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The heliopause is the boundary separating the predominantly solar-wind plasma of the heliosphere from the surrounding interstellar plasma. It is set by the interaction of flows, magnetic fields and pressure, rather than by a fixed spherical surface. It differs from the termination shock, where the solar wind slows abruptly inside the heliosphere.

Voyager 1 supplied a direct test. Plasma-wave oscillations observed in 2013 indicated a much greater local electron density, supporting a retrospective crossing in August 2012. Because the characteristic plasma frequency depends on the square root of electron density, the observed oscillation frequency served as a density diagnostic.^[ref]

The heliosheath, usually meaning the inner heliosheath, is the region of shocked solar wind between the termination shock and the heliopause. Solar wind plasma entering it has been slowed and compressed, and its flow turns as it approaches the boundary with the interstellar medium. The termination shock and heliopause are different boundaries: crossing the shock does not yet mean leaving solar-wind material.

The Voyager 2 plasma experiment provided direct measurements around several shock crossings between 30 August and 1 September 2007. The observed thermal plasma was cooler than a simple picture of complete conversion of the incoming flow energy into thermal-ion heat would suggest. The researchers inferred that much of the energy instead went into pickup ions or other energetic particles.^[ref]

The instrument used four Faraday cups, three facing approximately into the flow. Currents recorded at different particle energies and viewing directions were fitted with moving Maxwell-Boltzmann velocity distributions to estimate proton temperatures. This measures a selected part of the particle population; it does not directly measure all the energetic ions that may carry the remaining energy.^[ref]

The heliosphere is the region of space dominated by the solar-wind plasma and its carried magnetic field as they interact with the interstellar medium. The solar wind slows at the termination shock and encounters the interstellar plasma at the heliopause.

This is a plasma-interaction boundary, not the outer reach of the Sun's gravity or light. Voyager observations combine particle, magnetic-field and plasma-wave measurements to diagnose the transition. An increased local electron density outside the heliopause supplied an important independent diagnostic, illustrating why a boundary cannot always be identified from one field direction alone.^[ref]

The termination shock is the transition where the expanding solar wind slows from supersonic flow into the slower, compressed and heated flow of the outer heliosphere. It forms because the outward flow encounters pressure from its surroundings. It is distinct from the farther-out heliopause, where solar-wind plasma meets the interstellar plasma.

A shock wave converts organized flow kinetic energy into thermal and nonthermal particle energy. A spacecraft can therefore identify a crossing through changes in the magnetic field, plasma and energetic-particle populations, rather than through a visible solid boundary. Voyager 1 crossed the termination shock on 16 December 2004 near 94 astronomical units from the Sun. Its magnetic-field and particle instruments supplied evidence for entering the heliosheath.^[ref] The original particle report found enhanced low-energy protons but no local maximum of anomalous cosmic ray helium, illustrating why detecting a shock and explaining all particle acceleration are separate questions.^[ref]

Voyager 1 is a spacecraft launched on 5 September 1977 to investigate the outer Solar system. It flew past Jupiter in March 1979 and Saturn in November 1980, then continued outward on an extended mission to study the environment beyond the planets.^[ref]

On 25 August 2012 it crossed the heliopause, the boundary between the solar wind-dominated heliosphere and the surrounding interstellar medium. This boundary concerns the plasma environment; it is not a boundary beyond which the Sun's gravity vanishes. Its scientific instruments include detectors of charged particles, a magnetometer and a Voyager plasma-wave instrument. Together, measurements of particles, magnetic fields and plasma waves allow a moving probe to investigate a remote environment that cannot be sampled in a terrestrial laboratory.^[ref]

Voyager 2 is a robotic spacecraft launched on 20 August 1977 to investigate the outer Solar system. Its encounters with Jupiter in 1979, Saturn in 1981, Uranus in 1986 and Neptune in 1989 made one mission a comparative study of four giant planets. A gravity assist changes the spacecraft's trajectory and energy relative to the Sun by exchanging momentum with a moving planet, allowing a sequence of encounters that would require much more onboard propulsion if accomplished by engine firings alone.^[ref]

Voyager 2 later sampled the transition from the solar wind to the surrounding interstellar plasma. On 5 November 2018, its plasma instrument recorded a steep decline in the outward solar wind flow. The instrument inferred plasma properties from electrical currents collected from particles arriving in different directions. Changes in energetic-particle measurements supplied independent evidence: particles associated with the heliosphere declined while galactic cosmic rays became more prominent. The combined observations identify the heliopause crossing, rather than defining the boundary by a predetermined distance.^[ref]

This is a moving-laboratory experiment: the apparatus travels through regions that cannot be sampled from Earth, while several instruments test the interpretation of a sharp change. Crossing the heliopause means leaving the region dominated by the Sun's outward-flowing plasma; solar gravity does not suddenly end there. The crossing date and the December announcement date are different events.

The Voyager plasma-wave instrument measures fluctuating electric fields associated with plasma waves. Its original design combines a multichannel spectrum analyser with a wideband waveform receiver, making both frequency content and selected time-domain waveforms available.^[ref]

When an observed feature is identified with electron plasma oscillations, its frequency constrains electron number density through $f_p=(2\pi {)}^{-1}\sqrt{n_e{e}^2/({\epsilon }_0{m}_e)}$. Thus a fourfold density increase doubles the characteristic frequency. Wave identification, instrument calibration and the surrounding plasma conditions enter the inference. On Voyager 1, such measurements have provided local information about plasma beyond the heliopause.^[ref]