On the model of the solar wind-interstellar medium interaction with two shock waves

1976 ◽  
Vol 41 (2) ◽  
pp. 481-490 ◽  
Author(s):  
V. B. Baranov ◽  
K. V. Krasnobaev ◽  
M. S. Ruderman
Keyword(s):  
Solar Wind ◽  
Shock Waves ◽  
Interstellar Medium

Gasdynamic models of the solar wind/interstellar medium interaction

1994 ◽  
Vol 21 (4) ◽  
pp. 245-248 ◽  
Author(s):  
R. S. Steinolfson ◽  
V. J. Pizzo ◽  
T. Holzer
Keyword(s):  
Solar Wind ◽  
Interstellar Medium

Energy deposition in the solar wind by flare-generated shock waves

1968 ◽  
Vol 73 (15) ◽  
pp. 4875-4881 ◽  
Author(s):  
Murray Dryer ◽  
Donald L. Jones
Keyword(s):  
Solar Wind ◽  
Shock Waves ◽  
Energy Deposition

scholarly journals Element Abundances of Solar Energetic Particles and the Photosphere, the Corona, and the Solar Wind

Atoms ◽  
2019 ◽  
Vol 7 (4) ◽  
pp. 104 ◽  
Author(s):  
Donald V. Reames
Keyword(s):  
Solar Wind ◽  
Shock Waves ◽  
Solar Corona ◽  
Plasma Temperature ◽  
Energetic Particles ◽  
Solar Energetic Particles ◽  
Charge Ratio ◽  
Ambient Plasma ◽  
Element Abundances ◽  
Resonant Wave

From a turbulent history, the study of the abundances of elements in solar energetic particles (SEPs) has grown into an extensive field that probes the solar corona and physical processes of SEP acceleration and transport. Underlying SEPs are the abundances of the solar corona, which differ from photospheric abundances as a function of the first ionization potentials (FIPs) of the elements. The FIP-dependence of SEPs also differs from that of the solar wind; each has a different magnetic environment, where low-FIP ions and high-FIP neutral atoms rise toward the corona. Two major sources generate SEPs: The small “impulsive” SEP events are associated with magnetic reconnection in solar jets that produce 1000-fold enhancements from H to Pb as a function of mass-to-charge ratio A/Q, and also 1000-fold enhancements in 3He/4He that are produced by resonant wave-particle interactions. In large “gradual” events, SEPs are accelerated at shock waves that are driven out from the Sun by wide, fast coronal mass ejections (CMEs). A/Q dependence of ion transport allows us to estimate Q and hence the source plasma temperature T. Weaker shock waves favor the reacceleration of suprathermal ions accumulated from earlier impulsive SEP events, along with protons from the ambient plasma. In strong shocks, the ambient plasma dominates. Ions from impulsive sources have T ≈ 3 MK; those from ambient coronal plasma have T = 1 – 2 MK. These FIP- and A/Q-dependences explore complex new interactions in the corona and in SEP sources.

Interaction of the solar wind with the local interstellar medium: A multifluid approach

1996 ◽  
Vol 101 (A10) ◽  
pp. 21639-21655 ◽  
Author(s):  
G. P. Zank ◽  
H. L. Pauls ◽  
L. L. Williams ◽  
D. T. Hall
Keyword(s):  
Solar Wind ◽  
Interstellar Medium ◽  
Local Interstellar Medium

Requirements and design of a dual, thermal ion-electron instrument for an outer heliosphere and interstellar mission

2020 ◽  
Author(s):  
Benoit Lavraud ◽  
Andrei Fedorov ◽  
Michel Blanc ◽  
Robert Wimmer-Schweingruber ◽  
Qiugang Zong ◽  
...  
Keyword(s):  
Solar Wind ◽  
Interstellar Medium ◽  
Large Range ◽  
Signal To Noise Ratio ◽  
Limited Resources ◽  
High Signal ◽  
Signal To Noise ◽  
Outer Heliosphere ◽  
The Us ◽  
Scientific Rationale

<p>We present the scientific rationale, and ensuing requirements, for the measurement of thermal ions and electrons in the solar wind (including pick-up ions), the inner and outer heliosphere, and the interstellar medium. We place these in the context of the interstellar missions being currently designed in the US and China. From these requirements, we propose an instrument concept that permits to measure both thermal ions (without composition) and electrons, alternatively, with low resources and high signal-to-noise ratio in accordance with the limited resources and large range of count rates, as expected over the course of such a mission.</p>

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