Gasdynamics of the solar wind interaction with the interstellar medium

Баранов, В. Б.

doi:10.1007/bf00704240

Cited by 136 publications

(99 citation statements)

References 30 publications

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“…Interstellar plasma and neutral gas are efficiently coupled in the heliospheric interface through charge exchange, which modifies the properties of the inflowing interstellar atoms [Wallis, 1975;Ripken and Fahr, 1983;Baranov andMalama, 1993, 1995 The plasma-gas coupling also determines the extension of the heliospheric tail. The lack of direct experimental data limits our ability to validate the concepts of particle acceleration at, and the nature of, the termination shock.…”

Section: Heliospheric Interfacementioning

confidence: 99%

“…If the concept of the solar wind termination by a shock is correct, then there is a region containing hot (shocked) decelerated (subsonic) plasma beyond the termination shock. The properties of the postshock plasma would strongly depend on the nature of the shock, i.e., whether the shock is predominantly gasdynamical and strong [e.g., Baranov, 1990] Solar wind momentum flux is •50% higher over the sun's poles than near the ecliptic plane. Therefore the termination shock would likely be a factor of •1.2 farther away over the Sun's poles compared to the ecliptic at the same angle from the upwind direction.…”

Section: Termination Shockmentioning

confidence: 99%

“…We demonstrate the main features and potential of hellosphere imaging in the ENA fluxes using a two-shock gasdynamical model [Baranov andMalama, 1993, 1995;Baranov et al, 1998]. The two-shock (Baranov) model assumes that both the interstellar plasma flow and the solar wind plasma flow are supersonic.…”

Section: Modelmentioning

confidence: 99%

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Energetic neutral atom imaging of the heliospheric boundary region

Gruntman¹,

Roelof²,

Mitchell³

et al. 2001

J. Geophys. Res.

131

124

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Abstract. Energetic neutral atom (ENA) imaging is a powerful technique, which can remotely probe the properties of distant hot plasmas. Hot plasmas are abundant at the heliospheric boundary, the region where the expanding solar wind meets the surrounding local interstellar cloud. Here we present a new concept for imaging this boundary in ENA fluxes. Heliospheric ENAs are born from charge exchange between energetic protons and the background interstellar atomic hydrogen gas. The technique is ideal for studying the asymmetric threedimensional heliospheric interface region remotely, from 1 AU. We show that ENA imaging in the 0.2-6 keV energy range will establish the nature of the telTnination shock and properties of hot proton populations in the heliosheath. We also examine how the evolution of pickup proton populations at and beyond the shock can be explored. Global heliosphere ENA images will distinguish among the competing models of the interaction between the Sun and the local interstellar medium, and they will reveal the physics of important processes in the interface region. Heliospheric ENA fluxes are exceptionally weak, which makes imaging implementation difficult. Nonetheless, we show how single-pixel ENA sensors can image the heliosphere from a spicming spacecraft on a typical mission near 1 AU. The required instrumentation is briefly discussed. HeliosphereThe interaction of the expanding solar wind plasma and local interstellar medium (

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Section: Heliospheric Interfacementioning

confidence: 99%

Section: Termination Shockmentioning

confidence: 99%

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Energetic neutral atom imaging of the heliospheric boundary region

Gruntman¹,

Roelof²,

Mitchell³

et al. 2001

J. Geophys. Res.

131

124

View full text Add to dashboard Cite

show abstract

“…Although mass loading plays an important role in the dynamics of the solar wind (Baranov et al 1971;Baranov 1990;Zank 1999), there are a number of key differences between this scenario and the pulsar wind scenario. Firstly, the velocity of the Sun through the ISM is, most likely, weakly sub-fast magnetosonic (McComas et al 2012), whereas the pulsar's motion is highly supersonic; secondly, the pulsar wind is very light -composed of lepton pairs -and one would therefore expect mass loading to have a greater effect; thirdly, most of the research related to mass loading in the solar wind concen- trated on flow in the head region, while we are interested in the large scale dynamics of the tail flows.…”

Section: Introductionmentioning

confidence: 99%

Mass loading of bow shock pulsar wind nebulae

Morlino

Lyutikov

Vorster

2015

Mon. Not. R. Astron. Soc.

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We investigate the dynamics of bow shock nebulae created by pulsars moving supersonically through a partially ionized interstellar medium. A fraction of interstellar neutral hydrogen atoms penetrating into the tail region of a pulsar wind will undergo photo-ionization due to the UV light emitted by the nebula, with the resulting mass loading dramatically changing the flow dynamics of the light leptonic pulsar wind. Using a quasi 1-D hydrodynamic model of both non-relativistic and relativistic flow, and focusing on scales much larger than the stand-off distance, we find that if a relatively small density of neutral hydrogen, as low as 10 −4 cm −3 , penetrate inside the pulsar wind, this is sufficient to strongly affect the tail flow. Mass loading leads to the fast expansion of the pulsar wind tail, making the tail flow intrinsically non-stationary. The shapes predicted for the bow shock nebulae compare well with observations, both in Hα and X-rays.

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“…Therefore the models of the boundary region can be divided roughly according to number of interfaces; namely we have one-shock and two-shock models. A self-consistent gasdynamic model consisting of two shocks and heliopause (tangential discontinuity) was constructed in a series of papers by Baranov (1990), Baranov andMalama (1993, 1995) taking also into account the VLISM neutral particles. These authors solved Boltzmann's equation for the neutral component on the basis of a Monte Carlo approach and found a considerable enhancement in the hydrogen density at the heliopause in the region of the nose.…”

Section: T H E S T R U C T U R E Of T H E Heliospherementioning

confidence: 99%

Large-Scale Structure and Termination of the Heliosphere

Macek

1998

Highlights astron.

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A b s t r a c t . The question of the boundaries of the heliosphere is considered. The termination heliospheric shock should exist because the solar wind plasma flowing supersonically away from the Sun must make a transition to a subsonic flow. The heliopause is at the outermost extend of the solar wind. Beyond the heliopause lies the (very local) interstellar wind. Intensity of radio emissions at 2 to 3 kHz detected by the Voyager plasma wave instrument in the outer heliosphere can be explained provided that the electron beams generating Langmuir waves exist in the postshock plasma due to secondary shocks in the compressed solar wind beyond the termination shock. The field strengths of Langmuir waves required to generate the second harmonic emissions are 50 -100 pN m _ 1 . Alternatively, the emissions are generated in the vicinity of the heliopause. The Voyager 1 and 2 are proceeding toward a likely source region for Langmuir wave and these waves may be observed in situ in the near future. IntroductionSince the 1960's it is known that besides electromagnetic radiation, the Sun also radiates charged particles forming a solar wind. If our solar system moved freely in an empty interstellar space, the solar wind would expand to infinity. Because that is obviously not the case, it is believed that the heliosphere is a finite region of space dominated by the solar wind. Owing to mass conservation, the particle number density of the expanding solar wind should decrease inversely as the square of the distance r from the Sun. The solar wind density already falls below the expected density of the ionized component of the very local inter-stellar medium (VLISM) beyond Saturn's orbit. As a result the heliosphere forms a cavity in the ambient VLISM plasma (Parker, 1963;Axford, 1973;Fahr it al., 1986;Suess, 1990). The "nose" of the cavity is located approximately in the solar equatorial plane and is aligned with the apex, i.e., the "head-on" direction of the VLISM velocity. In the down-stream direction of the VLISM the heliosphere is thought to trail into a long comet-like tail. In spite of its asymmetry the cavity is still called the heliosphere; in fact, only near its nose can it be well approximated by a sphere.As the solar wind expands, the temperature of electrons and ions is reduced and the flow becomes progressively more and more supersonic, reaching the sonic Mach number of about 40 and the Alfv'enic Mach number of ~10 in the outer heliosphere (Belcher et al, 1993). The inner (termination) heliospheric shock exists because the solar wind must make a transition to a subsonic flow as it runs into the plasma of the VLISM. The heliospheric boundary region is sketched in Figure 1. The heliopause is at the outermost extend of the solar wind. Beyond the heliopause lies the interstellar wind. In this review we only consider some aspects of the physics of the heliospheric boundaries and apologize for incomplete references in this field of research. Physics, Woodbury, New York (1996) as well as to Proceedings of the first IS...

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Gasdynamics of the solar wind interaction with the interstellar medium

Cited by 136 publications

References 30 publications

Energetic neutral atom imaging of the heliospheric boundary region

Energetic neutral atom imaging of the heliospheric boundary region

Mass loading of bow shock pulsar wind nebulae

Large-Scale Structure and Termination of the Heliosphere

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