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Exploring the Solar System Galactic Frontier in Extreme Ultraviolet Mike Gruntman∗

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Exploring the Solar System Galactic Frontier in Extreme Ultraviolet Mike Gruntman∗ Acta Astronautica 63 (2008) 1203–1214 www.elsevier.com/locate/actaastro Exploring the solar system galactic frontier in extreme ultraviolet Mike Gruntman∗ Astronautics and Space Technology Division, USC Viterbi School of Engineering, 854 Downey Way, RRB-224, MC-1192, University of Southern California, Los Angeles, CA 90089-1192, USA Received 22 December 2006; received in revised form 18 June 2008; accepted 18 June 2008 Available online 14 July 2008 Abstract The solar system galactic frontier—the region where the expanding solar wind meets the surrounding galactic medium—remains poorly explored. The sheer size of the essentially asymmetric heliosphere calls for remote techniques to probe the properties of its global time-varying three-dimensional boundary. The Interstellar Boundary Explorer (IBEX) mission (launch in 2008) will image the region between the termination shock and the heliopause, the heliospheric sheath, in fluxes of energetic neutral atoms. Global imaging in extreme ultraviolet (EUV) will likely be the next logical step in remote exploration of the galactic frontier + from 1AU. Imaging in EUV will establish directional and spectral properties of (1) the glow of singly charged helium (He ) ions in the interstellar and solar wind plasmas; (2) emissions of hot plasma in the Local Bubble; and (3) characteristic emissions of the solar wind. Global imaging with ultrahigh sensitivity and ultrahigh spectral resolution will map the heliopause and reveal the three-dimensional flow pattern of the solar wind, including the flow over the Sun’s poles. This article presents the emerging concept of the experiment and space mission for heliosphere global imaging in EUV. © 2008 Elsevier Ltd. All rights reserved. 1. Galactic frontier 2007 at 84AU (ecliptic latitude =−31.6◦ and ecliptic longitude = 288.8◦). In September 2008, Voyagers 1 The interaction of the expanding solar wind plasma and 2 are at heliocentric distances of 107.5 and 87.0AU, with the surrounding galactic medium—local interstel- respectively. Crossing the termination shock is a ma- lar medium (LISM)—creates the heliosphere [1–4].The jor milestone in exploration of the outer heliosphere, heliosphere is a complex phenomenon (Fig. 1)where although Voyager spacecraft are instrumented for plan- the solar wind and interstellar plasmas, interstellar gas, etary flybys and not optimized for interstellar studies. magnetic field, and energetic particles all play impor- A possible Sun-LISM interaction [5] illustrates the tant roles [5–8]. The region where the solar wind meets main features of the heliosphere (Figs. 1 and 2). The the galactic medium remains poorly explored. The most interstellar wind (partially ionized interstellar gas) ap- distant operating spacecraft, Voyager 1, had reached the proaches the heliosphere with a supersonic velocity and termination shock and entered the slowed-down post- forms a bow shock. Interstellar neutral atoms penetrate ◦ shock solar wind at 94AU (ecliptic latitude = 34.8 the heliosphere, some reaching the Sun’s vicinity at ◦ and ecliptic longitude = 253.3 ) in December 2004. 1AU. The dynamic pressure of the expanding, highly Voyager 2 crossed the termination shock in September supersonic solar wind decreases with the heliocentric distance. At a certain distance from the Sun, this pres- ∗ Tel.: +12137405536; fax: +12138215819. sure equals the external LISM pressure of the interstel- E-mail address: [email protected]. lar wind and magnetic field. The solar wind expansion 0094-5765/$- see front matter © 2008 Elsevier Ltd. All rights reserved. doi:10.1016/j.actaastro.2008.06.011 1204 M. Gruntman / Acta Astronautica 63 (2008) 1203–1214 Fig. 1. Sun’s galactic neighborhood. The interaction of the expanding solar wind with the surrounding interstellar medium creates the heliosphere; CR—cosmic rays; B—interstellar magnetic field. Circles 1 and 2 show positions of Voyagers 1 and 2 spacecraft, respectively, heading in antisolar directions. The future Interstellar Probe will fly in the upwind (with respect to the interstellar wind) direction. Box (left) shows important directions (interstellar wind vector, apex, a-Centauri) in the ecliptic plane. transitions to a subsonic flow at the termination shock. tion shock will reveal the asymmetry of the magnetic There the kinetic energy of the supersonic flow is largely field, with the stronger effect expected in case of the converted into thermal energy in the subsonic plasma heliopause. beyond the shock. The subsonic heated postshock so- Voyager 1 will be turned off in 2020–2025 at 150AU lar wind plasma (Fig. 2, top) flows in the heliospheric from the Sun because of the decreasing power pro- sheath around the termination shock and down the he- vided by its radioisotope thermoelectric generators. If liospheric tail, where it eventually mixes with the in- operational when the spacecraft reaches the heliopause, terstellar galactic plasma at distances > 5000 AU [10]. Voyager 1 will not be able to determine the shape of the The galactic plasma (Fig. 2, bottom) flows around the heliosphere or the heliopause and the directional vari- heliopause, the boundary separating solar and galactic ations of the nature of the heliospheric sheath or the plasmas. processes therein. The spacecraft probes the essentially asymmetric three-dimensional heliospheric boundary in 2. Three-dimensional heliosphere one point-direction as the future Interstellar Probe will do. Interstellar Probe will reach 300–400AU from the Three fundamental factors make the heliosphere es- Sun in the approximately same direction as Voyager 1 sentially asymmetric: (1) the motion of the Sun with [12–14]. respect to the surrounding interstellar medium, some- Our present experimental capabilities to explore in times described as the interstellar wind; (2) asymmetry situ the outer heliosphere are limited by the technical of the solar wind flow in heliolatitude; and (3) in- difficulties, including propulsion limitations, and bud- terstellar magnetic field of the unknown magnitude getary realities of sending space probes to this distant and direction. The interstellar wind velocity and di- region and beyond. At the same time, the structure rection are well established: 26km/s (or 5.2AU/yr) and the physical processes at the solar system galactic and ecliptic latitude ≈ 5◦ and ecliptic longitude frontier—the heliospheric interface—are of fundamen- ≈ 255◦, respectively. The solar wind flow is highly tal importance for understanding the interaction of our anisotropic during solar minimum [9,11] with the typi- star, the Sun, with the galactic medium. This region also cal velocities near ecliptic 450km/s and over the poles needs to be charted for optimizing our first foray into 750km/s. The direction of interstellar magnetic field interstellar space by the Interstellar Probe mission and in the Sun’s vicinity is unknown. It is anticipated that for supporting the truly interstellar exploration and in- the shapes of both the heliopause and the termina- terstellar travel of the future. M. Gruntman / Acta Astronautica 63 (2008) 1203–1214 1205 comprehensive exploration and “putting on the maps” the solar system galactic frontier. The sheer size of the heliosphere calls for remote techniques to probe its global time-varying three-dimensional properties [15–17]. Two most promising experimental concepts have emerged to remotely study the heliospheric interface. These concepts rely on emissions originating at the solar system galactic frontier and reaching the observer at 1AU with little disturbance. First, heliosphere imag- ing in fluxes of energetic neutral atoms (ENAs) will probe the plasma properties in the heliospheric sheath between the termination shock and the heliopause (Fig. 2. Second, imaging of the heliosphere in extreme ultraviolet (EUV) wifth high spectral resolution will map the heliopause. The concept of ENA imaging of the heliospheric interface originated in late 1970s and early 1980s [18,19]. (Some not readily available publications can be downloaded from http://astronaticsnow.com/ENA/.) The first dedicated space experiment and instrumenta- tion to detect ENAs from the heliospheric interface had been prepared for launch by mid-1980s. The mission was repeatedly delayed and the experiment faded away [15,19]. In 1992, a prediction of strong anisotropy of he- liospheric ENA fluxes pointed to ENA imaging as a promising tool of studying the heliospheric sheath [20] Today, the concept [21] and the new generation of ENA instrumentation [15,22,23] are mature. NASA’s Inter- stellar Boundary Explorer [23] (IBEX) will be launched in 2008 to perform heliosphere ENA imaging. Global ENA images would clearly differentiate [21] between physically distinct possibilities of processes at the ter- mination shock and beyond and reveal properties of the Fig. 2. Interaction of the solar wind with the interstellar medium. plasma and pickup protons in the heliospheric sheath. ISG(P)—interstellar gas (plasma); BS—bow shock; TS—termination IBEX will deploy in a highly eccentric orbit, with a shock; HP—heliopause; CR—cosmic rays; B—magnetic field. Sun-pointed spinning spacecraft obtaining all-sky ENA Asymmetry of Sun’s output pattern [9] illustrates conditions typical for solar minimum. Angle q is counted from the upwind (interstellar images in several energy bins each six months [23]. wind) direction. Top: The heliospheric sheath (heliosheath) region The second concept to map the heliopause in EUV (orange; between TS and HP) con-tains the heated postshock solar and to explore the flow of interstellar plasma around it wind plasma and pickup protons, a source of heliospheric energetic (Fig. 2, bottom) was formulated in 1990s [17,24,25]. neutral atoms (ENAs); IBEX (launch in 2008) will image this re- EUV imaging is the next logical step [17,26,27] in re- gion in fluxes of ENAs. Bottom: Interstellar plasma (blue) flows around the heliopause. Imaging in extreme ultraviolet (EUV) will mote probing of the solar system galactic frontier after probe this flow and map the heliopause as discussed in this work. IBEX will have examined the termination shock and imaged the plasma and pickup protons in the helio- spheric sheath in fluxes of ENAs. EUV imaging will 3.
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