DETERMINATION OF INTERSTELLAR He PARAMETERS USING FIVE YEARS OF DATA FROM THE
                    <i>IBEX</i>
                    : BEYOND CLOSED FORM APPROXIMATIONS

Schwadron, N. A.; Möbius, E.; Leonard, T.; Fuselier, S. A.; McComas, D. J.; Heirtzler, D.; Kucharek, H.; Rahmanifard, F.; Bzowski, M.; Kubiak, M. A.; Sokół, J. M.; Swaczyna, P.; Frisch, P. C.

doi:10.1088/0067-0049/220/2/25

Cited by 84 publications

(102 citation statements)

References 55 publications

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“…Even a moderate increase in the relative velocities of the Sun and surrounding interstellar cloud from the present 25.4 km s −1 LIC velocity [133,142] to 45 km s −1 (such as found for the cloud named "Vela" by Redfield and Linsky 2008, [122]) leads to a decrease of the heliopause distance by 34% percent from 104 AU to 69 AU [3]. Interactions between the heliosphere and an evolving superbubble at different velocities leads to different configurations for the heliosphere.…”

Section: Impact Of Supernova On Heliospherementioning

confidence: 55%

“…The abundance patterns in the CLIC gas are similar to those of warm clouds [151] but vary between individual cloudlets [122]. The velocities of LIC gas [133] and LIC dust (from in situ measurements of interstellar dust inside of the heliosphere [134,135]) are in agreement indicating that the grain destruction must have occurred far in the past.…”

Section: Clic Kinematicsmentioning

confidence: 68%

“…Predictions from these models include densities of n HI ∼ 0.19 cm −3 , n(e)∼ 0.07 cm −3 , ionization levels of hydrogen and helium ∼ 22% and ∼ 39% respectively for a cloud temperature of 6300 K, the full destruction of carbonaceous grains in the LIC, and elevated gas-phase abundances for Fe and Mg that indicate silicate grains [10]. In situ measurements of interstellar HeI inside of the heliosphere yield a LIC temperature of 8000 ± 1300 K [133]. Solar abundances are also found for carbon in the low density gas at intermediate and high velocities toward Orion [168,151].…”

Section: Clic Kinematicsmentioning

confidence: 95%

“…Velocities for the cloud around the heliosphere can also be estimated from in situ measurements of interstellar gas (e.g. [132,133]) and dust [134,135] that share similar velocities. The upwind direction of the CLIC interstellar wind [5] coincides with the center of the S1 shell [73], with an angle of 14 • ± 18 • between CLIC LSR velocity and the S1 shell center.…”

Section: Clic Kinematicsmentioning

confidence: 99%

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Effect of Supernovae on the Local Interstellar Material

Frisch¹,

Dwarkadas²

2016

Handbook of Supernovae

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A range of astronomical data indicates that ancient supernovae created the galactic environment of the Sun and sculpted the physical properties of the interstellar medium near the heliosphere. In this paper we review the characteristics of the local interstellar medium that have been affected by supernovae. The kinematics, magnetic field, elemental abundances, and configuration of the nearest interstellar material support the view that the Sun is at the edge of the Loop I superbubble, which has merged into the low density Local Bubble. The energy source for the higher temperature X-ray emitting plasma pervading the Local Bubble is uncertain. Winds from massive stars and nearby supernovae, perhaps from the Sco-Cen Association, may have contributed radioisotopes found in the geologic record and galactic cosmic ray population. Nested supernova shells in the Orion and Sco-Cen regions suggest spatially distinct sites of episodic star formation. The heliosphere properties vary with the pressure of the surrounding interstellar cloud. A nearby supernova would modify this pressure equilibrium and thereby severely disrupt the heliosphere as well as the local interstellar medium.

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Section: Impact Of Supernova On Heliospherementioning

confidence: 55%

Section: Clic Kinematicsmentioning

confidence: 68%

Section: Clic Kinematicsmentioning

confidence: 95%

Section: Clic Kinematicsmentioning

confidence: 99%

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Effect of Supernovae on the Local Interstellar Material

Frisch¹,

Dwarkadas²

2016

Handbook of Supernovae

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“…However, these parameters are coupled. They can be expressed as a function of the interstellar neutral flow longitude and the range of allowable parameters along the 4D parameter tube is relatively large (see Schwadron et al 2015). Therefore, an independent measurement of the interstellar flow longitude would help to constrain this parameter tube.…”

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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