Science Opportunities from Observations of the Interstellar Neutral Gas with Adjustable Boresight Direction

Sokół, J. M.; Kubiak, M. A.; Bzowski, M.; Möbius, E.; Schwadron, N. A.

doi:10.3847/1538-4365/ab50bc

Cited by 20 publications

(54 citation statements)

References 79 publications

(135 reference statements)

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“…However, the conclusion that times of flight for the primary atoms are on the order of three solar cycles and for the secondary atoms an order of magnitude longer holds regardless of the viewing geometry. We verified this by simulating a different viewing geometry, namely that planned for a future space experiment IMAP-Lo Sokół et al 2019b). In this geometry, the viewing direction of the detector is no longer fixed perpendicular to the spacecraft rotation axis, and consequently, it will be possible to maintain the peak of the ISN flux in the instrument field of view almost throughout the year.…”

Section: Isn Hementioning

confidence: 88%

“…In this geometry, the viewing direction of the detector is no longer fixed perpendicular to the spacecraft rotation axis, and consequently, it will be possible to maintain the peak of the ISN flux in the instrument field of view almost throughout the year. Sokół et al (2019b) identified advantageous viewing geometries. We selected one of them, distant from the vantage points of IBEX, and calculated the times of flight and their spread, as well as the speeds of the observed atoms in the OHS.…”

Section: Isn Hementioning

confidence: 99%

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Time delay between outer heliosheath crossing and observation of interstellar neutral atoms

Bzowski¹,

Kubiak²

2020

Preprint

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In situ measurements of the heliospheric particle populations by the Voyager spacecraft can only be put in an appropriate context with remote-sensing observations of energetic and interstellar neutral atoms (ENAs and ISN, respectively) at 1 au when the time delay between the production and the observation times is taken into account. ENA times of flight from the production regions in the heliosheath are relatively easy to estimate because these atoms follow almost constant speed, force-free trajectories. For the ISN populations, dynamical and ballistic selection effects are important, and times of flight are much longer. We estimate these times for ISN He and H atoms observed by IBEX and in the future by IMAP using the WTPM model with synthesis method. We show that for the primary population atoms, the times of flight are on the order of three solar cycle periods, with a spread equivalent to one solar cycle. For the secondary populations, the times of flight are on the order of ten solar cycle periods, and during the past ten years of observations, IBEX has been collecting secondary He atoms produced in the OHS during almost entire 19th century. ISN atoms penetrating the heliopause at the time of Voyager crossing will become gradually visible about 2027, during the planned IMAP observations. Hypothetical variations in the ISN flow in the Local Interstellar Medium are currently not detectable. Nevertheless, we expect steady-state heliosphere models used with appropriately averaged solar wind parameters to be suitable for understanding the ISN observations.

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Section: Isn Hementioning

confidence: 88%

Section: Isn Hementioning

confidence: 99%

Time delay between outer heliosheath crossing and observation of interstellar neutral atoms

Bzowski¹,

Kubiak²

2020

Preprint

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“…In addition, the systematic uncertainties injected by the substantial ionization loss of these species on their way to 1 AU can be largely eliminated with the observations at various ecliptic longitudes (Sokół et al. 2019b ).…”

Section: Observations Of Energetic Neutral Atoms and Interstellar Neu...mentioning

confidence: 99%

“…In this way, Ne and O will be better separated, and their angular distribution is obtained separately at different ecliptic longitudes. In addition, the systematic uncertainties injected by the substantial ionization loss of these species on their way to 1 AU can be largely eliminated with the observations at various ecliptic longitudes (Sokół et al 2019b).…”

Section: Interstellar Oxygen and Other Heavy Speciesmentioning

confidence: 99%

The Heliosphere and Local Interstellar Medium from Neutral Atom Observations at Energies Below 10 keV

et al. 2022

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As the heliosphere moves through the surrounding interstellar medium, a fraction of the interstellar neutral helium, hydrogen, and heavier species crossing the heliopause make it to the inner heliosphere as neutral atoms with energies ranging from few eV to several hundred eV. In addition, energetic neutral hydrogen atoms originating from solar wind protons and from pick-up ions are created through charge-exchange with interstellar atoms.This review summarizes all observations of heliospheric energetic neutral atoms and interstellar neutrals at energies below 10 keV. Most of these data were acquired with the Interstellar Boundary Explorer launched in 2008. Among many other IBEX breakthroughs, it provided the first ever all-sky maps of energetic neutral atoms from the heliosphere and enabled the science community to measure in-situ interstellar neutral hydrogen, oxygen, and neon for the first time.These observations have revolutionized and keep challenging our understanding of the heliosphere shaped by the combined forces of the local interstellar flow, the local interstellar magnetic field, and the time-dependent solar wind.

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“…All these models derive from a series of seminal papers by Hummer (Hummer 1962(Hummer , 1964(Hummer , 1968(Hummer , 1969a and assume that the temperature of the ISN gas inside the heliosphere is isotropic. However, the anisotropy of the distribution function of ISN gas within a few au from the Sun is strong and can be adequately represented neither by an isotropic nor anisotropic Maxwell-Boltzmann function (see, e.g., Fahr 1979;Kubiak et al 2019;Sokó l et al 2015b;Sokó l et al 2019) even when one neglects the charge exchange reaction between the charged and neutral interstellar components in the outer heliosheath.…”

Section: Introductionmentioning

confidence: 99%

WawHelioGlow: a model of the heliospheric backscatter glow. I. Model definition

Kubiak,

Bzowski,

Kowalska-Leszczynska

et al. 2021

Preprint

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The helioglow is a fluorescence of interstellar atoms inside the heliosphere, where they are excited by the solar EUV emission. So far, the helioglow of interstellar H and He have been detected. The helioglow features a characteristic distribution in the sky, which can be used to derive both the properties of interstellar neutral gas and those of the solar wind. This requires a simulation model capable of catching with a sufficient realism the essential coupling relations between the solar factors and interstellar. The solar factors include the solar wind flux and its variation with time and heliolatitude, as well as the heliolatitude and time variation of the solar EUV output. The ISN gas inside the heliosphere features a complex distribution function, which varies with time and location. The paper presents the first version of a WawHelioGlow simulation model for the helioglow flux using an optically thin, single scattering approximation. The helioglow computations are based on a sophisticated kinetic treatment of the distribution functions of interstellar H and He provided by the (n)WTPM model. The model takes into account heliolatitudinal and spectral variations of the solar EUV output from observations. We present a formulation of the model and the treatment of the solar spectral flux. The accompanying Paper II illustrates details of the line of sight evolution of the elements of the model and a brief comparison of results of the WawHelioGlow code with selected sky maps of the hydrogen helioglow, obtained by the SWAN instrument onboard the SOHO mission.

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Science Opportunities from Observations of the Interstellar Neutral Gas with Adjustable Boresight Direction

Cited by 20 publications

References 79 publications

Time delay between outer heliosheath crossing and observation of interstellar neutral atoms

Time delay between outer heliosheath crossing and observation of interstellar neutral atoms

The Heliosphere and Local Interstellar Medium from Neutral Atom Observations at Energies Below 10 keV

WawHelioGlow: a model of the heliospheric backscatter glow. I. Model definition

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