Исследование подтвердило, что Юпитер активно выбрасывает ионы водорода в космос

A study published Wednesday in Nature Astronomy confirms for the first time that Jupiter is actively bleeding hydrogen ions into space — and that the same electric field which powers the planet's dazzling polar auroras is the engine doing the ejecting. The finding, led by Jian-zhao Wang of the Laboratory for Atmospheric and Space Physics at the University of Colorado Boulder, establishes a new mass-loss pathway from the solar system's largest planet and proposes a mechanism that almost certainly operates at every strongly magnetized world in the universe, from Earth to Neptune and beyond. What Juno Actually Did That Telescopes Never Could For 36 years, scientists tracked Jupiter's hydrogen ions the only way they could: by watching the infrared light those ions emit from afar. Telescopes on the ground, Hubble, and more recently the James Webb Space Telescope have all detected the glow of trihydrogen cations — molecular ions written as H₃⁺ and consisting of three hydrogen nuclei sharing two electrons — shining from Jupiter's polar auroral zones. Those light-based observations are inherently limited: they capture signals averaged along the entire line of sight through the atmosphere, giving no information about whether individual ions are moving, where they are going, or how fast. What the new study delivers is categorically different. Juno did not observe light. It flew physically into the auroral region and caught the ions themselves. The spacecraft's Jovian Auroral Distributions Experiment, known as JADE, is an instrument suite measuring particles directly — measuring ion energy and direction in place, inside the plasma. Its ion sensor (JADE-I) uses a time-of-flight versus energy-per-charge technique: by measuring how long a particle takes to travel a fixed distance in combination with its kinetic energy, the instrument can calculate the particle's mass with enough precision to distinguish H⁺ (a single proton), H₂⁺ (molecular hydrogen ion), and H₃⁺ (trihydrogen cation), which have mass-to-charge ratios of 1, 2, and 3 respectively. The ion sensor covers energies from 5 electron volts to 50,000 electron volts over a wide field of view, and rotates with the spacecraft to sweep all directions every 30 seconds. During multiple close passes of Jupiter — the tight, elliptical orbits the mission calls perijoves — JADE's ion sensor captured unambiguous H₃⁺ signatures directly inside the auroral zone above the northern polar region. The detections appeared in distinct bursts, not continuously, associated with specific structures in the polar electric current system. Crucially, the measured upward velocities of those bursts exceeded Jupiter's escape speed — the velocity above which a particle will never return to the planet. The Two Stages That Carry Hydrogen Ions to Freedom Jupiter's escape velocity at auroral altitudes above its ionosphere is approximately 60 km/s (37 mph). That is a formidable barrier for a molecular ion originating in the cold upper atmosphere. The Wang et al. paper proposes that the escape unfolds in two stages, both driven by the unique electromagnetic environment above Jupiter's upward auroral current region — the structure scientists call Zone I. Stage one — wave heating. Deep in Zone I, energetic electrons stream downward from the magnetosphere. These electrons, carrying energies from roughly 10,000 to 100,000 electron volts, interact with the local plasma through a process called Landau resonance, generating ion cyclotron waves at the specific frequencies that resonate with H⁺, H₂⁺, and H₃⁺ ions. Through resonant wave interaction, the ions absorb energy across the magnetic field — perpendicular to the field lines — gaining momentum in the direction transverse to the direction they need to travel to escape. This perpendicular kick is the critical first step: without it, cold ionospheric ions cannot reach the higher-altitude electric potential structures that could accelerate them along the field. An independent paper published in Geophysical Research Letters in May 2026 by Skinner et al. confirmed that H₃⁺ ion cyclotron waves are present in Jupiter's Zone I, consistent with exactly this process, and found that the phenomenon involves multiple ion species simultaneously. Stage two — the electric field that makes the aurora also makes the escape. Above the ionosphere, a large quasi-static electric potential structure — a difference in voltage between high and low altitudes along the magnetic field — powers Jupiter's aurora by accelerating electrons downward into the atmosphere, where they collide with hydrogen molecules and produce the ultraviolet and infrared light visible from Earth. That same potential, oriented along the field lines, also acts on upward-moving positive ions: it accelerates them in the opposite direction, outward, providing the final push that brings H₃⁺ ions above escape velocity and sends them permanently into the surrounding magnetosphere. This symmetry — the aurora-making field doing double duty as the ejection engine — is the paper's most elegant finding. The estimated outflow rate is on the order of 10²⁶ ions per second, which the study places as one contribution to a broader system of plasma exchange between Jupiter's ionosphere and its vast magnetospheric environment. Juno's Waves instrument — the spacecraft's radio and plasma wave sensor — provided independent corroboration in the same perijove datasets: it detected ion cyclotron wave signatures consistent with H₃⁺ in the outflow region, giving the study a second instrumental line of evidence separate from the particle detection. What H₃⁺ Is and Why It Matters The trihydrogen cation was first identified by J.J. Thomson in 1911 during experiments on hydrogen plasma discharge, when he noticed a species with a mass-to-charge ratio of 3 that grew stronger in pure hydrogen gas. For most of the twentieth century it was considered a chemical curiosity — too reactive to survive in ordinary environments, stable only in the low-temperature, low-density conditions of interstellar space, where it serves as the starting point for a vast chain of chemical reactions building larger and more complex molecules. Its presence in planetary atmospheres was first confirmed at Jupiter in 1989, when Pierre Drossart at the Paris Observatory and Steve Miller at University College London detected its infrared emission in the auroras. Saturn and Uranus followed. Then in March 2025, a team using the James Webb Space Telescope detected H₃⁺ at Neptune — the last of the four giant planets — for the first time, completing the picture of H₃⁺ as a universal feature of the outer solar system's strongly magnetized worlds. In Jupiter's ionosphere, H₃⁺ is produced most efficiently in the auroral zones, where energetic electrons raining down from the magnetosphere ionize molecular hydrogen (H₂ + H₂⁺ → H₃⁺ + H, or through direct electron impact on H₂). Once formed, H₃⁺ regulates ionospheric temperature and electrical conductance — acting, in researchers' terminology, as a "thermostat" by efficiently radiating excess energy as infrared light. Same Physics as Earth, Different Scale The polar wind — the continuous outflow of ionospheric plasma from a planet's polar regions — was first predicted theoretically in 1968 by Axford and separately by Banks and Holzer. It was subsequently observed at Earth directly using satellite measurements, confirming that light ions (hydrogen and helium) stream supersonically outward along open magnetic field lines from the polar ionosphere into interplanetary space, carrying away atmospheric material over geological timescales. The mechanism is the same one Wang et al. document at Jupiter. But Jupiter's magnetic field is roughly 20,000 times stronger than Earth's in terms of the volume it controls, and its auroral power is hundreds of times greater. The Wang et al. result establishes that the two-stage acceleration process — perpendicular wave heating followed by parallel electric field acceleration — scales from Earth's relatively modest conditions to the most magnetically intense environment among the solar system's planets. That scaling argument is the paper's largest implication: no strongly magnetized planet, wherever it orbits in the galaxy, is immune to this form of ionospheric mass loss. The mechanism is not a Jupiter peculiarity; it is a fundamental property of how magnetospheres and ionospheres interact under intense auroral forcing. What Comes Next for Saturn, Uranus, and Neptune The Wang et al. paper argues explicitly that the H₃⁺ escape mechanism documented at Jupiter may operate at all strongly magnetized planets in the outer solar system. Saturn and Uranus both have substantial H₃⁺ auroral emission and well-documented auroral current systems. Neptune, where JWST's 2025 discovery confirmed H₃⁺ for the first time, is a particular focus: its magnetic field geometry is highly unusual (tilted roughly 47 degrees from its rotation axis and significantly offset from the planet's center), which may produce distinctive patterns of ionospheric escape that differ from Jupiter's more regular configuration. The measurements at Jupiter also begin to quantify a contribution to magnetospheric plasma that was long suspected but never confirmed: the ionosphere as a direct source of ions for the inner magnetosphere. Jupiter's magnetosphere is dominated by plasma sourced from Io's volcanic sulfur and oxygen, but lighter species including H⁺ and now confirmed H₃⁺ from the ionosphere itself may account for a meaningful fraction of the plasma population at smaller distances from the planet. The Juno mission, now well into its extended phase with more than 57 close Jupiter passes completed, continues collecting data. The mission includes the University of Colorado Boulder, Princeton University, Southwest Research Institute, the University of Minnesota, Lancaster University, the University of Liège, and Johns Hopkins Applied Physics Laboratory among its science team institutions. The Waves instrument data and the JADE data used in the Wang et al. study are publicly available through NASA's Planetary Data System, and derived datasets and code have been deposited on Zenodo. Frequently Asked Questions What exactly did Juno detect at Jupiter? Juno's JADE ion sensor physically flew through Jupiter's polar auroral region and directly measured trihydrogen cation (H₃⁺) ions — molecular ions consisting of three hydrogen nuclei — moving upward at velocities exceeding Jupiter's escape speed. This is the first time any spacecraft has detected H₃⁺ in motion, as an escaping plasma, inside the environment where the ion is produced. All prior knowledge of H₃⁺ at Jupiter came from infrared light observations made from a distance, which cannot reveal the motion or escape of individual ions. How is Jupiter's aurora connected to hydrogen leaking away? The electric field structure above Jupiter's auroral polar region — the same quasi-static voltage difference that accelerates electrons downward into the atmosphere to produce the aurora — also pushes positively charged ions in the opposite direction: upward and outward along the magnetic field. Combined with a first-stage process in which plasma waves heat the ions perpendicular to the field, giving them the initial energy boost they need to reach the electric field structure at higher altitudes, this two-stage mechanism carries H₃⁺ ions to escape velocity and sends them permanently into the surrounding magnetosphere. Can this happen at other planets? The paper proposes that the same mechanism — ion cyclotron wave heating plus field-aligned electric potential acceleration — should operate at any planet with a strong enough magnetic field to sustain the auroral current system that drives both processes. Saturn and Uranus both have H₃⁺ in their auroras and are likely candidates. In March 2025, the James Webb Space Telescope detected H₃⁺ at Neptune for the first time, making it the fourth solar system giant planet confirmed to host the ion — and therefore a potential candidate for the same escape pathway, pending in-situ measurement. Earth's own polar wind operates on related physics, though at far lower magnetic-field intensities. Why does this matter if Jupiter is not losing its atmosphere noticeably? Jupiter is massive enough that the H₃⁺ outflow rate documented here represents a physically significant but not catastrophic mass loss over human timescales. The importance is twofold. First, the ionosphere has now been confirmed as a direct plasma source for Jupiter's inner magnetosphere — something previously suspected but unverified. Second, the finding establishes a measurement technique and a confirmed physical mechanism that can be applied to future spacecraft visiting Saturn, Uranus, Neptune, or strongly magnetized exoplanets orbiting other stars, where atmospheric retention is a central question for understanding whether those worlds could support liquid water or life. ⓒ 2026 TECHTIMES.com All rights reserved. Do not reproduce without permission.