scholarly journals A slow mode transition region adjoining the front boundary of a magnetic cloud as a relic of a convected solar wind feature: Observations and MHD simulation

2008 ◽  
Vol 113 (A9) ◽  
pp. n/a-n/a ◽  
Author(s):  
Charles J. Farrugia ◽  
Nikolai V. Erkaev ◽  
Ulrich Taubenschuss ◽  
Vladimir A. Shaidurov ◽  
Charles W. Smith ◽  
...  
Keyword(s):  
Solar Wind ◽  
Transition Region ◽  
Magnetic Cloud ◽  
Mode Transition ◽  
Slow Mode ◽  
Mhd Simulation ◽  
Front Boundary

scholarly journals Full compressible 3D MHD simulation of solar wind

2020 ◽  
Vol 500 (4) ◽  
pp. 4779-4787
Author(s):  
Takuma Matsumoto
Keyword(s):  
Solar Wind ◽  
Transition Region ◽  
Solar Physics ◽  
Mass Loss Rate ◽  
Three Dimensional ◽  
Lower Atmosphere ◽  
Fast Solar Wind ◽  
Solar Mass ◽  
Mhd Simulation ◽  
Driving Mechanisms

ABSTRACT Identifying the heating mechanisms of the solar corona and the driving mechanisms of solar wind are key challenges in understanding solar physics. A full three-dimensional compressible magnetohydrodynamic (MHD) simulation was conducted to distinguish between the heating mechanisms in the fast solar wind above the open field region. Our simulation describes the evolution of the Alfvénic waves, which includes the compressible effects from the photosphere to the heliospheric distance s of 27 solar radii (R⊙). The hot corona and fast solar wind were reproduced simultaneously due to the dissipation of the Alfvén waves. The inclusion of the transition region and lower atmosphere enabled us to derive the solar mass-loss rate for the first time by performing a full three-dimensional compressible MHD simulation. The Alfvén turbulence was determined to be the dominant heating mechanism in the solar wind acceleration region (s > 1.3 R⊙), as suggested by previous solar wind models. In addition, shock formation and phase mixing are important below the lower transition region (s < 1.03 R⊙) as well.

The comet/solar wind transition region at Giacobini-Zinner

1986 ◽  
Vol 13 (4) ◽  
pp. 393-396 ◽  
Author(s):  
M. F. Thomsen ◽  
S. J. Bame ◽  
W. C. Feldman ◽  
J. T. Gosling ◽  
D. J. McComas ◽  
...  
Keyword(s):  
Solar Wind ◽  
Transition Region

Slow mode transition in the frontside magnetosheath

1992 ◽  
Vol 97 (A6) ◽  
pp. 8295 ◽  
Author(s):  
P. Song ◽  
C. T. Russell ◽  
M. F. Thomsen
Keyword(s):  
Mode Transition ◽  
Slow Mode

An overview of the impact of the January 10-11 1997 magnetic cloud on the magnetosphere via global MHD simulation

1998 ◽  
Vol 25 (14) ◽  
pp. 2537-2540 ◽  
Author(s):  
C. C. Goodrich ◽  
J. G. Lyon ◽  
M. Wiltberger ◽  
R. E. Lopez ◽  
K. Papadopoulos
Keyword(s):  
Magnetic Cloud ◽  
Mhd Simulation ◽  
Global Mhd Simulation ◽  
The Impact

scholarly journals Radial variation of solar wind electrons inside a magnetic cloud observed at 1 and 5 AU

2000 ◽  
Vol 105 (A12) ◽  
pp. 27269-27275 ◽  
Author(s):  
R. M. Skoug ◽  
W. C. Feldman ◽  
J. T. Gosling ◽  
D. J. McComas ◽  
D. B. Reisenfeld ◽  
...  
Keyword(s):  
Solar Wind ◽  
Magnetic Cloud ◽  
Radial Variation

Ionospheric Power Consumption in Global MHD Simulation Predicted From Solar Wind Measurements

2004 ◽  
Vol 32 (4) ◽  
pp. 1511-1518 ◽  
Author(s):  
M. Palmroth ◽  
H.E.J. Koskinen ◽  
T.I. Pulkkinen ◽  
P. Janhunen
Keyword(s):  
Solar Wind ◽  
Power Consumption ◽  
Mhd Simulation ◽  
Wind Measurements ◽  
Global Mhd Simulation

What can Hall-MHD simulations tell us about the transition region in the solar wind proton density spectrum?

2020 ◽  
Author(s):  
Victor Montagud-Camps ◽  
František Němec ◽  
Jana Šafránková ◽  
Zdeněk Němeček ◽  
Roland Grappin ◽  
...  
Keyword(s):  
Solar Wind ◽  
Transition Region ◽  
Spectral Index ◽  
Density Fluctuations ◽  
Power Density Spectrum ◽  
Proton Density ◽  
Density Spectrum ◽  
Significant Difference ◽  
Field Fluctuations ◽  
Hall Mhd

<p>Similarly to the power density spectrum of magnetic field fluctuations in the solar wind, the spectrum of density fluctuations also shows multiple spectral slopes. Both of them present a spectral index varying between –3/2 and –5/3 in the inertial range and close to –2.8 between the proton and electron gyrofrequencies.</p><p>Despite these similarities, the spectrum of density fluctuations has a significant difference with respect to the magnetic and velocity fluctuations spectra: it shows a transition region between the inertial and the kinetic ranges with spectral index typically around –1.</p><p>We have combined the results of compressible Hall-MHD numerical simulations and measurements of the BMSW instrument onboard Spektr-R satellite to study the possible causes of the flattening in the density spectrum. Both numerical and experimental approaches point towards an important role played by Kinetic Alfvén Waves.</p>

ESTABLISHING THE ORIENTATION OF SHOCK WAVE PLANE OF SOLAR WIND MAGNETIC CLOUD FOR CONCLUSIONS ABOUT THE LEVEL OF AURORAL SUBSTORM ACTIVITY

2019 ◽  
Vol 17 (1) ◽  
pp. 195-202 ◽  
Author(s):  
N. A. Barkhatov ◽  
S. E. Revunov ◽  
M. V. Mukhina ◽  
M. L. Gruzdeva ◽  
O. T. Cherney ◽  
...  
Keyword(s):  
Shock Wave ◽  
Solar Wind ◽  
Magnetic Cloud ◽  
Auroral Substorm ◽  
Substorm Activity
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