The interstellar boundary explorer (IBEX): Update at the end of phase B

McComas, D. J.; Allegrini, F.; Bartolone, L.; Bochsler, P.; Bzowski, M.; Collier, M. R.; Fahr, H. J.; Fichtner, H.; Frisch, P. C.; Funsten, H. O.; Fuselier, S. A.; Gloeckler, G.; Gruntman, M.; Izmodenov, V.; Knappenberger, P. H.; Lee, M.; Livi, S.; Mitchell, D. G.; Möbius, E.; Moore, T. E.; Pope, S.; Reisenfeld, D. B.; Roelof, E. C.; Runge, Howard; Scherrer, J.; Schwadron, N. A.; Tyler, Robert T.; Wieser, Martin; Witte, M.; Würz, Peter; Zank, G. P.

doi:10.1063/1.2359334

Cited by 17 publications

(18 citation statements)

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“…[15] Maximum instrument background per energy channel is on the order of 10 À2 counts/s, significantly lower than the average expected count rate [McComas et al, 2006]. Included in this calculation are ENAs produced from charge-exchange of ions with outgassing neutrals from the spacecraft, charge-exchange of heliospheric pickup ions with these neutrals, and secondary ions generated in the entrance subsystem.…”

Section: Methodsmentioning

confidence: 99%

“…[2] The Interstellar Boundary Explorer (IBEX), scheduled for launch in 2008, is designed to make the first global images of the heliosheath beyond the heliospheric termination shock, using energetic neutral atoms (ENAs) generated by charge exchange between downstream protons and interstellar hydrogen atoms [McComas et al, 2004[McComas et al, , 2006. These ENAs are no longer bound to the magnetic field and therefore follow trajectories determined only by the gravitational force and radiation pressure from the Sun.…”

Section: Introductionmentioning

confidence: 99%

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Implications of solar wind suprathermal tails for IBEX ENA images of the heliosheath

et al. 2008

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[1] Decades of interplanetary measurements of the solar wind and other space plasmas have established that the suprathermal ion intensity distributions (j) are non-Maxwellian and are characterized by high-energy power law tails (j $ E Àk ). Recent analysis by Fisk and Gloeckler of suprathermal ion observations between 1-5 AU demonstrates that a particular differential intensity distribution function emerges universally between $2-10 times the solar wind speed with k $ 1.5. This power law tail is particularly apparent in downstream distributions beyond reverse shocks associated with corotating interaction regions. Similar power law tails have been observed in the downstream flow beyond the termination shock by the Low Energy Charged Particle instrument on both Voyager 1 and Voyager 2. Using kappa distributions with internal energy, density, and bulk flow derived from large-scale magnetohydrodynamic models, we calculate the simulated flux of energetic neutral atoms (ENAs) produced in the heliosheath by charge exchange between solar wind protons and interstellar hydrogen. We then produce simulated ENA maps of the heliosheath, such as will be measured by the Interstellar Boundary Explorer Mission (IBEX). We also estimate the expected signal to noise and background ratio for IBEX. The solar wind suprathermal tail significantly increases the ENA flux within the IBEX energy range, $0.01-6 keV, by more than an order of magnitude at the highest energies over the estimates using a Maxwellian. It is therefore essential to consider suprathermal tails in the interpretation of IBEX ENA images and theoretical modeling of the heliospheric termination shock.

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Section: Methodsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Implications of solar wind suprathermal tails for IBEX ENA images of the heliosheath

et al. 2008

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“…This population, however tenuous it is, is important for the reasons of diagnostics of both heliospheric heliosheath and of the inner sheaths of astrospheres, because it can be observed spectroscopically (Linsky and Wood 1996;Wood et al 2007). It is also the main target of observations by IBEX (McComas et al 2004a(McComas et al , 2005(McComas et al , 2006. The atoms created by charge exchange inherit the local parameters of the plasma; owing to their relatively large speed they are able to penetrate close to the Sun with few losses, carrying the information on the conditions in their birth places.…”

Section: Hydrogenmentioning

confidence: 99%

“…While the heliospheric boundaries are Fig. 7 Schematic diagram of an equatorial cut through the termination shock taken from McComas and Schwadron (2006). The Archimedean spiral flux tubes first cross the termination shock near the nose and their connection points move back along the flanks of the shock as they continue to propagate out through the heliosheath.…”

Section: Anomalous Cosmic Rays and Heliospheric Asymmetriesmentioning

confidence: 99%

“…The two Voyager spacecraft provide in situ data on both solar wind and interstellar particle populations in the inner heliosheath regions. The IBEX mission (McComas et al 2004a(McComas et al , 2005(McComas et al , 2006(McComas et al , 2009, will add to these data by mapping the interaction between interstellar neutrals and the solar wind using observations of energetic neutral atoms (ENAs) with energies of 10 eV-6 keV, formed from charge exchange between H • and H + . The ENA data will constrain the filtration of interstellar neutrals entering the heliosphere.…”

Section: Introductionmentioning

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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Low‐Energy Lunar Trajectory Design

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The interstellar boundary explorer (IBEX): Update at the end of phase B

Cited by 17 publications

References 8 publications

Implications of solar wind suprathermal tails for IBEX ENA images of the heliosheath

Implications of solar wind suprathermal tails for IBEX ENA images of the heliosheath

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

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