How catching the interstellar wind in the inner solar system led the way on a road to interdisciplinary research between heliophysics and astrophysics

1 Introduction

For a long time, astronomers have located the Sun inside the local interstellar cloud (LIC) (Bertin et al., 1993; Lallement et al., 1995; Redfield and Linsky, 2008; Frisch et al., 2009), albeit close to its edge. However, a recent study places the Sun in a mixing region between the LIC and the G-Cloud (Swaczyna et al., 2022a). It compares in situ measurements of the interstellar neutral (ISN) gas flow vector through the solar system, based on precision analysis of ISN imaging (Wood et al., 2015; Swaczyna et al., 2022b) and pickup ion (PUI) observations (Taut et al., 2018; Bower et al., 2019), with those obtained from stellar absorption lines for nearby interstellar clouds. PUI observations on New Horizons that the H density in our neighborhood is twice as high (Swaczyna et al., 2020) than that derived from absorption lines in the LIC and G-Cloud (Redfield and Linsky, 2008; Linsky et al., 2022) support this finding. To my knowledge, this is the first time that space physics-based in situ observations have diagnosed the interaction of two interstellar clouds, placing the solar system exactly where the action is. Thus, the time has come to conduct genuine interdisciplinary studies between space and astrophysics, and we will map the road that led us here.

2 Discovery of interstellar pickup ions

The journey started on 11 September 1984 at the German Spacecraft Operations Center in Oberpfaffenhofen. After waiting in suspense, the solar wind (SW) conditions appeared to be on target for the first ion cloud release from the Active Magnetospheric Particle Tracer Explorers (AMPTE) Ion Release Module (IRM) (Haerendel et al., 1985), with the interplanetary magnetic field (IMF) almost perpendicular to the SW. After a quick readiness check, the IRM ejected two Li and CuO canisters. They drifted for 10 mins before the mixture ignited and generated an expanding cloud, which silenced the SW for a few seconds like within a comet coma (Häusler et al., 1986). The nearly perpendicular IMF was supposed to pick up the freshly generated Li⁺ ions and propel them toward the Earth’s magnetosphere. Capable of identifying these ions, the time-of-flight (TOF) spectrograph AMPTE SULEICA (Möbius et al., 1985a) indeed found only seven Li⁺ ions before the IMF turned any ions out of its field of view (FOV) (Möbius et al., 1986). However, this disappointing result came with a stunning surprise. He⁺ ions showed up with the Li⁺ ions repeatedly. The IMF must have picked them up in the SW, freshly ionized from a gas almost at rest like Li, as shown in Figure 1A, hence called PUIs.

FIGURE 1

FIGURE 1. (A) Historic TOF versus energy representation of individual He⁺ and Li⁺ PUIs detected before and after the first AMPTE Li release. (B) He⁺ PUI flux obtained with AMPTE SULEICA as a function of day of the year in 1984. The flux reaches a maximum in early December when the Earth is downwind of the Sun relative to the ISN gas flow through the solar system [adapted from (Möbius et al., 1985b)], reproduced with permission from Springer Nature. AMPTE IRM was in the SW only from September through January, hence the clipped coverage of PUIs. (C) PUI motion in the plane perpendicular to the IMF (the blue circular symbol), gyrating about the IMF in the SW frame (the dashed black line), and moving on a cycloid in the spacecraft frame (the solid red line). After ionization from neutral gas at rest, a PUI (the open red circle) starts with V = 0 in the rest frame, while it is injected into the SW with V’ = -V_SW in the SW frame. Therefore, the PUI gyrates about the IMF with the speed V_SW (the dashed black circle). In the rest frame, this gyration is seen as a cycloid trajectory, which starts with V = 0, reaches a maximum speed of 2V_SW or cut-off at the top, where the PUI speed in the SW frame adds to the SW speed, and completes one turn again with V = 0. This motion is similar to that of a valve of a bicycle wheel, as seen by an observer at rest. It distinguishes PUIs from the motion and energy distribution of SW ions. Scattering of PUIs in their pitch angle α (see 1D) at fluctuations in the IMF bring PUIs to the cut-off for all IMF angles. Continuous PUI production from the Sun to the observer and adiabatic cooling in the expanding SW fills the velocity space between 2V_sw and the SW itself. An introduction to PUIs may be found in a recent text book (Hsieh and Möbius, 2022) and review (Zirnstein et al., 2022) and presents a full overview on PUIs in the heliosphere. (D) PUI motion in the SW-IMF plane, along with the AMPTE SULEICA FoV. If the IMF is at an angle α < 90° relative to the SW, PUIs are injected into the SW at pitch angle α, resulting in a velocity component parallel to the IMF, which leads to an overall transport of PUIs in the rest frame at angle α relative to the IMF. Shown are sample directions of the PUI motion for IMF orientations that, after initial pickup, lead the ions into the FoV (solid line, α > 70°) or miss the FoV (dashed line, α < 70°).

Their fluxes exceeded those for He from the Earth’s exosphere at IRM’s distance by three orders of magnitude. Memories arose from an astronomy seminar as a student at Bochum about background radiation. My assignment focused on Lyman-α background, which, to my disappointment, originated in our backyard, ISN gas illuminated by the Sun (Bertaux and Blamont, 1971). Contrary to earlier astronomical wisdom, the solar system is not (Fahr, 1968) within a Strömgren sphere (Strömgren, 1939). The ISN gas blows through the solar system as an interstellar wind, too fast for ionization before reaching 1 AU. Interstellar He forms a unique pattern in the inner heliosphere, focused downwind of the Sun (Weller and Meier, 1974; Fahr et al., 1976). I thought, “Wouldn’t it not be cool if the He⁺ ions were of interstellar origin?” Indeed, they exhibited the predicted behavior with a substantial flux enhancement in early December when the Earth is downwind of the flow (Möbius et al., 1985b) (Figure 1B). The literature from a student seminar proved invaluable for identifying a fundamental discovery, PUIs from the interstellar wind, and so did the humble explorer AMPTE (Krimigis et al., 1982), initiated by Tom Krimigis and Gerhard Haerendel.

The He⁺ ions were visible continuously up to a cut-off at 2V_sw or 4E_sw, as previously predicted (Vasyliunas and Siscoe, 1976) (Figure 1C), contrary to locally injected Li⁺ PUIs that entered SULEICA only during favorable IMF orientations (Figure 1D). Continuous He⁺ PUI injection into the SW affords its effective scattering in pitch angle α at IMF fluctuations and adiabatic cooling in the expanding SW (Isenberg, 1986; Isenberg, 1987; Möbius et al., 1988), filling the observed spectra up to 4E_sw, as explained in a recent text book (Hsieh and Möbius, 2022) and PUI review (Zirnstein et al., 2022).

3 Diagnostic opportunities with pickup ions and their challenges

This first in situ diagnostic method for ISN gas expanded the horizon of space plasma physics into the Sun’s galactic neighborhood. It allowed the sampling of interstellar He, H (Gloeckler et al., 1993), N, O, and Ne (Gloeckler and Geiss, 1998), the calculation of their abundance ratios (Gloeckler and Geiss, 2001), and an estimate of the ISN flow velocity and temperature (Möbius et al., 1995).

However, PUIs presented formidable challenges in determining the dynamic ISN parameters precisely. Slower than anticipated pitch-angle scattering made the PUI distributions asymmetric in the SW frame, softened the otherwise sharp cut-off at 2V_sw, and lowered the most easily accessible part of the PUI fluxes above the SW energy (Gloeckler et al., 1995; Möbius et al., 1998). PUI distributions and fluxes varied substantially in response to SW structures, such as stream interaction regions (SIRs) and coronal mass ejections (CMEs) (Möbius et al., 2010). Non-radial PUI transport in the SW affects the shape and location of the focusing cone (Möbius et al., 1996; Chalov and Fahr, 2006; Quinn et al., 2016). Effective acceleration into a suprathermal tail smoothens the PUI cut-off further (Gloeckler et al., 2000; Möbius et al., 2019).

However, one person’s trash may be another’s treasure. When interstellar PUIs came up as a tentative explanation for the He⁺ by AMPTE IRM, Dieter Hovestadt exclaimed “SULEICA has detected the seed particles for the anomalous cosmic rays (ACR)” (Garcia-Munoz et al., 1973; Hovestadt et al., 1973; Klecker, 1995; Jokipii, 1998). ACRs are substantially overabundant in O and Ne over galactic cosmic rays. Dieter pointed to a model that implicated the ISN gas (Fisk et al., 1974) and opened another essential connection for PUIs. They form a particle distribution that enables preferential injection into acceleration to higher energies. The enormous injection efficiency compared to underlying bulk plasma was visible in SIRs (Gloeckler et al., 1994; Morris et al., 2001; Möbius et al., 2002) and CMEs (Kucharek et al., 2003), with remarkable He⁺ overabundances over SW He²⁺ in the respective energetic particles. Identifying He⁺ PUIs as the source solved a previous mystery: He⁺/He²⁺ ratios in energetic interplanetary particles that substantially exceeded the SW ratio (Hovestadt et al., 1984).

Another aspect of the PUI distribution took a surprising turn much later. During a seminar on the PUI discovery, Martin Lee mused whether Alfvén waves that lag behind the SW could reduce the He⁺ PUI cut-off energy by ≈ 10–15% from the nominal 4E_sw as the observations seemed to suggest. However, this conclusion would have been a stretch with SULEICA’s 10% energy width, data points spaced by 20% in energy, and integration over a 40 × 45° FOV. Only 15 years later, when analyzing PUI data from CELIAS (Hovestadt et al., 1995) on the SOlar and Heliospheric Observatory (SOHO), centered around June, or upwind of the Sun relative to the ISN flow, the original question entered daylight again but with a twist. The cut-off was ≈15% above the nominal value. SOHO observing upwind and AMPTE IRM downwind suggested an explanation. Because in the SW frame, PUI injection occurs with the vector sum of its local ISN flow and SW velocities, and the cut-off was at a noticeably higher PUI speed on the upwind side than the downwind side (Möbius et al., 1999).

The advent of PLASTIC (Galvin et al., 2008) on the Solar Terrestrial RElations Observatory (STEREO), with superior energy and angle resolution in the PUI regime, enabled a more detailed study of the PUI evolution after their initial injection (Drews et al., 2015). It also turned this earlier discovery into a precision tool to obtain at least the ISN flow direction with much higher fidelity. When increasing ionization losses of the ISN flow from the upwind to the downwind side could not produce the He⁺ PUI crescent (Sokól et al., 2016), as proposed earlier (Drews et al., 2012), flux modulation due to the shifting PUI cut-off within the fixed energy window in the analysis became the focal point. This explanation suggested using symmetry in the PUI cut-off shift in the flow axis to determine the ISN flow longitude precisely (Möbius et al., 2015a; Taut et al., 2018; Bower et al., 2019). This measurement has now become a linchpin in obtaining the complete set of dynamic ISN gas parameters in the very local interstellar medium (VLISM) just outside the solar system from local observations the inner heliosphere, complementary to the direct ISN flow observations at 1 AU (Möbius et al., 2009a) with the Interstellar Boundary Explorer (IBEX) (McComas et al., 2009a). These neutral gas measurements became possible after the pioneering observations of the He ISN flow with Ulysses GAS (Witte et al., 1996).

4 Catching the neutral interstellar wind directly

The discovery of the interstellar PUIs triggered the invitation by Hans Fahr in 1986 to a series of workshops focused on the interaction between the heliosphere and the surrounding interstellar medium that involved German, Polish, and Soviet groups. The workshops revolved around observational and modeling efforts to understand our galactic neighborhood. During one meeting, Helmut Rosenbauer jokingly regretted that the PUI observations would steal the thunder of Ulysses GAS (Witte et al., 1992), whose launch was still in the future. However, this tiny sensor that measured the ISN He distribution via sputtering Li⁺ ions off a LiF surface obtained images of the He ISN flow during the transit of Ulysses to Jupiter and during the three fast latitude scans when Ulysses scoped out the 3D structure of the SW and energetic particles. Following the He atoms along their hyperbolic trajectories in the Sun’s gravitational field (Fahr, 1974; Wu and Judge, 1979; Lee et al., 2012; Lee et al., 2015) with a tailored fitting technique (Banaszkiewicz et al., 1996) translates the neutral He images into the velocity distribution function outside the heliosphere. The GAS observations of the He ISN flow enabled the most detailed and accurate determination of the ISN flow vector and temperature (Witte, 2004). These values were validated and placed into context with PUI and solar ultraviolet backscattering observations of ISN He within a scientific team at the International Space Science Institute (ISSI). The team effort consolidated the ISN gas parameters (Möbius et al., 2004) and reemphasized the complementary nature of the three in situ observation techniques, each affected by different systematic uncertainties.

This collaborative work on the physical state of the interstellar medium dovetailed into the proposal of a potential explorer mission to study the VLISM and its interaction with the heliosphere, the Interstellar Pathfinder, which, in two attempts, almost made it into a Phase B study, but only “almost”. The studies proposed sounded like the perfect interdisciplinary endeavor that could engage two scientific communities, heliophysics and astrophysics, and thus garner multiple support. Instead, the advice was to root the proposal firmly in heliophysics; otherwise, it may fall between all chairs. In a third attempt, the concentration on two neutral atom cameras with the capability to image the boundary of the heliosphere in energetic neutral atoms (ENA) and to simultaneously capture the interstellar wind of He, O, and possibly H under the constraints of a Small Explorer kicked the proposal above the threshold and led to the successful IBEX mission (McComas et al., 2009a).

The combination of mechanical collimation, surface conversion of neutral atoms into negative ions, electrostatic energy analysis, post-acceleration, and a triple time-of-flight measurement in IBEX-Lo (Fuselier et al., 2009) enabled the observation of the He, H, and O ISN flow (Möbius et al., 2009b) and even Ne (Bochsler et al., 2012) (Figures 2A,C). Thus, IBEX went substantially beyond the GAS capabilities, increasing the signal-to-background ratio by orders of magnitude for He and expanding to other species. However, with its observations limited severely in ecliptic longitude to less than 2 months in early spring when the IBEX FOV points to the oncoming flow, approximately parallel to the Earth’s orbit, the observations and analysis are subject to degeneracy in the ISN parameter space. It is obvious for an idealized ISN trajectory that passes IBEX precisely perpendicular to the IBEX-Sun line, i.e., reaching its perihelion at the point of observation (Möbius et al., 2012) (Figures 2B,D). Trajectories that start at infinity over a wide range of ISN speeds V_ISN∞ and inflow longitudes λ_ISN∞ fulfill this condition when coupled with the hyperbolic trajectory equation:

$\mathrm{c}os\left({\lambda }_{ISN\infty }+{180}^o-{\lambda }_{Peak}\right)=\mathit{cos}{\theta }_{\infty }=\frac{-1}{1+\frac{r_E{V}_{ISN\infty }^2}{G{M}_S}}.(1)$

FIGURE 2

FIGURE 2. Left: Combination of IBEX ENA maps in Mollweide projection that illustrate the interstellar medium information collected at 1 AU. Right: Schematic view of the ISN and ENA trajectories from their source to the observer at 1 AU. (A) ISN He and H flow based on H count rates at 15 eV, along with secondary He neutrals [adapted from (Park et al., 2016; Swaczyna et al., 2018)], reproduced with permission from AAS. (B) Schematic representation of ISN He, O, and Ne (green), as well as H (red) trajectories in the plane that contains ${\overrightarrow{V}}_{ISN\infty }$, the Sun, and the in-ecliptic location λ_Peak where the bulk ISN flow is observed at its perihelion. The ISN flow arrives from λ_ISN∞ at the heliopause, whose value is connected through the angle swept out by the arriving atoms from infinity to perihelion or true anomaly θ_∞ to λ_Peak and V_ISN∞ in Eq. 1; Eq. 1 describes unbound Keplerian trajectories. It describes V_ISN∞ as a function of λ_ISN∞ (samples shown as dashed green lines) for the observed value of λ_Peak. An extended range of observer locations for the angular distribution of the ISN flow around the peak constrains λ_ISN∞ and V_ISN∞ separately. For ISN H, λ_Peak shifts to larger ecliptic longitude due to the partial compensation of gravitation by solar radiation pressure, increasingly during high solar activity (dashed red) (Rahmanifard et al., 2019). (C) ISN O and Ne flow based on O count rates at 279 eV, along with secondary O neutrals [adapted from (Park et al., 2015)], reproduced with permission from AAS. (D) Same representation as above for the ISN flow (green) and secondary neutral distributions (blue), whose arrival directions at the heliopause and λ_Peak at 1AU are shifted to a smaller longitude. In the maps, the ISN He, O, and Ne flow arrives from the same direction in the sky, deflected westward from the arrival direction outside the heliopause (shown as a yellow dot in panel A) due to the Sun’s gravitation. In contrast, the ISN H flow is deflected eastward due to radiation pressure. The arrival directions of the ISN flow (yellow dot) and secondary He (white dot), the Ribbon center (open red circle), and the derived ${\overrightarrow{B}}_{ISM}$ direction line up along the ${\overrightarrow{B}}_{ISM}$—${\overrightarrow{V}}_{ISN}$ plane (the dashed green line).

θ_∞ is the angle swept out by the position vector of the atom from infinity to perihelion or the true anomaly of the trajectory; λ_Peak is the ecliptic longitude of the observer when seeing the peak ISN flow; M_s is the Sun’s mass; G is the gravitational constant; and r_E = 1 AU (Lee et al., 2012). Because the inflow latitude β_ISN∞ and temperature T_ISN∞ connect these quantities dynamically, the analysis of IBEX observations leads to a four-dimensional tube in the parameter space (McComas et al., 2012). Observations of the full He distribution over a range in ecliptic longitude constrain the tube in length (Schwadron et al., 2015a; Möbius et al., 2015b; Swaczyna et al., 2015; Swaczyna et al., 2018), and the PUI analysis previously discussed provides a complementary value for λ_ISN (Möbius et al., 2015a; Taut et al., 2018; Bower et al., 2019).

5 Synergism between PUI, ISN flow, and ENA observations for the heliosphere and beyond

When IBEX-Lo caught the interstellar wind, IBEX-Hi (Funsten et al., 2009) and Lo (Fuselier et al., 2009) combined took the first all-sky images of the heliospheric boundary in the light of ENAs, thus expanding the emerging field of neutral-atom astronomy to its horizon (Hsieh and Möbius, 2022). At low ENA energies, the IBEX maps reveal secondary He (Kubiak et al., 2014; Kubiak et al., 2016) (Figure 2A) and O (Park et al., 2015; Park et al., 2016) (Figure 2C) interstellar neutral flows, which originate in the region outside the heliopause from the charge exchange of interstellar ions with the ISN gas flow. The secondary neutral flow appears slower and hotter than the pristine ISN flow, hence also referred to as the “warm breeze” (Kubiak et al., 2014). This is because the secondary neutrals mimic the distribution of the interstellar plasma, which slows down and heats in response to the presence of the heliosphere. As the secondary neutral signal is at a level of a few percent of the pristine ISN flow for He and O, its prior analysis is necessary before the velocity distribution of secondary neutrals can be extracted from the observations. Both secondary populations appear substantially deflected relative to the pristine ISN flow in the same direction as ISN H (Lallement et al., 2005) in a plane, dubbed the H-deflection plane, which, based on global heliospheric simulations, contains the interstellar flow velocity ${\overrightarrow{V}}_{ISN}$ and the interstellar magnetic field (ISMF) ${\overrightarrow{B}}_{ISM}$ (Izmodenov et al., 2005), and thus may be termed the ${\overrightarrow{B}}_{ISM}-{\overrightarrow{V}}_{ISN}$ plane. It should be noted that the H ISN flow direction represents a combination of primary H ISN and secondary H and thus shows a deflection (Izmodenov et al., 2005; Lallement et al., 2005) between the primary He (Schwadron et al., 2015a) and O (Schwadron et al., 2016) ISN and the secondary He and O directions (Kubiak et al., 2016; Park et al., 2019). The ${\overrightarrow{B}}_{ISM}$ orientation deduced from the arrangement of the multiple flow directions in the sky was consistent with the heliospheric asymmetry derived from the Voyager 1 and 2 termination shock traversals (Opher et al., 2006; Stone et al., 2008).

Interestingly, the first IBEX ENA sky maps revealed a bright unanticipated Ribbon (McComas et al., 2009b) that traces out a circle in the sky, which conforms with ${\overrightarrow{B}}_{ISM}\bullet \overrightarrow{r}=0$ (Schwadron et al., 2009). $\overrightarrow{r}$ indicates the look direction, and ${\overrightarrow{B}}_{ISM}$ is consistent with the orientation found in global heliospheric models constrained by the aforementioned observations (Izmodenov et al., 2005; Lallement et al., 2005; Pogorelov et al., 2009a; Opher et al., 2009). However, the physical processes that conspire to form the Ribbon are less clear and still under debate at this writing. More than a dozen models, involving different source locations and mechanisms, emerged as summarized in an early review (McComas et al., 2014). The frontrunner, which explains most of the observed Ribbon features, appears to be a model that starts with neutral SW entering the VLISM. Next, charge exchange with interstellar H⁺ generates PUIs, and those injected into the ISMF at ≈90^o are temporarily stored in a ring distribution. This PUI population produces Ribbon ENAs in another charge exchange with ISN H (Heerikhuisen et al., 2010; McComas et al., 2014). A significant challenge for this model is the susceptibility of a PUI ring concentrated at ≈90^o to ${\overrightarrow{B}}_{ISM}$ to instabilities (Gary et al., 1986), which would render the intermediate storage time too short for an effective Ribbon production (Florinski et al., 2010). Several different approaches promise to mitigate this challenge, but their coverage goes beyond the scope of this paper, and the interested reader is referred to Hsieh and Möbius (2022). Simulations based on this Ribbon model constrain the orientation of ${\overrightarrow{B}}_{ISM}$ (Zirnstein et al., 2016) consistent with a field topology around the heliosphere that describes correctly (Schwadron et al., 2015b) the observed TeV cosmic ray anisotropies (Abdo et al., 2008; Abdo et al., 2009; Abbasi et al., 2011). It also agrees with field directions obtained from starlight polarization in our extended neighborhood (Frisch et al., 2022). Remarkably, the Ribbon model also constrains the magnetic field strength (Zirnstein et al., 2016) to values that agree with an earlier determination based on the Voyager TS crossings (Gloeckler et al., 1997).

However, the magnetic field direction measured by Voyager 1 and 2 outside the heliopause, starting in line with the heliospheric field, and the Ribbon-derived direction are still far from each other. After first seemingly approaching the IBEX direction (Schwadron et al., 2015c), it turned back again in response to heliospheric disturbances (Schwadron et al., 2018). Also, the ENA belt, discovered by Cassini INCA at higher energies (Krimigis et al., 2009), appears oriented differently in the sky than the Ribbon, and the heliosheath thickness and heliosphere shapes differ as derived from the ENAs in different energy regimes (Dialynas et al., 2017; Schwadron and Bzowski, 2018). Whether and how the remote and in situ observations of ${\overrightarrow{B}}_{ISM}$ will converge, or the Ribbon and Belt are one or separate phenomena, remain open questions. Also, the debates on the heliospheric topology (Pogorelov et al., 2015; Opher et al., 2020) and the precise extrapolation to the undisturbed ${\overrightarrow{B}}_{ISM}$ (Zirnstein et al., 2016; Izmodenov and Alexashov, 2020) continue.

Yet, combining the O, He, and H ISN flow arrival directions at the heliopause with the He and O secondary neutrals and the ISMF direction arranges them along an arc that represents the plane, which organizes the deflection of the interstellar plasma flow around the heliosphere (Pogorelov et al., 2009b; Izmodenov et al., 2009). Thus, together with ${\overrightarrow{B}}_{ISM}$ and ${\overrightarrow{V}}_{ISN}$, the secondary neutral flow observations effectively constrain the shape of the heliopause and the plasma flow around it in global heliosphere models, while the TS and heliopause crossings of the two Voyager spacecraft (Stone et al., 2008; Krimigis et al., 2013; Stone et al., 2013; Burlaga and Ness, 2014) provide a linchpin on the absolute size of the heliosphere.

6 Foray into the VLISM, a truly interdisciplinary endeavor between space plasma and astrophysics

With the fidelity of the ISN flow and secondary neutral observations and analysis achieved to date, catching the interstellar wind in the inner heliosphere now connects to several aspects of astrophysics in our galactic neighborhood. For example, a detailed analysis of the secondary He flow provides the He⁺ density, and thus, the ratio of ionized and neutral He and H in the VLISM (Bzowski et al., 2019), which, in turn, constrains the radiation environment in the Sun’s neighborhood (Slavin and Frisch, 2008). Improvements in the precision of the locally obtained interstellar flow parameters (Swaczyna et al., 2022b) and densities (Swaczyna et al., 2020) now strongly support an earlier suspicion, i.e., that the Sun is neither inside the LIC nor the G-cloud proper (Redfield and Linsky, 2008). Most likely, the solar system traverses an interaction region between these two adjacent interstellar clouds in our immediate galactic neighborhood (Swaczyna et al., 2022a). A recently discovered anisotropy in the ISN He distribution (Wood et al., 2019) may even be a sign of incomplete mixing of the two cloud populations and thus provide insights into the kinetics of the interstellar cloud interaction. Furthermore, obtaining abundances of the ISN species that make it inside the heliosphere through PUI (Gloeckler and Geiss, 2001) and ISN sampling, in particular, for O and Ne (Park et al., 2014), provides a window on the processing of matter in the Milky Way over time (Prantzos et al., 1998). With the interstellar ³He/⁴He ratio from PUIs (Gloeckler and Geiss, 1996) and the D/H ratio from ISN observations (Rodriguez-Moreno et al., 2013), we even touch upon cosmology and Big Bang nucleosynthesis (Schramm et al., 1998). In summary, combining space physics-based in situ diagnostics and astronomy-based spectroscopy finally enables genuine interdisciplinary research opportunities.

By placing a powerful suite of sensors for ENAs, PUIs, energetic particles, interstellar dust, and Lyman-α radiation at the Lagrangian point L1, while monitoring the interplanetary environment, the Interstellar Mapping and Acceleration Probe (IMAP) (McComas et al., 2018) will bring our understanding of the heliosphere and its place in the interstellar medium to the next level. A future dream of an Interstellar Probe that will venture into the VLISM proper and unravel thus far inaccessible ion populations and related interaction processes has recently moved closer to a realization after a detailed scientific and technical feasibility study (McNutt et al., 2021), (Brandt et al., 2023).

Data availability statement

Publicly available datasets were analyzed in this study. These data can be found at: http://ibex.swri.edu/researchers/publicdata.shtml.

Author contributions

The author confirms being the sole contributor of this work and has approved it for publication.

Acknowledgments

The author is very grateful to the many individuals at various institutions that made the many spacecraft missions successful whose observations contributed substantially to the results compiled in this paper. He also gratefully acknowledges the many fruitful collaborations with wonderful colleagues that triggered new insights in many ways. Support for the work toward this manuscript by the IBEX and IMAP projects and by NASA Grant 80NSSC18K1212 is thankfully acknowledged.

Conflict of interest

The author declares that the research was conducted in the absence of any commercial or financial relationships that could be construed as a potential conflict of interest.

Publisher’s note

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