Studies of interstellar pickup ions in the solar wind

progress report, NASA grant NAGW-2579 to the University of New Hampshire
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National Aeronautics and Space Administration, National Technical Information Service, distributor , [Washington, DC, Springfield, Va
Interstellar gas., Ions., Solar wind., Atmospheric phy
Statementprincipal investigator, Philip A. Isenberg; co-investigators: Martin A. Lee, Eberhard Möbius.
Series[NASA contractor report] -- NASA-CR-202559., NASA contractor report -- NASA CR-202559.
ContributionsLee, Martin A., Möbius, Eberhard., United States. National Aeronautics and Space Administration.
The Physical Object
Pagination1 v.
ID Numbers
Open LibraryOL15507319M

Get this from a library. Studies of interstellar pickup ions in the solar wind: progress report, NASA grant NAGW to the University of New Hampshire. [Philip A Isenberg; Martin A Lee; Eberhard Möbius; United States.

National Aeronautics and Space Administration.]. Data collected by the magnetometer onboard the Ulysses spacecraft are surveyed for the occurrence of waves generated during the pick-up of interstellar hydrogen.

Thirty one wave events were found during a day study period, between Ma and Decem (after the Ulysses encounter with Jupiter). It is found that observation of the waves does not depend on the magnitude of Cited by: Bernstein waves are not commonly discussed in the solar wind literature.

For this reason, our early working premise was that the observed waves were the result of a high-frequency instability described by Gray et al. () whereby newly ionized interstellar pickup. The interaction of interstellar pick-up ions with the solar wind is studied by comparing a model for the velocity distribution function of pick-up ions with actual measurements of He(+) ions in the solar wind.

last 40 years. The interstellar neutral gas flows into the heliosphere, is ionized by solar UV photons and charge-exchange with the solar wind to form interstellar pickup ions (PUIs) and a neutral solar wind.

The PUIs are carried outwards with the solar wind to its termination shock, where their. Caption: The new heliosphere. a, The HP [heliopause] is shown by the yellow surface (case B) defined by a solar wind density of cm −3.

The white lines represent the solar magnetic field. The red lines represent the interstellar magnetic field. b, The standard view of a comet long tail extending thousands of astronomical units.

The interaction of interstellar pick-up ions with the solar wind is studied by comparing a model for the velocity distribution function of pick-up ions with actual measurements of He+ ions in the solar wind.

The model includes the effects of pitch-ang'e diffusion due to interplanetary Alfvén waves, adiabatic deceleration in the expanding solar wind and the radial variation of the source by: We present observations of interstellar pickup hydrogen and helium in the solar wind which show large, highly-correlated fluctuations in flux which are not correlated significantly with the solar-wind hydrogen flux.

The correlation of the fluctuations in the two species implies that the fluctuations are caused by transport after ionization. solar wind ions. Recent observations of pickup ions by the Ulysses spacecraft (e.g.

Gloeckler et al. ) adds to the indirect evidence for this scenario, which by now has be-come quite compelling.

However, one essential element of the process, namely how pickup ions are first injected into the acceleration mechanism, has engendered controversy.

Scientific understanding of the physics of pickup ions, their relation to interstellar atoms and anomalous cosmic rays, and their influence on the solar wind has been advanced almost entirely by Ulysses (and to a lesser extent ACE), and it is the only spacecraft to directly measure neutral interstellar material.

Description Studies of interstellar pickup ions in the solar wind PDF

@article{osti_, title = {INTERSTELLAR PICK-UP IONS OBSERVED BETWEEN 11 AND 22 AU BY NEW HORIZONS}, author = {Randol, B.

and McComas, D. and Schwadron, N. A., E-mail: [email protected]}, abstractNote = {We report new observations by the Solar Wind Around Pluto instrument on the New Horizons spacecraft, which measures energy per charge (E/q) spectra of solar.

The heliosphere in the local interstellar medium: proceedings of the first ISSI Workshop NovemberBern, Switzerland.

Details Studies of interstellar pickup ions in the solar wind PDF

Magnetohydrodynamic Medium.- Voyager Observations of the Magnetic Field, Interstellar Pickup Ions and Solar Wind in the Distant Heliosphere.- \/a>> # The heliosphere in the local interstellar medium. Acceleration of interstellar pickup ions in the disturbed solar wind observed on Ulysses Article (PDF Available) in Journal of Geophysical Research Atmospheres 99(A9) October with 65 Reads.

The solar wind, a continual low-density flux of charged particles, streams outward from the corona and expands supersonically throughout and beyond the solar system.

The solar wind and the interstellar medium interact to create the global heliosphere, shown schematically in Fig. The interaction between the solar wind, flowing radially. Solar wind is an ionized gas made up primarily of protons and electrons with minor ions in amounts similar to those in the corona.

The electrons and ions are very tightly bound to lines of magnetic flux, again like the coronal plasma in streamers. However, the magnetic field in the solar wind is relatively weak and thus is carried along by the solar wind.

Recently also the diffuse x-ray background has received attention as a potentially powerful diagnostic technique for the interstellar gas/solar wind interaction (see, e.g., Cravens, ; Robertson et al., ).

This radiation is produced through the excitation of heavy solar wind ions when they collide with interstellar gas atoms. Included would be studies of solar wind, neutral species, and pickup ions in the interplanetary medium, in situ studies of particle acceleration at the termination shock, which is a model for other astrophysical shocks, studies of the penetration of interstellar gas and dust into the heliosphere, and exploration of the hydrogen wall apparently.

Pickup ions, created by ionization of slow moving atoms and molecules well inside the heliosphere, provide us with a new tool to probe remote regions in and beyond the heliosphere and to study.

The interstellar medium begins where the interplanetary medium of the Solar System ends. The solar wind slows to subsonic velocities at the termination shock, 90– astronomical units from the the region beyond the termination shock, called the heliosheath, interstellar matter interacts with the solar wind.

Voyager 1, the farthest human-made object from the Earth (after Further studies of waves accompanying the solar wind pickup of interstellar hydrogen, ().

Heating of the solar wind by pickup ion driven Alfv•n ion cyclotron instability. Keywords: Interstellar pickup ions, solar wind, turbulence PACS: Vg; Lk. INTRODUCTION The ionization and pickup of inflowing interstellar hydrogen has large-scale effects on the supersonic solar wind [].

The pickup process adds energy and momentum to the wind, resulting in heating and deceleration, which have been observed by the. solar wind alpha particles [Gloeckler et al., ], and rare 3He+ pickup ions. In addition to the interstellar pickup ions, SWICS distributions showed that the majority of the observed C+ and a fraction of the O+ and N+ are produced by an additional “inner source” of neutral atoms located near the Sun [Geiss et al., ].

The inner source.

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A new study reveals that interstellar winds, blown in from the a cloud of gas surrounding the solar system, have changed over the last 40 years. @article{osti_, title = {Pickup ion processes associated with spacecraft thrusters: Implications for solar probe plus}, author = {Clemens, Adam and Burgess, David}, abstractNote = {Chemical thrusters are widely used in spacecraft for attitude control and orbital manoeuvres.

They create an exhaust plume of neutral gas which produces ions via photoionization and charge exchange. studies support the concept of interstellar helium penetration of the solar system.

The techniques include optical (interplanetary glow) and in situ (pickup ions and direct flux detection) measurements [e.g., Moebius et al.,and references therein]. [3] Optical observations and pickup ion measurementsCited by: 4.

The data from these diverse sources shows that the direction of the interstellar wind has changed some 4 to 9 degrees over the last 40 years. “Previously we thought the local interstellar medium was very constant, but these results show that it is highly dynamic, as is the heliosphere’s interaction with it,” said David McComas, IBEX principal investigator at Southwest Research Institute.

11 spacecraft over 4 decades show that the particle wind streaming in to the solar system from interstellar space has changed direction over the last 40 years.

1I/‘Oumuamua is not the first interstellar object ever detected in the solar system per se; it’s the first macroscopic object. Astronomers have previously detected cosmic rays, gas, and ions. The red lines represent the interstellar magnetic field.

b, The standard view of a comet long tail extending thousands of astronomical units. V1 and V2 are shown in this artist rendition; V2 has now passed the HP. The yellow dot represents the Sun. The supersonic solar wind region is represented by the blue region around the Sun. Turbulent heating of the distant solar wind by interstellar pickup protons in a decelarating flow.

Astrophys J., Wang, C., H. Li, J.D. Richardson, J.R. Kan. Interplanetary shock characteristics and associated geosynchronous magnetic field variations estimated from. Interstellar atoms flow past the Earth as the solar system passes through the surrounding interstellar cloud at 23 kilometers per second (50, miles per hour).

The latest IBEX measurements of the interstellar wind direction were found to differ from those made by .Modeling the Time-dependent Solar Wind, Interstellar Pickup Ions, and Turbulence at the Ulysses, Voyager, and New Horizons Spacecraft Using Empirically-derived Boundary Conditions PM - PM: Li, Hui 3D Turbulence with Global Reconnection: PM - PM Fu, Xiangrong: Compressible Turbulence in the Solar Wind near the Sun.The Fluff is held at bay just beyond the edge of the solar system by the sun's magnetic field, which is inflated by solar wind into a magnetic bubble more than 10 billion km wide.

Called the "heliosphere," this bubble acts as a shield that helps protect the inner solar .