Direct observation of He+ pick-up ions of interstellar origin in the solar wind

Möbius, E.; Hovestadt, D.; Klecker, B.; Scholer, M.; Gloeckler, G.; Ipavich, F. M.

doi:10.1038/318426a0

Cited by 389 publications

(224 citation statements)

References 17 publications

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“…Interstellar PUIs are created from interstellar wind neutrals by ionization processes, such as photoionization by EUV radiation, charge-exchange with solar wind protons, and electron impact. PUI were already predicted in the 1970s by Fahr (1971) and subsequently confirmed by observations of the AMPTE spacecraft (Möbius et al 1985). One can easily identify PUIs by their almost exclusive single-charge state and their highly suprathermal velocity distribution function (VDF), which is a consequence of the pickup process.…”

Section: Contextmentioning

confidence: 84%

Challenges in the determination of the interstellar flow longitude from the pickup ion cutoff

Taut

Berger

Möbius

et al. 2018

A&A

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Context. The interstellar flow longitude corresponds to the Sun's direction of movement relative to the local interstellar medium. Thus, it constitutes a fundamental parameter for our understanding of the heliosphere and, in particular, its interaction with its surroundings, which is currently investigated by the Interstellar Boundary EXplorer (IBEX). One possibility to derive this parameter is based on pickup ions (PUIs) that are former neutral ions that have been ionized in the inner heliosphere. The neutrals enter the heliosphere as an interstellar wind from the direction of the Sun's movement against the partially ionized interstellar medium. PUIs carry information about the spatial variation of their neutral parent population (density and flow vector field) in their velocity distribution function. From the symmetry of the longitudinal flow velocity distribution, the interstellar flow longitude can be derived. Aims. The aim of this paper is to identify and eliminate systematic errors that are connected to this approach of measuring the interstellar flow longitude; we want to minimize any systematic influences on the result of this analysis and give a reasonable estimate for the uncertainty. Methods. We use He + data measured by the PLAsma and SupraThermal Ion Composition (PLASTIC) sensor on the Solar TErrestrial RElations Observatory Ahead (STEREO A) spacecraft. We analyze a recent approach, identify sources of systematic errors, and propose solutions to eliminate them. Furthermore, a method is introduced to estimate the error associated with this approach. Additionally, we investigate how the selection of interplanetary magnetic field angles, which is closely connected to the pickup ion velocity distribution function, affects the result for the interstellar flow longitude. Results. We find that the revised analysis used to address part of the expected systematic effects obtains significantly different results than presented in the previous study. In particular, the derived uncertainties are considerably larger. Furthermore, an unexpected systematic trend of the resulting interstellar flow longitude with the selection of interplanetary magnetic field orientation is uncovered.

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Section: Contextmentioning

confidence: 84%

Challenges in the determination of the interstellar flow longitude from the pickup ion cutoff

Taut

Berger

Möbius

et al. 2018

A&A

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“…Because they suddenly find themselves immersed in a rapidily moving magnetized plasma, they behave like pickup ions in the solar wind (Moebius et al, 1985;Gloeckler et al, 1993;Isenberg, 1995). They initially have the form of a monoenergetic ring beam gyrating around the magnetic field.…”

Section: Anisotropy and Non-maxwellian Distributionsmentioning

confidence: 99%

Observational Signatures of Particle Acceleration in Supernova Remnants

Helder¹,

Vink²,

Bykov³

et al. 2012

Particle Acceleration in Cosmic Plasmas

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We evaluate the current status of supernova remnants as the sources of Galactic cosmic rays. We summarize observations of supernova remnants, covering the whole electromagnetic spectrum and describe what these observations tell us about the acceleration processes by high Mach number shock fronts. We discuss the shock modification by cosmic rays, the shape and maximum energy of the cosmic-ray spectrum and the total energy budget of

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“…Pickup He was discovered by Möbius et al (1985). Pickup ions of H, 4 He and 3 He, N, O, Ar, and Ne have now been measured in the inner 5 AU by several different spacecraft, including Ulysses data obtained at all ecliptic latitudes (Möbius et al 1985;Gloeckler and Fisk 2007;. The observed PUI population consists of ions with an interstellar origin, that are mixed with an inner source of PUIs that peaks near the Sun and consists of low-FIP elements (Geiss et al 1995;Schwadron and Gloeckler 2007).…”

Section: Pickup Ions and Anomalous Cosmic Raysmentioning

confidence: 99%

“…3.1). Pickup He was discovered by Möbius et al (1985). Pickup ions of H, 4 He and 3 He, N, O, Ar, and Ne have now been measured in the inner 5 AU by several different spacecraft, including Ulysses data obtained at all ecliptic latitudes (Möbius et al 1985;Gloeckler and Fisk 2007;.…”

Section: Pickup Ions and Anomalous Cosmic Raysmentioning

confidence: 99%

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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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Direct observation of He+ pick-up ions of interstellar origin in the solar wind

Cited by 389 publications

References 17 publications

Challenges in the determination of the interstellar flow longitude from the pickup ion cutoff

Challenges in the determination of the interstellar flow longitude from the pickup ion cutoff

Observational Signatures of Particle Acceleration in Supernova Remnants

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

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