthward directed. Studying their travel time is a key-point to understand when the disturbance will be observed at Earth. In this work, we study the CME that originated the interplanetary disturbance observed on 2013/10/02. According to the observations, the CME that caused the interplanetary disturbance was ejected on 2013/09/29. We obtained the CME speed and estimate of the time of arrival at the Lagrangian Point L1 using the concept of expansion speed. We found that observed and estimated times of arrival of the shock differ between 2 and 23 hours depending on method used to estimate the radial speed.

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