The Effects of a κ‐Distribution in the Heliosheath on the Global Heliosphere and ENA Flux at 1 AU

Heerikhuisen, J.; Pogorelov, N. V.; Florinski, V.; Zank, G. P.; Roux, J. A. le

doi:10.1086/588248

Cited by 163 publications

(135 citation statements)

References 49 publications

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“…Consequently, we present a first modeling attempt to explore how the quasi-stationary suprathermal PUI distribution function in the solar wind evolves with increasing heliocentric distance when assuming the model and whether that results in the values of about 1.6 to 2.0 typically used for simulations of the outer heliosphere [Heerikhuisen et al, 2008;Opher et al, 2013;Zirnstein et al, 2014].…”

Section: 1002/2014ja020431mentioning

confidence: 99%

“…Within the line of our approach we chose the distribution and obtain, using the auxiliary function g (r) defined in (2), and get from (11), see, e.g., Gradshteyn and Ryzhik [2007]:…”

Section: The Case 0 < ≠mentioning

confidence: 99%

“…Motivated by this and by the finding that distributions have been found to be reasonable approximations not only in the supersonic solar wind [e.g., Scudder, 1996;Leubner, 2004;Pierrard and Lazar, 2010] but also in the heliosheath [Heerikhuisen et al, 2008;Opher et al, 2013;Zirnstein et al, 2014], we investigate-starting from a phase space transport equation like the one used by Fahr and Fichtner [2011] and specifying the velocity distribution as a function-whether one can derive a differential equation describing the evolution of the parameter with heliocentric distance.…”

Section: Introductionmentioning

confidence: 99%

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On the radial evolution of κ distributions of pickup protons in the supersonic solar wind

2014

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It is well known that (pickup) ions in the inner heliosphere do not maintain Maxwellian distributions but tend to nonequilibrium distributions with extended suprathermal tails. Such states have been classified as quasi-equilibria which in many cases can well be described by so-called distributions. With the present study we start out from a phase space transport equation for pickup ions in the inner heliosphere that adequately describes the most important processes such as injection, convection, cooling, and diffusion in velocity space. Assuming that the underlying distribution functions are distributions, we proceed from this transport equation to a second-order moment, i.e., pressure equation which represents an ordinary differential equation for the parameter as function of heliocentric distance. This strategy allows one to describe the transition from an initial Vasyliunas-Siscoe distribution to distributions with gradually more pronounced suprathermal tails. While the velocity dependence of the velocity diffusion coefficient determines the systematic reduction of the parameter , the latter always has the (formal) asymptotic value ∞ = 3∕2. This translates into values of 1.5 ≤ TS ≤ 2.2 in the upstream region of the (upwind) solar wind termination shock that defines the outer validity range of the model.

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Section: 1002/2014ja020431mentioning

confidence: 99%

“…Within the line of our approach we chose the distribution and obtain, using the auxiliary function g (r) defined in (2), and get from (11), see, e.g., Gradshteyn and Ryzhik [2007]:…”

Section: The Case 0 < ≠mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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On the radial evolution of κ distributions of pickup protons in the supersonic solar wind

2014

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“…Christon 1987;Collier and Hamilton 1995;Grabbe 2000;Mauk et al 2004;Schippers et al 2008;Dialynas et al 2009;Ogasawara et al 2013), outer heliosphere and inner heliosheath (e.g. Decker and Krimigis 2003;Decker et al 2005;Heerikhuisen et al 2008;Zank et al 2010;Livadiotis et al 2011Livadiotis et al , 2013, and other general plasma analyses (e.g. Milovanov …”

Section: Introductionmentioning

confidence: 99%

Electrostatic shielding in plasmas and the physical meaning of the Debye length

Livadiotis

McComas

2014

J. Plasma Phys.

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This paper examines the electrostatic shielding in plasmas, and resolves inconsistencies about what the Debye length really is. Two different interpretations of the Debye length are currently used: (1) The potential energy approximately equals the thermal energy, and (2) the ratio of the shielded to the unshielded potential drops to 1/e. We examine these two interpretations of the Debye length for equilibrium plasmas described by the Boltzmann distribution, and non-equilibrium plasmas (e.g. space plasmas) described by kappa distributions. We study three dimensionalities of the electrostatic potential: 1-D potential of linear symmetry for planar charge density, 2-D potential of cylindrical symmetry for linear charge density, and 3-D potential of spherical symmetry for a point charge. We resolve critical inconsistencies of the two interpretations, including: independence of the Debye length on the dimensionality; requirement for small charge perturbations that is equivalent to weakly coupled plasmas; correlations between ions and electrons; existence of temperature for nonequilibrium plasmas; and isotropic Debye shielding. We introduce a third Debye length interpretation that naturally emerges from the second statistical moment of the particle position distribution; this is analogous to the kinetic definition of temperature, which is the second statistical moment of the velocity distribution. Finally, we compare the three interpretations, identifying what information is required for theoretical/experimental plasma-physics research: Interpretation 1 applies only to kappa distributions; Interpretation 2 is not restricted to any specific form of the ion/electron distributions, but these forms have to be known; Interpretation 3 needs only the second statistical moment of the positional distribution.

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“…from the Loop I superbubble), and essentially unabsorbed X-ray emission from the 10 6 K tenuous, ∼0.005 cm −3 , LB plasma (e.g. Snowden et al 2000;Henley et al 2007), with some foreground contamination from the heliosphere (Sect. 4.2).…”

Section: Interstellar Radiation Field and The Heliospherementioning

confidence: 99%

The Galactic Environment of the Sun: Interstellar Material Inside and Outside of the Heliosphere

et al. 2009

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Interstellar material (ISMa) is observed both inside and outside of the heliosphere. Relating these diverse sets of ISMa data provides a richer understanding of both the interstellar medium and the heliosphere. The galactic environment of the Sun is dominated by warm, low-density, partially ionized interstellar material consisting of atoms and dust grains. The properties of the heliosphere are dependent on the pressure, composition, radiation field, ionization, and magnetic field of ambient ISMa. The very low-density interior of the Local Bubble, combined with an expanding superbubble shell associated with star formation in the Scorpius-Centaurus Association, dominate the properties of the local interstellar medium (LISM). Once the heliosphere boundaries and interaction mechanisms are understood, interstellar gas, dust, pickup ions, and anomalous cosmic rays inside of the heliosphere can be directly compared to ISMa outside of the heliosphere. Our understanding of ISMa at the Sun is further enriched when the circumheliospheric interstellar material is compared to observations of other nearby ISMa and the overall context of our galactic environment. The IBEX mission will map the interaction region between the heliosphere and ISMa, and improve the accuracy of comparisons between ISMa inside and outside the heliosphere.

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The Effects of a κ‐Distribution in the Heliosheath on the Global Heliosphere and ENA Flux at 1 AU

Cited by 163 publications

References 49 publications

On the radial evolution of κ distributions of pickup protons in the supersonic solar wind

On the radial evolution of κ distributions of pickup protons in the supersonic solar wind

Electrostatic shielding in plasmas and the physical meaning of the Debye length

The Galactic Environment of the Sun: Interstellar Material Inside and Outside of the Heliosphere

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