
IMAP-Ultra captures images of very energetic neutral atoms, particularly hydrogen (H) atoms, produced in the solar system at the The place where the solar wind slows down and begins to interact with the interstellar medium. The heliosheath has a few parts: the termination shock (the innermost part of the boundary), the heliopause (the outermost part of the boundary), and the part in between the inner and outer boundary., the region where the A stream of charged particles, mostly protons and electrons, that escapes into the Sun's outer atmosphere at high speeds and streams out into the solar system in all directions. slows, compresses, and becomes much hotter as it meets the interstellar medium (ISM). Approximately every three months, The IMAP-Ultra instrument consists of an identical pair of imagers that collect, count, measure, and map energetic neutral atoms (ENAs) of energies from 5-40 kiloelectronvolts (keV.) Ultra consists of two identical instruments that are positioned on opposite sides of the spacecraft at different angles. Together, the Ultra pair will be able to image the entire celestial sphere. produces detailed images that cover more than 50% of the The bubble-like region surrounding the solar system inflated by the solar wind, shielding the solar system from interstellar radiation., providing new understanding about how Charged particles (electrons, protons, and ions) that are moving very fast (high energy). If the particles originate at the Sun, they are known as Solar Energetic particles (SEPs). and pressures at the edge of the solar system and beyond vary over A measure of the flow of events. to form our own heliospheric bubble.
IMAP-Ultra’s measurements complement those of IMAP-Lo and IMAP-Hi, providing a high-resolution comprehensive map of the origins and energies of the collected heliospheric particles and energies.
IMAP-Ultra design and assembly is led by John Hopkins APL.