Global properties of the solar wind. I - The invariance of the momentum flux density

1980 ◽  
Vol 241 ◽  
pp. 417 ◽  
Author(s):  
R. Steinitz ◽  
M. Eyni
Keyword(s):  
Solar Wind ◽  
Flux Density ◽  
Momentum Flux ◽  
Global Properties

Determination of the solar wind angular momentum flux from the HELIOS data - an observational test of the Weber and Davis theory

1983 ◽  
Vol 271 ◽  
pp. 335 ◽  
Author(s):  
V. Pizzo ◽  
R. Schwenn ◽  
E. Marsch ◽  
H. Rosenbauer ◽  
K.-H. Muehlhaeuser ◽  
...  
Keyword(s):  
Solar Wind ◽  
Angular Momentum ◽  
Momentum Flux ◽  
Observational Test

scholarly journals Solar cycle dependence of scaling in solar wind fluctuations

2008 ◽  
Vol 15 (3) ◽  
pp. 445-455 ◽  
Author(s):  
S. C. Chapman ◽  
B. Hnat ◽  
K. Kiyani
Keyword(s):  
Solar Wind ◽  
Solar Cycle ◽  
Momentum Flux ◽  
Magnetic Fluctuations ◽  
Mhd Turbulence ◽  
Scaling Properties ◽  
Two Component ◽  
Energy And Momentum ◽  
Cycle Dependence

Abstract. In this review we collate recent results for the statistical scaling properties of fluctuations in the solar wind with a view to synthesizing two descriptions: that of evolving MHD turbulence and that of a scaling signature of coronal origin that passively propagates with the solar wind. The scenario that emerges is that of coexistent signatures which map onto the well known "two component" picture of solar wind magnetic fluctuations. This highlights the need to consider quantities which track Alfvénic fluctuations, and energy and momentum flux densities to obtain a complete description of solar wind fluctuations.

Correlations for the Choked Mass and Momentum Flux Density Considering Real-Gas Thermodynamics

2019 ◽  
Vol 141 (8) ◽  
Author(s):  
Matthias Banholzer ◽  
Michael Pfitzner
Keyword(s):  
Flux Density ◽  
Mass Flux ◽  
Momentum Flux ◽  
Second Phase ◽  
Cfd Simulations ◽  
Choked Flow ◽  
Saturation Properties ◽  
Isentropic Flow ◽  
Computational Fluid Dynamics Cfd ◽  
Reduced Pressures

The choked mass flux density and the choked momentum flux density for the nonideal fluids methane and nitrogen have been calculated using the Soave–Redlich–Kwong equation of state (EoS). For the computation a steady, one-dimensional (1D), isenthalpic and isentropic flow is assumed. The developed algorithm for the calculation of the choked flow properties includes a bounded multidimensional Newton method. A possible second phase emerging in the critical nozzle area is excluded using the saturation properties of the considered fluids. The critical ratios of pressure, density, temperature, and speed of sound are discussed and compared to other publications. Formulations of the choked mass flux density and the choked momentum flux density explicit in Tr, pr, and Zr are given valid for different reduced pressures and temperatures depending on the fluid. Additional computational fluid dynamics (CFD) simulations are carried out in order to validate the findings of the algorithm and the proposed correlations.

Solar wind mass and momentum flux variations at 0.3 AU

1994 ◽  
Vol 14 (4) ◽  
pp. 135-138 ◽  
Author(s):  
P. Hick ◽  
B.V. Jackson
Keyword(s):  
Solar Wind ◽  
Momentum Flux

scholarly journals The solar wind angular-momentum flux observed during Solar Orbiter's first orbit

2021 ◽  
Author(s):  
Daniel Verscharen ◽  
David Stansby ◽  
Adam Finley ◽  
Christopher Owen ◽  
Timothy Horbury ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Angular Momentum ◽  
Momentum Flux ◽  
Large Scale ◽  
Magnetic Field Data ◽  
Proton Data ◽  
Scale Properties ◽  
Orbiter Mission

<p>The Solar Orbiter mission is currently in its cruise phase, during which the spacecraft's in-situ instrumentation measures the solar wind and the electromagnetic fields at different heliocentric distances. </p><p>We evaluate the solar wind angular-momentum flux by combining proton data from the Solar Wind Analyser (SWA) Proton-Alpha Sensor (PAS) and magnetic-field data from the Magnetometer (MAG) instruments on board Solar Orbiter during its first orbit. This allows us to evaluate the angular momentum in the protons in addition to that stored in magnetic-field stresses, and compare these to previous observations from other spacecraft. We discuss the statistical properties of the angular-momentum flux and its dependence on solar-wind properties. </p><p>Our results largely agree with previous measurements of the solar wind’s angular-momentum flux in the inner heliosphere and demonstrate the potential for future detailed studies of large-scale properties of the solar wind with the data from Solar Orbiter.</p>

scholarly journals Solar wind, mass and momentum losses during the solar cycle

2010 ◽  
Vol 6 (S271) ◽  
pp. 395-396
Author(s):  
R. Pinto ◽  
S. Brun ◽  
L. Jouve ◽  
R. Grappin
Keyword(s):  
Solar Wind ◽  
Solar Cycle ◽  
Wind Speed ◽  
Mass Flux ◽  
Solar Minimum ◽  
Momentum Flux ◽  
Loss Rate ◽  
Convection Zone ◽  
Mass Loss Rate ◽  
Good Agreement

AbstractWe study the connections between the sun's convection zone evolution and the dynamics of the solar wind and corona. We input the magnetic fields generated by a 2.5D axisymmetric kinematic dynamo code (STELEM) into a 2.5D axisymmetric coronal MHD code (DIP). The computations were carried out for an 11 year cycle. We show that the solar wind's velocity and mass flux vary in latitude and in time in good agreement with the well known time-latitude assymptotic wind speed diagram. Overall sun's mass loss rate, momentum flux and magnetic breaking torque are maximal near the solar minimum.

Momentum flux invariance in the solar wind

1983 ◽  
Vol 272 ◽  
pp. 325 ◽  
Author(s):  
D. J. Mullan
Keyword(s):  
Solar Wind ◽  
Momentum Flux

Understanding our global heliosphere with UV observations: Unique opportunities on Interstellar Probe

2020 ◽  
Author(s):  
Elena Provornikova ◽  
Pontus Brandt ◽  
Ed Roelof ◽  
Olga Katushkina ◽  
Igor Baliukin ◽  
...  
Keyword(s):  
Solar Wind ◽  
Interstellar Medium ◽  
Plasma Properties ◽  
Outer Heliosphere ◽  
New Horizons ◽  
Global Properties ◽  
Observation Strategy ◽  
Local Interstellar Cloud ◽  
First Time ◽  
Interstellar Probe

<p class="p1">Solar Lyman-a emission re-radiated from H atoms incoming to the heliosphere from interstellar medium is a powerful tool to probe globally plasma properties both at the heliosphere boundary and near the Sun. H Lyman-α line profiles reflect velocity distributions of low energy H atoms in the heliosphere which hold information about the plasma near the heliopause. H Lyman α intensities as observed at 1 AU serve as diagnostic of global properties of the solar wind. In this talk we will review what we have learned about the global heliospheric interaction from H Lyman-a observations from inside the heliosphere on SWAN/SOHO, Voyages/UVS and New Horizons/Alice missions. Outward trajectory of Interstellar Probe going through the outer heliosphere to the interstellar medium (ISM) up to 1000 AU enable unique science opportunities to explore global interaction between the solar wind and local ISM by observing for the first time Lyman-a emission from outside of the heliosphere. We will report a progress of UV working group in outlining primary science questions on the nature of the global heliosphere and Local Interstellar Cloud, planning observation strategy, measurement requirements and synergies with planetary UV observations for potential KBO fly-by.</p>

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