scholarly journals Purple Auroral Rays and Global Pc1 Pulsations Observed at the CIR‐Associated Solar Wind Density Enhancement on 21 March 2017

2018 ◽  
Vol 45 (20) ◽  
Author(s):  
K. Shiokawa ◽  
M. Ozaki ◽  
A. Kadokura ◽  
Y. Endo ◽  
T. Sakanoi ◽  
...  
Keyword(s):  
Solar Wind ◽  
Solar Wind Density ◽  
Density Enhancement ◽  
Pc1 Pulsations

scholarly journals SMEI 3D RECONSTRUCTION OF A CORONAL MASS EJECTION INTERACTING WITH A COROTATING SOLAR WIND DENSITY ENHANCEMENT: THE 2008 APRIL 26 CME

2010 ◽  
Vol 724 (2) ◽  
pp. 829-834 ◽  
Author(s):  
B. V. Jackson ◽  
A. Buffington ◽  
P. P. Hick ◽  
J. M. Clover ◽  
M. M. Bisi ◽  
...  
Keyword(s):  
Solar Wind ◽  
3D Reconstruction ◽  
Coronal Mass Ejection ◽  
Solar Wind Density ◽  
Density Enhancement ◽  
Mass Ejection

scholarly journals Effects of solar wind density on auroral electrojets and brightness under influence of substorms

2009 ◽  
Vol 27 (1) ◽  
pp. 113-119 ◽  
Author(s):  
J.-H. Shue ◽  
Y. Kamide ◽  
J. W. Gjerloev
Keyword(s):  
Solar Wind ◽  
Auroral Oval ◽  
Auroral Electrojet ◽  
The Other ◽  
Auroral Ionosphere ◽  
Stored Energy ◽  
Solar Wind Density ◽  
The Earth ◽  
Density Enhancement ◽  
Solar Wind Parameters

Abstract. Using the auroral electrojet indices and Polar Ultraviolet Imager auroral images, we examined two fortuitous events during which the solar wind density had clear enhancements while the other solar wind parameters were relatively constant. Two electrojet enhancements were found in each event. The first electrojet enhancement was likely to be related to a substorm in which an auroral bulge appeared at premidnight. The second electrojet enhancement was driven by the density enhancement in the solar wind. The auroral oval became wider in latitude and the auroral distribution became dispersed after the density enhancement arrived at the Earth. The total auroral power integrated over the entire nightside region from 50 to 80° MLAT, however, did not increase significantly in response to the density enhancement. Our interpretation is that the substorm that occurred prior to the solar wind density enhancement had drained out a significant portion of the stored energy in the magnetotail; therefore, less precipitation energy was deposited into the auroral ionosphere by the density enhancement.

Large-scale solar wind density enhancement and its boundaries: Helios 1, 2 and IMP 8 observations

2008 ◽  
Vol 56 (3-4) ◽  
pp. 398-405 ◽  
Author(s):  
P.A. Dalin ◽  
Yu.I. Yermolaev ◽  
G.N. Zastenker ◽  
M.O. Riazantseva
Keyword(s):  
Solar Wind ◽  
Large Scale ◽  
Solar Wind Density ◽  
Density Enhancement

scholarly journals Sun-Earth connection event of super geomagnetic storm on 2001 March 31: the importance of solar wind density

2020 ◽  
Vol 20 (3) ◽  
pp. 036 ◽  
Author(s):  
Li-Bin Cheng ◽  
Gui-Ming Le ◽  
Ming-Xian Zhao
Keyword(s):  
Solar Wind ◽  
Geomagnetic Storm ◽  
Solar Wind Density ◽  
Earth Connection

Response of the inner and outer magnetosphere to solar wind density fluctuations during the recovery phase of a moderate magnetic storm

2007 ◽  
Vol 69 (14) ◽  
pp. 1707-1722 ◽  
Author(s):  
N. Zolotukhina ◽  
V. Pilipenko ◽  
M.J. Engebretson ◽  
A.S. Rodger
Keyword(s):  
Solar Wind ◽  
Magnetic Storm ◽  
Recovery Phase ◽  
Density Fluctuations ◽  
Solar Wind Density ◽  
Outer Magnetosphere

MHD simulations of magnetospheric response to a strong solar wind density pulse

2021 ◽  
Author(s):  
Andrey Samsonov ◽  
Jennifer A. Carter ◽  
Graziella Branduardi-Raymont ◽  
Steven Sembay
Keyword(s):  
Solar Wind ◽  
Dynamic Pressure ◽  
Solar Wind Density ◽  
Ionospheric Currents ◽  
X Ray ◽  
Interplanetary Coronal Mass Ejection ◽  
Explorer Mission ◽  
The One ◽  
Mass Ejection ◽  
Present Simulation

<p>On 16-17 June 2012, an interplanetary coronal mass ejection with an extremely high solar wind density (~100 cm<sup>-3</sup>) and mostly strong northward (or eastward) interplanetary magnetic field (IMF) interacted with the Earth’s magnetosphere. We have simulated this event using global MHD models. We study the magnetospheric response to two solar wind discontinuities. The first is characterized by a fast drop of the solar wind dynamic pressure resulting in rapid magnetospheric expansion. The second is a northward IMF turning which causes reconfiguration of the magnetospheric-ionospheric currents. We discuss variations of the magnetopause position and locations of the magnetopause reconnection in response to the solar wind variations. In the second part of our presentation, we present simulation results for the forthcoming SMILE (Solar wind Magnetosphere Ionosphere Link Explorer) mission. SMILE is scheduled for launch in 2024. We produce two-dimensional images that derive from the MHD results of the expected X-ray emission as observed by the SMILE Soft X-ray Imager (SXI). We discuss how SMILE observations may help to study events like the one presented in this work.</p>

Deriving CME volume and density from remote sensing data

2021 ◽  
Author(s):  
Manuela Temmer ◽  
Lukas Holzknecht ◽  
Mateja Dumbovic ◽  
Bojan Vrsnak ◽  
Nishtha Sachdeva ◽  
...  
Keyword(s):  
Solar Wind ◽  
Solar Wind Speed ◽  
Remote Sensing Data ◽  
Propagation Speed ◽  
Solar Wind Density ◽  
Sheath Region ◽  
Pile Up ◽  
Mass Ejection ◽  
Interplanetary Propagation

<p>Using combined STEREO-SOHO white-light data, we present a method to determine the volume and density of a coronal mass ejection (CME) by applying the graduated cylindrical shell model (GCS) and deprojected mass derivation. Under the assumption that the CME  mass is roughly equally distributed within a specific volume, we expand the CME self-similarly and calculate the CME density for distances close to the Sun (15–30 Rs) and at 1 AU. The procedure is applied on a sample of 29 well-observed CMEs and compared to their interplanetary counterparts (ICMEs). Specific trends are derived comparing calculated and in-situ measured proton densities at 1 AU, though large uncertainties are revealed due to the unknown mass and geometry evolution: i) a moderate correlation for the magnetic structure having a mass that stays rather constant and ii) a weak correlation for the sheath density by assuming the sheath region is an extra mass - as expected for a mass pile-up process - that is in its amount comparable to the initial CME deprojected mass. High correlations are derived between in-situ measured sheath density and the solar wind density and solar wind speed as measured 24 hours ahead of the arrival of the disturbance. This gives additional confirmation that the sheath-plasma indeed stems from piled-up solar wind material. While the CME interplanetary propagation speed is not related to the sheath density, the size of the CME may play some role in how much material is piled up.</p>

A neural network-based mid-term prognosis of geomagnetic storms that uses pre-storm effects related to current sheets and magnetic islands

2021 ◽  
Author(s):  
Mikhail Fridman
Keyword(s):  
Solar Wind ◽  
Solar Minimum ◽  
High Speed ◽  
Geomagnetic Storms ◽  
Magnetic Islands ◽  
Solar Wind Density ◽  
Short Term ◽  
Storm Effects ◽  
Term Forecast ◽  
Advance Time

<p>Mid-term prognoses of geomagnetic storms require an improvement since theу are known to have rather low accuracy which does not exceed 40% in solar minimum. We claim that the problem lies in the approach. Current mid-term forecasts are typically built using the same paradigm as short-term ones and suggest an analysis of the solar wind conditions typical for geomagnetic storms. According to this approach, there is a 20-60 minute delay between the arrival of a geoeffective flow/stream to L1 and the arrival of the signal from the spacecraft to Earth, which gives a necessary advance time for a short-term prognosis. For the mid-term forecast with an advance time from 3 hours to 3 days, this is not enough. Therefore, we have suggested finding precursors of geomagnetic storms observed in the solar wind. Such precursors are variations in the solar wind density and the interplanetary magnetic field in the ULF range associated with crossings of magnetic cavities in front of the arriving geoeffective high-speed streams and flows (Khabarova et al., 2015, 2016, 2018; Adhikari et al., 2019). Despite some preliminary studies have shown that this might be a perspective way to create a mid-term prognosis (Khabarova 2007; Khabarova & Yermolaev, 2007), the problem of automatization of the prognosis remained unsolved.</p>

scholarly journals Solar wind density model from km-wave type III bursts

Solar Physics ◽  
1973 ◽  
Vol 29 (1) ◽  
pp. 197-209 ◽  
Author(s):  
Hector Alvarez ◽  
F. T. Haddock
Keyword(s):  
Solar Wind ◽  
Density Model ◽  
Solar Wind Density ◽  
Wave Type ◽  
Type Iii
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