<i>Interplanetary Dynamical Processes</i>

Parker, E. N.; Marshak, R. E.; Johnson, G. L.

doi:10.1063/1.3051487

Cited by 865 publications

(957 citation statements)

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“…The means and standard deviations of the distributions of magnetic ÿeld strength B, density N , and bulk speed V are 30:5 ± 11:2 nT, 59:8 ± 44:4 cm −3 , and 423 ± 112 km=s, respectively for a period of approximately half a solar cycle. On average, the magnetic ÿeld strength and density in the orbital zone of Mercury are 5 and 10 times that at Earth, respectively, and the speed is the same as that at Earth, consistent with the Parker spiral ÿeld model (Parker, 1963;Slavin and Holzer, 1981). Thus, to extent that the interaction of the solar wind with Mercury depends on B and N , it is 5 -10 times as strong as the interaction of the solar wind with Earth.…”

Section: Radial Variationssupporting

confidence: 52%

Magnetic fields and plasmas in the inner heliosphere: Helios results

Burlaga

2001

Planetary and Space Science

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The magnetic ÿeld of Mercury and the structure and dynamics of Mercury's magnetosphere, which will be studied by the spacecraft orbiting Mercury, are strongly in uenced by the interaction of the solar wind with Mercury. In order to understand the internal magnetic ÿeld, it will be necessary to correct the observations of the external ÿeld for the distortions produced by the solar wind. Understanding of the solar wind interaction with Mercury is essential for understanding the structure and dynamics of the magnetosphere and phenomena such as magnetic storms. Helios 1 and 2 made a number of passes in the region traversed by the orbit of Mercury, and each pass provided a sample of the solar wind environment of Mercury. This paper reviews the plasma and magnetic ÿeld observations from Helios that provide a general basis for interpreting the observations of Mercury that will be made by orbiting spacecraft. The variables that govern the structure and dynamics of the magnetospheres of Mercury and Earth are approximately 5 -10 times larger at Mercury than at Earth. Thus, the solar wind interaction with Mercury will be much stronger than the interaction with Earth. Moreover, the solar wind at Mercury is probably more variable than that at Earth. There is a clear need for measurements of the solar wind during the approach of spacecraft to Mercury and while they are in orbit around Mercury.

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Section: Radial Variationssupporting

confidence: 52%

Magnetic fields and plasmas in the inner heliosphere: Helios results

Burlaga

2001

Planetary and Space Science

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“…It is also evident from the typical velocity of the ejected material that the ensuing motion is highly energetic and non-linear and considerable amount of mass and magnetic field are ejected in the process.Comparing the motion with non-linear gas dynamics, Parker 9 has pointed out that the hydrodynamic blast wave theory can be used successfully to describe the flow due to sudden expansion of solar corona.By using similarity solution method of the hydrodynamic equations he has presented a number of numerical solutions and applied the results to the flow produced by sudden coronal expansion.…”

Section: Etc)mentioning

confidence: 99%

Evolution of Flare Generated Magnetohydrodynamic Shock in Solar Wind

Sharma¹,

Ojha²,

Kumar³

2016

jusps-B

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A self-similar spherically symmetric model is constructed to describe a blast wave in the solar wind produced by a solar flare. The shock wave is assumed to advance into a conducting gas streaming with a constant velocity ahead of the shock. Numerical solutions are obtained for the distribution of flow variables within the shocked gas for the special choice of parameters and for uniform and non-uniform distribution of density in ambient solar atmosphere. In particular, the time of transit of the shock at the earth's orbit is calculated. It is observed that the streaming ambient solar atmosphere reduces variations in flow variables in crossing the shock at earth's orbit.

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“…Fairly simple models can be developed by treating the solar wind from a hydrodynamic point of view, and thus solving the one-dimensional equations of motion along a single field line (e.g. Parker, 1963). The main aim of such models is to obtain accurate expressions for the plasma density, velocity, and especially temperature at 1 AU.…”

Section: Solar Wind Modellingmentioning

confidence: 99%

From the Sun’s atmosphere to the Earth’s atmosphere: an overview of scientific models available for space weather developments

et al. 2002

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Abstract. Space weather aims at setting operational numerical tools in order to nowcast, forecast and quantify the solar activity events, the magnetosphere, ionosphere and thermosphere responses and the consequences on our technological societies. These tools can be divided in two parts. The first has a geophysical base (Sun, interplanetary medium, magnetosphere, atmosphere). The second concerns technological applications (telecommunications, spacecraft orbits, power plants ...). In this paper, we aim at giving an overview of the models that belong to the first class (geophysics) that might serve in the future as a basis for building global operational codes. For each model, we consider the physics underneath, the input and output parameters, and whether it is already operational, whether it may become operational in the near future, or if it is an academic research tool. Relevant references are given in order to serve as a starting point for further readings.

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Interplanetary Dynamical Processes

Cited by 865 publications

References 0 publications

Magnetic fields and plasmas in the inner heliosphere: Helios results

Magnetic fields and plasmas in the inner heliosphere: Helios results

Evolution of Flare Generated Magnetohydrodynamic Shock in Solar Wind

From the Sun’s atmosphere to the Earth’s atmosphere: an overview of scientific models available for space weather developments

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