scholarly journals Solar Wind Composition Associated with the Solar Activity

10.5772/35508 ◽  
2012 ◽  
Author(s):  
X. Wang ◽  
B. Klecker ◽  
P. Wurz
Keyword(s):  
Solar Wind ◽  
Solar Activity ◽  
Solar Wind Composition

Apollo 11 and 12 solar wind composition experiments: Fluxes of He and Ne isotopes

1970 ◽  
Vol 75 (31) ◽  
pp. 5972-5979 ◽  
Author(s):  
J. Geiss ◽  
P. Eberhardt ◽  
F. Bühler ◽  
J. Meister ◽  
P. Signer
Keyword(s):  
Solar Wind ◽  
Solar Wind Composition

What Magnetospheric Workers Should Know about Solar Wind Composition

1983 ◽  
pp. 73-98 ◽  
Author(s):  
S. J. Bame ◽  
W. C. Feldman ◽  
J. T. Gosling ◽  
D. T. Young ◽  
R. D. Zwickl
Keyword(s):  
Solar Wind ◽  
Solar Wind Composition

Long-term cosmic ray/solar activity hysteresis phenomenon and properties of solar wind for the last 200 years

1999 ◽  
Author(s):  
L. I. Dorman ◽  
G. Villoresi ◽  
I. V. Dorman ◽  
N. Iucci ◽  
M. Parisi
Keyword(s):  
Solar Wind ◽  
Solar Activity ◽  
Cosmic Ray ◽  
Hysteresis Phenomenon

scholarly journals Commission 49: Interplanetary Plasma and Heliosphere: (Plasma Interplanetaire et Heliosphere)

2000 ◽  
Vol 24 (1) ◽  
pp. 77-84
Author(s):  
F. Verheest ◽  
M. Vandas ◽  
B. Buti ◽  
N.F. Cramer ◽  
M. Dryer ◽  
...  
Keyword(s):  
Solar Wind ◽  
Gas Flow ◽  
Recent Literature ◽  
Interplanetary Space ◽  
Charged Dust ◽  
Interstellar Gas ◽  
Interplanetary Plasma ◽  
Flow Through ◽  
Transient Events ◽  
Solar Wind Composition

In the last decade the triennial reports from Commission 49 have covered various topics like (nonlinear) plasma processes, magnetohydrodynamic phenomena and flows in the heliosphere, solar wind composition, transient events in, and latitudinal dependencies of, the heliosphere, interstellar gas flow through the interface region, kinetic versus magnetohydrodynamic theory in heliospheric plasmas and charged dust in space plasmas. Continuing the tradition of summarizing specific aspects to give astronomers outside our own specialty a flavour of our field, we now address recent advances in understanding coronal mass ejections in interplanetary space and the inner heliospheric solar wind under quiet and perturbed conditions. We owe a great debt of gratitude to the eminent contributors for their valiant efforts in writing these succinct but clear reports and guiding us through the recent literature.

scholarly journals Breathing of heliospheric structures triggered by the solar-cycle activity

2003 ◽  
Vol 21 (6) ◽  
pp. 1303-1313 ◽  
Author(s):  
K. Scherer ◽  
H. J. Fahr
Keyword(s):  
Solar Wind ◽  
Solar Activity ◽  
Solar Cycle ◽  
Activity Cycle ◽  
Periodic Variation ◽  
Galactic Cosmic Rays ◽  
Activity Period ◽  
Solar Cycles ◽  
Interplanetary Physics ◽  
Ram Pressure

Abstract. Solar wind ram pressure variations occuring within the solar activity cycle are communicated to the outer heliosphere as complicated time-variabilities, but repeating its typical form with the activity period of about 11 years. At outer heliospheric regions, the main surviving solar cycle feature is a periodic variation of the solar wind dynamical pressure or momentum flow, as clearly recognized by observations of the VOYAGER-1/2 space probes. This long-periodic variation of the solar wind dynamical pressure is modeled here through application of appropriately time-dependent inner boundary conditions within our multifluid code to describe the solar wind – interstellar medium interaction. As we can show, it takes several solar cycles until the heliospheric structures adapt to an average location about which they carry out a periodic breathing, however, lagged in phase with respect to the solar cycle. The dynamically active heliosphere behaves differently from a static heliosphere and especially shows a historic hysteresis in the sense that the shock structures move out to larger distances than explained by the average ram pressure. Obviously, additional energies are pumped into the heliosheath by means of density and pressure waves which are excited. These waves travel outwards through the interface from the termination shock towards the bow shock. Depending on longitude, the heliospheric sheath region memorizes 2–3 (upwind) and up to 6–7 (downwind) preceding solar activity cycles, i.e. the cycle-induced waves need corresponding travel times for the passage over the heliosheath. Within our multifluid code we also adequately describe the solar cycle variations in the energy distributions of anomalous and galactic cosmic rays, respectively. According to these results the distribution of these high energetic species cannot be correctly described on the basis of the actually prevailing solar wind conditions.Key words. Interplanetary physics (heliopause and solar wind termination; general or miscellaneous) – Space plasma physics (experimental and mathematical techniques)

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