MPO Scientific Aspects BepiColombo – Mission to Mercury MPO Scientific Aspects & System Update Rita Schulz Johannes Benkhoff

BepiColombo Elements

Mercury Planetary Orbiter Mercury Magnetospheric Orbiter MPO orbit optimized for study of planet itself MMO orbit optimized for study of magnetosphere

Mercury Orbits MMO: 400 x 11,800 km 9.3 hours Direction of Sun at perihelion MPO:

Scientific Objectives Origin of Mercury Evolution of Mercury MPO Instruments (Selected by SPC; Nov. 2004) & Scientific Objectives Nature of surface modifications on Mercury Structure and variability of the magnetosphere of Mercury

BELA BepiColombo Laser Altimeter CoPI’s: N. Thomas / T. Spohn Science Goals Figure of the Planet Interior Structure and Composition of Mercury Formation and Evolution of the Planet

MERCURY (RADIOMETER and) THERMAL INFRARED SPECTROMETER MERTIS MERCURY (RADIOMETER and) THERMAL INFRARED SPECTROMETER PI: E.K. Jessberger Science goals: to study the surface composition of Mercury to identify the key rock-forming minerals to map the surface mineralogy to measure surface temperature and thermal inertia

Mercury Imaging X-ray Spectrometer (MIXS) PI: S. Dunkin To produce global elemental maps of key rock-forming elements To perform high spatial resolution mapping of these elemental abundances where solar conditions permit To confirm that the auroral zone is an intense source of continuum and line X-rays

SIXS (Solar Intensity X-ray and particle Spectrometer) PI: J. Houvelin Scientific Objectives accurate physical estimates of solar X-ray and particle irradiation at the surface of Mercury. Data provided by SIXS are mandatory for a valid fluorescence analysis of MIXS spectra.

(ITALIAN SPRING ACCELEROMETER) ISA (ITALIAN SPRING ACCELEROMETER) PI: V. Iafolla AN ACCELEROMETER TO MEASURE THE INERTIAL ACCELERATIONS ACTING ON THE MPO the global gravity field of Mercury and its temporal variations the local gravity anomalies the rotation state of Mercury the orbit of the Mercury center–of–mass around the Sun

MERMAG Magnetic Field Investigation PI: A. Balogh The primary objective to provide magnetic field measurements that will lead to the detailed description of Mercury’s planetary magnetic field, and thereby constrain models of the evolution and current state of the planetary interior. The secondary objective to contribute to the study of the interaction of the solar wind with the Hermean magnetic field and the planet itself, the formation and dynamics of the magnetosphere as well as to the processes that control the interaction of the magnetosphere with the planet.

PHEBUS: A FUV-EUV Spectrometer PI: E. Chassefiere 1) Vertical/ geographic/ seasonal mapping of already detected elements (H, He, O, Na, K, Ca). 2) Search for still non-detected compounds (Si, Mg, Al, Fe, S, C, N, OH, H2), and vertical/ geographic/ seasonal mapping. 3) Search for noble gases other than He (Ne, Ar, Xe, Kr) and mapping/ monitoring if possible. 4) Search for ion species (He+, Na+, O+, Mg+, Al+, Ca+, C+, N+, S+, …) and mapping/ monitoring if possible. 5) Measurement of surface reflectance at 121.6 nm in polar craters in order to search for surface ice layers.

PI: E. Flamini SIMBIO-SYS Spectrometer and Imagers for MPO BepiColombo Integrated Observatory SYStem SIMBIO-SYS SIMBIO-SYS package: It incorporates capabilities to perform: medium space resolution global mapping in stereo and colour imaging using two pan-chromatic and 3 broad-band filters Stereo Channel STC; high spatial resolution imaging in a pan-chromatic and 3 broad-band filters High Resolution Imaging Channel HRIC; imaging spectroscopy in the spectral range 400  2000 nm Visible Infrared Hyperspectral Imager VIHI . PI: E. Flamini Classification of Mercury surface features Mercury surface composition

SIMBIO-SYS Science Surface geology: stratigraphy, geomorphology Volcanism: lava plain emplacement, volcanoes identification Global tectonics: structural geology, mechanical properties of lithosphere Surface age: crater population and morphometry, degradation processes Surface composition: maturity and crustal differentiation, weathering, rock forming minerals abundance determination Geophysics: libration measurements, internal planet dynamics

PI: L. Iess MORE Mercury Orbiter Radio-science Experiment Scientific Objectives Determine the gravity field of Mercury Determine the size and physical state of its core Provide crucial experimental constraints to models of Mercury’s internal structure Test theories of gravity Measure the gravitational oblateness of the Sun Test and characterize the most advanced interplanetary tracking system ever built Assess the performances of the novel tracking system in precise orbit determination and space navigation. 

SERENA Search for Exospheric Refilling and Emitted Natural Abundances PI: S. Orsini Units: ELENA: Emitted Low-Energy Neutral Atoms STROFIO: Start from a ROtating FIeld spectrOmeter MIPA: Miniature Ion Precipitation Analyser PICAM: Planetary Ion CAMera

Mercury Gamma-ray and Neutron Spectrometer MGNS PI: I.G.Mitrofanov Scientific goals: to determine the elemental compositions by the measurements of nuclear lines of major soil-composing elements to determine the elemental compositions by the measurements of the leakage flux of neutrons and of the lines of natural radioactive elements to determine the regional distribution of volatile depositions on the polar areas of Mercury which are permanently shadowed from the Sun, and to provide a map of column density of this depositions

MGNS Backup: MANGA Mercury composition Analysis by Neutron and Gamma-ray spectoscopy PI: C. d'Uston

MPO Payload Selection by SPC (Nov. 2004) BELA Laser Altimeter N. Thomas / T. Spohn ISA Radio Science V. Iafolla Accelerometer MERMAG Magnetometer A. Balogh MERTIS IR Spectrometer E.K. Jessberger   MGNS or Gamma Ray and I. Mitrofanov MANGA Neutron Spectrometer C. d'Uston MIXS / X-ray Spectrometer S. Dunkin SIXS Solar Monitor J. Houvelin MORE Radio Science L. Iess Ka-band Transponder PHEBUS UV Spectrometer E. Chassefiere   SERENA Neutral Particle Analyser/ S. Orsini (Elena, MIPA, Ion Spectrometers PICAM, Strofio) SIMBIO-SYS High Res.+ Stereo Cameras E. Flamini (HIRC, STC, VIHI) visual and NIR Spectrometer

MPO Science Topics Instruments plus MMO Payload Surface Interior Morphology High Resolution Colour Camera Stereo Camera Vis-Near-IR Mapping Spectrom. TIR Map. Spectrom/Radiometer X-ray Spectrom/Solar Monitor γ-Ray Neutron Spectrometer Ultraviolet Spectrometer Neutral & Ion Particle Analyser Laser Altimeter Radio Science Experiment Magnetometer Surface Topography Composition Temperature State of Core Core/Mantle Interior Composition Magnetic Field Composition Dynamics Exosphere Surface Release Left panel is the sensitivity and antenna length of Geotail, Phobos-2, and Nozomi plasma wave instruments. Through the long wire antennas, we can survey the plasma space around the Mars in the finest level.  Right panel is the spectra observed by Nozomi around the Earth, if wire antennas were extended. PWA can catch all the important waves we expect. Source/Sink Balance Structure, dynamics plus MMO Payload Magnetosphere Composition Interactions