Global Observations of the Interstellar Interaction from the Interstellar Boundary Explorer (IBEX)

McComas, D. J.; Allegrini, F.; Bochsler, P.; Bzowski, M.; Christian, E. R.; Crew, G. B.; Demajistre, R.; Fahr, H. J.; Fichtner, H.; Frisch, P. C.; Funsten, H. O.; Fuselier, S. A.; Gloeckler, G.; Gruntman, M.; Heerikhuisen, J.; Izmodenov, Vladislav; Janzen, P. H.; Knappenberger, P. H.; Krimigis, S. M.; Kucharek, H.; Lee, M.; Livadiotis, G.; Livi, S.; MacDowall, R. J.; Mitchell, D. G.; Möbius, E.; Moore, T. E.; Pogorelov, N. V.; Reisenfeld, D. B.; Roelof, E. C.; Saul, L.; Schwadron, N. A.; Valek, P. W.; Vanderspek, R.; Würz, Peter; Zank, G. P.

doi:10.1126/science.1180906

Cited by 483 publications

(591 citation statements)

References 30 publications

(39 reference statements)

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“…This implies that HSTOF can observe a different dependence on direction of the hydrogen ENA flux than the lower energy instruments INCA (highest energy channel ∼46 keV: Krimigis et al 2009) and IBEX (E ≤ 6 keV: McComas et al 2009) The result is not substantially changed by taking adiabatic acceleration, diffusion and escape processes into account. Our preliminary result (Czechowski et al 2006b), which suggested a strong diffusion effect, was affected by the error in calculating the adiabatic acceleration (see the remark in Sect.…”

Section: Results From the Model: The Ena Fluxesmentioning

confidence: 97%

HSTOF ENA observations and energetic ion distributions in the heliosheath

Czechowski

Hilchenbach

Hsieh

2012

A&A

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Context. Launched in 1996, HSTOF on board SOHO was the first instrument to detect the energetic neutral atoms (ENA) from the heliosheath. After mid 2003, the field of view of HSTOF was restricted to the flank sectors of the heliosheath, in which region the energetic ion distributions are still unknown. Interpretation of these data requires understanding of the energetic ion transport in the inner heliosheath. Aims. We update the HSTOF ENA hydrogen and helium spectra by adding the results from the recent (2006−2010) measurements. We calculate the energetic ion distributions in a numerical model of the heliosheath and use them as a basis for interpreting the HSTOF ENA observations, in particular those of the flank sectors. Methods. The hydrogen and helium ENA spectra were derived from the HSTOF observations of two 90 • -wide ecliptic longitude sectors around the crosswind directions. The energetic ion distributions in the heliosheath were calculated in a simple model of the heliosphere, assuming that the main acceleration occurs at the termination shock. The effects of different processes (charge-exchange loss, adiabatic acceleration, parallel diffusion and escape across the boundary) were determined with different assumptions about the boundary conditions and the transport parameters. The resulting ion distributions were used to calculate the ENA fluxes, which can be compared with the observations by HSTOF and other instruments. Results. The energetic ion density in the flank sectors of the heliosphere is lower than in the forward (upwind) sector. As a result, the contribution of the flanks of the heliosheath to the production of ENA is not directly proportional to the thickness of the heliosheath, but instead is comparable to the contribution of the forward sector, which agrees with the HSTOF data. The HSTOF ENA flux intensity is nevertheless significantly lower than the model calculations. Near the heliopause there appears a region of low energetic ion density caused by the charge-exchange and the escape losses.

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Section: Results From the Model: The Ena Fluxesmentioning

confidence: 97%

HSTOF ENA observations and energetic ion distributions in the heliosheath

Czechowski

Hilchenbach

Hsieh

2012

A&A

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“…Recently, our understanding of the boundaries of the heliosphere and its interaction with the LISM has been expanded by the unexpected results of the Interstellar Boundary EXplorer (IBEX) and the in situ observations by the Voyager spacecraft (Stone et al 2005). Among the findings is the IBEX ribbon (McComas et al 2009), which provides insight into the interstellar magnetic field. Another key component of the interaction is the interstellar flow vector, u LISM , which denotes the relative motion between the Sun and the LISM.…”

Section: Contextmentioning

confidence: 99%

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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“…Details of both statistical smoothing as we apply it to TWINS data and the background suppression procedure are provided in McComas et al [2012, Appendix A]. This technique that produces statistically smoothed images has also been applied successfully to the ENA measurements on IBEX [McComas et al, 2009b].…”

Section: Twins Ena Instrumentsmentioning

confidence: 99%

Evolution of CIR storm on 22 July 2009

et al. 2012

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[1] Global images of ion intensities are deconvolved from TWINS ENA images during the main and recovery phase of a CIR storm on 22 July 2009. The global spatial ion images taken at different times, along with solar wind data, geomagnetic activity indices, geosynchronous orbit observations, and in situ measurements from the THEMIS mission provide a picture of the evolution of the ring current during both the main phase and early recovery phase of the storm. Major features of the evolution are consistent with expectations based upon time dependent geomagnetic indices, e.g., SYM/H and ASY/H, and geosynchronous orbit detection of dipolarizations from GOES 11 and 12. Direct comparisons are made with in situ THEMIS ESA and SST spectral measurements. The peak energy of the ion spectrum in the ring current is seen to decrease in the recovery phase. The time evolution of the ion energy spectra over the range from 2.5 to 97.5 keV at the spatial peaks of the ring current in the inner magnetosphere obtained from ENA images is presented for the first time.

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Global Observations of the Interstellar Interaction from the Interstellar Boundary Explorer (IBEX)

Cited by 483 publications

References 30 publications

HSTOF ENA observations and energetic ion distributions in the heliosheath

HSTOF ENA observations and energetic ion distributions in the heliosheath

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

Evolution of CIR storm on 22 July 2009

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