Our Star is one of hundred billion stars in the galaxy that plows through interstellar gas, plasma, and dust made up of the material from supernova remnants. With its pulsating solar wind, the Sun carves out the enormous habitable magnetic bubble encasing the entire solar system that we live in. Understanding the unique interaction mechanisms defining the boundary to interstellar space represents one of the oldest problems in space physics today. These mechanisms are also fundamentally responsible for the vast range of astrospheres observed around hundreds of other stars and exoplanetary systems in our galaxy. Beyond the heliosphere, the local interstellar medium presents an unexplored territory that has a decisive role in the shape and behavior of the entire heliosphere.

The potential for a mission to the Local Interstellar Medium (LISM) has been explored since the beginning of the space age. The remarkable science opportunities that arise from such an "Interstellar Probe" have fueled the community for almost six decades, resulting in multiple studies identifying compelling science goals and questions (Holzer, Mewaldt, and Neugebauer 1990; Liewer et al. 2001; McNutt 2002; Mewaldt and Liewer 2002; Wimmer-Schweingruber et al. 2009; Fiehler and McNutt 2012; Stone 2015; Wang 2018). Throughout those decades the general science questions have not really changed and revolve around the exploration of the heliospheric boundary and the properties of the unexplored LISM. A trajectory through the outer solar system and the Kuiper Belt, beyond our zodiacal cloud, naturally offers groundbreaking opportunities for Planetary Science and Astrophysics as well, even with relatively modest contributions.

The current study has developed its science goals from past efforts and current collaboration with the community. An interstellar probe would answer a wide range of questions from many different disciplines. The brief list below links to more detailed descriptions for each of the proposed topics, including specific questions and objectives for each field of inquiry. We have also provided links to the webinars previously presented by the Interstellar Probe Study team to provide further context and background to each topic.

A potential Interstellar Probe mission would seek to understand:

  • Our Heliosphere as a Habitable Astrosphere and its Place in the Galaxy
  • The Origin and Evolution of Planetary Systems
  • How Early Galaxies and Stars were formed

Understanding our Heliosphere as a Habitable Astrosphere and its Place in the Galaxy

As the expanding, magnetized solar wind meets the plasma, gas and dust flows of the LISM, a complex and vast interface is created that separates the solar environment from the unperturbed interstellar environment that our solar bubble plows through. The interface region spans a sun-centered distance of 90 AU to at least 120 AU (for reference, Pluto is located at 39.5 AU from the Sun). This region is the culmination of remarkable physical processes of astrophysical scales that dictate the entire shape, extent and dynamics of our heliosphere and astrospheres of other star systems.

The limited knowledge we have of this region has been collected by Voyager 1 and 2 that uncovered completely unexpected phenomena that could not be understood with the science payload designed for planetary flybys during the Grand Tour. Several remote observations from deep inside the heliosphere have been seeking information for decades of the heliospheric boundary and what lies beyond, and have found tantalizing evidence for large-scale structures and interactions that cannot be fully explained.

Energetic Neutral Atoms (ENAs) and Ultraviolet (UV) are powerful techniques to gain information on the global structure and dynamics of the boundary, but have all been conducted from vantage points from deep inside the heliosphere looking out making it difficult to interpret the observations uniquely. The emission patterns from the remote Energetic Neutral Atom (ENA) observations by NASA IBEX and Cassini missions have revealed completely unexpected emission patterns from the boundary region that are not yet understood, but seem to indicate large-scale features and variations relating to the shape and thickness of the heliosheath and the external interstellar magnetic field direction. The upcoming NASA IMAP mission will characterize these features at unprecedented resolution from 1 AU and will serve as a crucial guide for an Interstellar Probe mission through the boundary. UV observations conducted by the SOHO, Voyager and New Horizons missions have resolved interstellar hydrogen interacting with the heliosphere forming a "Hydrogen Wall" and an unexplained significant excess of hydrogen.

Interstellar space, or LISM beyond the boundary of our heliosphere is largely unexplored territory and may very well be where an Interstellar Probe would make its most historic scientific discoveries. The unfiltered LISM holds the key to understanding the interaction with the global heliosphere (and other astrospheres), the nearby galactic environment, and how matter in the galaxy originated and evolved. It has long been thought that the heliosphere is completely surrounded by the Local Interstellar Cloud. New evidence is mounting that the heliosphere is in contact with no less than four different interstellar clouds and that the Sun is entering a new region of interstellar space with drastically different properties within relatively short galactic time scales (~6000 years) (Linsky et al., 2019). In a sense, a galactic event with the heliosphere in the leading role is happening around us, which makes the exploration of the LISM timely. Even modest changes in the charge fraction would have drastic consequences for the size of the heliosphere (Baranov & Malama, 1993).

All knowledge we have of the surrounding LISM are average properties (neutral and singly ionized elements in the UV range) derived from absorptions spectra along line of sights towards the nearest handful of stars, and from measurements of interstellar PUIs and dust penetrating the heliosphere (43 total detections to date). Sampling the local ionization state, flows, and chemical and isotopic composition of particles and dust of the unprocessed surrounding LISM would therefore be of vital to our understanding of the heliospheric interaction; provide the first direct determination of the interstellar cloud properties, and provide historical constraints on the chemical evolution of the galaxy and nucleosynthesis. Furthermore, venturing in to an unexplored territory is guaranteed to offer new discoveries of questions that we never knew how to ask.

With the new availability of larger launch vehicles than ever before, humanity now has been given access to the heliospheric boundary and to the galactic environment beyond. In order to design possible mission architectures for this historic exploration, a set of science questions and objectives must be formulated that can be used to derive rigorous requirements on measurements, spacecraft and operations. Below is an example of such compelling questions that have been assembled from past studies and by the community in this study.

Science Question 1: What is the global nature of the heliosphere?

Explore the impact of the solar system on the interstellar medium as an example of the interaction of a stellar system with its interstellar environment

  • What is the size, shape, and structure of the heliosphere?
  • What upholds the force balance of heliosphere against the local interstellar medium (LISM)?
  • Where and what is the "ribbon/belt" and how does its remote and in-situ diagnostic tell us about the global heliosphere and the interaction with the LISM?
  • How do shocks propagate through the outer heliosphere, beyond the heliopause and how do they accelerate particles?
  • What is the structure and nature of the heliopause?
  • Does the heliosphere create a bow shock in the interstellar medium?
  • What is the structure and composition of the neutral "hydrogen" wall and what is its relation to similar structures and winds observed in other astrospheres?

Relevant Webinars

Our Boundary to Interstellar Space: A New Regime of Space Physics Imaging the Heliospheric Boundary

Science Question 2: How do the Sun and galaxy affect the dynamics of the heliosphere?

Explore the influence of the Sun's activity, the interstellar medium and its possible inhomogeneity on the dynamics and evolution of the global heliosphere

  • How do the termination shock and heliopause respond to solar variations and interstellar pressure?
  • How do the Sun and heliosphere influence the temperature, ionization state, energetic particle environment and the magnetic field direction of the local interstellar medium? How far does the influence extend?
  • How does the interstellar medium affect the inner heliosphere and solar wind dynamics?
  • What roles do thermal plasma, pickup ions, waves, and anomalous cosmic rays play in determining the structure of the termination shock?

Relevant Webinars

Our Boundary to Interstellar Space: A New Regime of Space Physics Imaging the Heliospheric Boundary

Science Question 3: What is the nature of the nearby interstellar medium?

Explore the interstellar medium and determine directly the properties of the interstellar gas, the interstellar magnetic field, low-energy cosmic rays, and interstellar dust

  • How does the composition of interstellar matter differ from that of the solar system?
  • What constraints do the interstellar abundances of 2H and 3He place on Big Bang and chemical evolution theories?
  • Is there evidence for recent nucleosynthesis in the interstellar medium?
  • What is the density, temperature, and ionization state of the interstellar gas, and the strength and direction of the interstellar magnetic field?
  • What processes control the ionization state, heating, and dynamics of the interstellar medium?
  • How much interstellar matter is in the form of dust and where did it originate?
  • What are the properties of interstellar neutral gas and dust that penetrate into the heliosphere?
  • How much greater are low-energy (‹ 100 MeV) cosmic ray (both ACR and GCR) nuclei and electron intensities outside the heliosphere?
  • What are the spectra of galactic cosmic rays in the local interstellar medium ranging from H to Fe as well as electrons and what is their relation to galactic gamma ray and radio emission?
  • Where in the galaxy are cosmic rays being accelerated?

Relevant Webinars

Into the Unknown Local Interstellar Cloud

Interstellar Dust Grains: Galactic Messengers (December)

Possibilities for Planetary Science and Astrophysics

The solar system was formed from a collapsing nebula of dust and gas, where gravitational accretion and collisions formed rocky asteroids, icy comets, and Kuiper Belt Objects (KBO) in the protoplanetary disk (PPD), then planets and moons as many of these objects merged and accreted further. The relic planetesimals of this era of formation in the first 100 Myr, i.e. the small bodies that didn't become planets & moons, were relegated to the asteroid and Kuiper Belts and Oort Cloud. Further sculpting and diminution of these relic populations occurred as the planets migrated and scattered most of the remnants to produce the belt substructures we see today. During all of these processes – planetary formation, planetesimal scattering, relic body evolution – secondary dust from the bodies was created due to impacts, grinding, and sputtering. Much of this dust is emitted into circum-solar orbits, creating and supplying the solar system's debris disk. This disk extends from inside the orbit of Mercury (the so-called "F-ring") to the heart of the Kuiper Belt (as recently detected by New Horizons, Poppe+2019). Similar debris disks have been observed around thousands of other stars, and similarly hold immense amounts of information on how exoplanetary systems form and evolve. However, almost nothing is known about the large-scale structure of our own circum-solar debris disk since we live inside it and foreground emissions obscure its overall structure. Therefore, there is no local ground truth for the critical interpretation of other circumstellar disks. By implementing a relatively simple, low mass and power dust detector and infrared camera instrument suite onboard an interstellar probe, the 3D structure of the debris disk can be captured and remove the bottleneck in our understanding of planetary system formation and evolution.

The recent New Horizons flybys of Pluto, its small moons, Charon, and Arrokoth revolutionized our knowledge about dwarf planets and planetesimals in the Kuiper belt. Surprisingly, dwarf planets and moons such as Pluto and Charon are or were ocean worlds and are or were potentially habitable. Just as planetary flybys in the inner and middle solar system revealed our first views of planets, moons, and asteroids, an interstellar probe could allow us to have the exhilarating third (and potentially fourth and fifth) flybys of a KBO planet or planetesimal ever accomplished. Such first-order exploration would reveal the astronomical and geological processes shaping the Kuiper belt and the diversity of worlds it hosts.

Letter to Dwarf Planet Observers

Relevant webinars

Possibilities for Planetary Science and Astrophysics

Just as the Cosmic Microwave Background (CMBR) contains huge amounts of diagnostic information that has allowed us to revolutionize our understanding of the Big Bang and the era of our Universe's formation, the Cosmic Infrared Background (CIBR) contains huge amounts of diagnostic information about the era of galaxy formation. However, the light from the nearby relic debris disk dust, (aka the "Zodiacal" cloud or "Zody") not only obscures its larger structure, but completely overwhelms the remnant light in the diffuse cosmic backgrounds produced in the time when galaxies first formed. This may be the biggest stumbling block in experimental astrophysics today since it leaves theories of galaxy and stellar formation without any constraints. An interstellar probe carrying a simple IR mapping spectrometer to outside the Zodiacal cloud (i.e. well outside its relic planetesimal source regions in the Main Asteroid Belt and the Kuiper Belt) would thus eliminate the local foreground Zody emissions and help unveil the early universe of the first stars and galaxies by making the first truly unobscured CIBR measurements.

Relevant webinars

Possibilities for Planetary Science and Astrophysics

Science Traceability Matrix Download (2 pages)

Traceability Matrix Page 1 Traceability Matrix Page 2

Baseline and Augmented Model Payloads Download (2 pages)

Payload Page 1 Payload Page 2