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>

Revisiting the Strongest Martian X-Ray Halo Observed by XMM-Newton on 2003 November 19–21

2020 ◽  
Author(s):  
Limei Yan ◽  
Jiawei Gao ◽  
Lihui Chai ◽  
Lingling Zhao ◽  
Zhaojin Rong ◽  
...  
Keyword(s):  
Solar Wind ◽  
Solar Cycle ◽  
Direct Evidence ◽  
Dynamic Pressure ◽  
Mars Global Surveyor ◽  
Propagation Models ◽  
X Ray ◽  
Interplanetary Coronal Mass Ejection ◽  
Solar Cycle 23 ◽  
Mass Ejection

<p>On 2003 November 20–21, when the most intense geomagnetic storm during solar cycle 23 was observed at Earth, XMM-Newton recorded the strongest Martian X-ray halo hitherto. The strongest Martian X-ray halo has been suggested to be caused by the unusual solar wind, but no direct evidence has been given in previous studies. Here, based on the Mars Global Surveyor (MGS) observations, unambiguous evidence of unusual solar wind impact during that XMM-Newton observation was found: the whole induced magnetosphere of Mars was highly compressed. The comparison between the solar wind dynamic pressure estimated at Mars from MGS observation and that predicted by different solar wind propagation models suggests that the unusal solar wind is probably related to the interplanetary coronal mass ejection observed at Earth on 2003 November 20.</p>

scholarly journals Photospheric magnetic field of an eroded-by-solar-wind coronal mass ejection

2016 ◽  
Vol 12 (S327) ◽  
pp. 67-70
Author(s):  
J. Palacios ◽  
C. Cid ◽  
E. Saiz ◽  
A. Guerrero
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Coronal Mass Ejection ◽  
Coronal Hole ◽  
Interplanetary Medium ◽  
Flux Rope ◽  
Magnetic Characteristics ◽  
Interplanetary Coronal Mass Ejection ◽  
Fast Wind ◽  
Mass Ejection

AbstractWe have investigated the case of a coronal mass ejection that was eroded by the fast wind of a coronal hole in the interplanetary medium. When a solar ejection takes place close to a coronal hole, the flux rope magnetic topology of the coronal mass ejection (CME) may become misshapen at 1 AU as a result of the interaction. Detailed analysis of this event reveals erosion of the interplanetary coronal mass ejection (ICME) magnetic field. In this communication, we study the photospheric magnetic roots of the coronal hole and the coronal mass ejection area with HMI/SDO magnetograms to define their magnetic characteristics.

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>

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 Sonification of Astronomical Data

2011 ◽  
Vol 7 (S285) ◽  
pp. 133-136 ◽  
Author(s):  
Wanda L. Diaz-Merced ◽  
Robert M. Candey ◽  
Nancy Brickhouse ◽  
Matthew Schneps ◽  
John C. Mannone ◽  
...  
Keyword(s):  
Solar Wind ◽  
Time Series Data ◽  
Solar Wind Plasma ◽  
Series Data ◽  
Astronomical Data ◽  
X Ray ◽  
The Earth ◽  
Polar Type ◽  
Mass Ejection ◽  
The Impact

AbstractThis document presents Java-based software called xSonify that uses a sonification technique (the adaptation of sound to convey information) to promote discovery in astronomical data. The prototype is designed to analyze two-dimensional data, such as time-series data. We demonstrate the utility of the sonification technique with examples applied to X-ray astronomy and solar data. We have identified frequencies in the Chandra X-Ray observations of EX Hya, a cataclysmic variable of the intermediate polar type. In another example we study the impact of a major solar flare, with its associated coronal mass ejection (CME), on the solar wind plasma (in particular the solar wind between the Sun and the Earth), and the Earth's magnetosphere.

scholarly journals NEW INSIGHTS INTO SOLAR WIND IMPLANTED VOLATILES FOR LUNAR REGOLITH CHARACTERIZATION: A SIMULATION BASED APPROACH

2018 ◽  
Vol IV-4 ◽  
pp. 199-206
Author(s):  
S. Shukla ◽  
S. Majumdar ◽  
A. Maiti ◽  
S. Kumar
Keyword(s):  
Activation Energy ◽  
Solar Wind ◽  
Frequency Domain ◽  
Particle Density ◽  
Lunar Regolith ◽  
Lunar Soil ◽  
Crystal Defects ◽  
Mining Sites ◽  
Interplanetary Coronal Mass Ejection ◽  
Mass Ejection

<p><strong>Abstract.</strong> The effect of solar wind implanted volatiles into the top 100 nm of the lunar regolith plays a significant role in quantitatively assessing the lunar surface isotopic composition. In essence, these volatiles can either quickly sputter out of the surface or be retained. The implantation processes exhibit a functional dependency on the surface temperature, ilmenite abundance and the activation energy associated with the optical maturity of the lunar soil. The prime focus of this study is to simulate the implication of these incident volatiles in characterizing the regolith for a better insight into the modeling of lunar exosphere during both Interplanetary Coronal Mass Ejection (ICME) and usual cases. Additionally, the proposed model quantifies the total lunar oxygen repository along with determining the associated textural and frequency domain measures for probable future lunar <sup>3</sup>He mining sites. In this 30-day simulation, the particles bombard the reconstructed lunar grid wherein each cell displays varying particle density at a given local time. Moreover, both the activation energy and TiO<sub>2</sub> content are assumed to be in a Gaussian distribution having (&amp;mu;, &amp;sigma;) of (0.96, 0.025) and (12.52, 3.44) respectively. It has been found that the surfaces characterized by high activation energy tend to retain solar wind implants due to the large numbers of crystal defects. However, for H and heavy trace ions, intermediate activation energy range demonstrates diurnal behavior with the diffusive loss at local noon time. The study also finds an intriguing relationship between the lunar O<sub>2</sub> and retained H sites (frequency domain). Furthermore, this could be utilized as a generic exospheric modeling paradigm for airless bodies and contribute to the understanding of the physical processes associated with solar astronomy.</p>

Dusk side clockwise vortex generation and aurora intensity decrease after Solar Wind Dynamic Pressure Decrease

2021 ◽  
Author(s):  
Jinyan Zhao ◽  
Quanqi Shi ◽  
Anmin Tian ◽  
Ruilong Guo ◽  
Xiao-Chen Shen
Keyword(s):  
Solar Wind ◽  
Pressure Pulse ◽  
Dynamic Pressure ◽  
Simulation Method ◽  
Solar Wind Dynamic Pressure ◽  
Ionospheric Currents ◽  
The Earth ◽  
Sudden Decrease ◽  
Pulse Arrival ◽  
Observation Results

&lt;p&gt;A solar wind dynamic pressure increase/decrease leads to the compression/expansion of the Earth&amp;#8217;s magnetosphere. In response, field-aligned currents, which are carried by precipitating or escaping plasma particles, are generated in the magnetosphere and in lead to variations in the auroral intensity. In this study, we investigate magnetospheric and ionospheric responses (including magnetospheric plasma vortex, ionospheric currents and aurorae) to a sudden decrease in solar wind dynamic pressure (SW P&lt;sub&gt;dyn&lt;/sub&gt;), which is critical for further understanding of the solar wind-magnetosphere-ionosphere coupling. We focused on a SW P&lt;sub&gt;dyn&lt;/sub&gt; decrease event that monitored by OMNI. A counter-clockwise plasma vortex was generated in the dusk side magnetosphere uncovered by using MHD simulation method and a clockwise equivalent ionospheric currents (EIC) vortex was generated in the dusk side ionosphere within about ten minutes after the pressure pulse arrival. Simultaneously, the observation results of Spherical Elementary Currents (SECs) showed that the EIC vortex region is dominated by downward field-aligned currents and the ground-based All-Sky Imager (ASI) observations in the vicinity of this EIC vortex showed that the aurorae diminished. These observations are consistent with the scenario proposed by Shi et al. (2014) that flow vortices in the magnetosphere generated by SW P&lt;sub&gt;dyn&lt;/sub&gt; sudden decrease carry downward field-aligned currents into the dusk side ionosphere, generating ionospheric current vortex and thereby modulating auroral activity on the dusk side.&lt;/p&gt;

Is the relation between the solar wind dynamic pressure and the magnetopause standoff distance so simple?

2020 ◽  
Author(s):  
Andrey Samsonov ◽  
Graziella Branduardi-Raymont
Keyword(s):  
Solar Wind ◽  
Dynamic Pressure ◽  
Simple Relation ◽  
Solar Wind Dynamic Pressure ◽  
Standoff Distance ◽  
Solar Wind Density ◽  
Pressure Balance ◽  
Velocity Increase ◽  
The Earth ◽  
Parameter Density

&lt;p&gt;The relation between the solar wind dynamic pressure and magnetopause standoff distance is usually supposed to be R&lt;sub&gt;SUB&lt;/sub&gt;~P&lt;sub&gt;d&lt;/sub&gt;&lt;sup&gt;-1/N&lt;/sup&gt;. The simple pressure balance condition gives N=6, however N varies in empirical magnetopause models from 4.8 to 7.7. Using several MHD models, we simulate the magnetospheric response to increases in the dynamic pressure by varying separately the solar wind density or the velocity. We obtain different values of N depending on which parameter, density or velocity, has been varied and for which IMF orientation. The changes in the standoff distance are smaller (higher N) for a density increase and greater (smaller N) for a velocity increase for southward IMF. We explain this result by enhancement of the Region 1 current that moves the magnetopause closer to the Earth for a high solar wind velocity. We suggest for developers of new empirical magnetopause models in the future to replace the simple relation between R&lt;sub&gt;SUB&lt;/sub&gt; and P&lt;sub&gt;d&lt;/sub&gt; with a fixed N by a more complicated relation which would separate inputs in the dynamic pressure from the density and velocity taking into account the IMF orientation.&lt;/p&gt;

Multi-point observations of a reconnection outflow associated with interacting flux ropes in the solar wind

2020 ◽  
Author(s):  
Zoltan Vörös ◽  
Emiliya Yordanova ◽  
Owen Roberts ◽  
Yasuhito Narita
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Flow Shear ◽  
Magnetic Flux Ropes ◽  
Interplanetary Coronal Mass Ejection ◽  
Flux Ropes ◽  
Magnetic Field Magnitude ◽  
Field Fluctuations ◽  
Mass Ejection ◽  
The Magnetic Field

&lt;p&gt;Twisted magnetic flux ropes embedded in an interplanetary coronal mass ejection (ICME) often contain oppositely oriented magnetic fields and potentially reconnecting current sheets. Reconnection outflows in the solar wind can be identified through magnetic field and plasma signatures, for example, through decreasing magnetic field magnitude, enhanced bulk velocity, temperature and (anti)correlated rotations of the magnetic field and plasma velocity. We investigate a reconnection outflow observed by ACE, WIND and Geotail spacecraft within the interaction region of two flux ropes embedded into an ICME. The SOHO spacecraft, located 15 RE upstream, 120 RE in GSE Y and 5 RE in GSE Z direction from the ACE spacecraft, does not see any plasma signatures of the reconnection outflow. At the same time the other spacecraft, also separated by more than 200 RE in X and Y GSE directions, observe strong plasma and magnetic field fluctuations at the border of the exhaust. &amp;#160;The fluctuations could be associated with Kelvin-Helmholtz (KH) instability at the border of the reconnection outflow with strong flow shear.&amp;#160; It is speculated that the KH instability driven fluctuations and dissipation is responsible for stopping the reconnection outflow which is therefore not seen by SOHO.&lt;/p&gt;

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