SERENA-HEWG meeting, Santa Fe, May, 2008

Hermean environment (from Milillo et al., SSR, 2005) SERENA-HEWG meeting, Santa Fe, May, 2008

NASA-MESSENGER SERENA-HEWG meeting, Santa Fe, May, 2008 The environment is one of the high-priority scientific target of the mission:  What is the nature of Mercury's magnetic field?  What are the unusual materials at Mercury's poles?  What volatiles are important at Mercury? MESSENGER’s instruments devoted to the environment are: Magnetometer (MAG) Energetic Particle and Plasma Spectrometer (EPPS) Mercury Atmospheric and Surface Composition Spectrometer (MASCS) X-Ray Spectrometer (XRS)

ESA-JAXA BepiColombo The mission has among its major scientific objectives  Determination of the composition, origin and dynamics of Mercury's exosphere and polar deposits and  Investigation of the structure and dynamics of Mercury's magnetosphere. SERENA-HEWG meeting, Santa Fe, May, 2008 BepiColombo is composed by two spacecraft: the MMO is completely devoted to environment, while MPO has different instruments devoted to the environment.

Instrument for environment SERENA-HEWG meeting, Santa Fe, May, 2008 InstrumentTarget MERMAG MPO/MAG Vector magnetic field (accuracy 10 pT and time res. up to 128 Hz) MMO/MGF MMO/PWI EWO(OFA/WFC/EFD) SORBET AM 2 P WPT MEFISTO LF-SC DB-SC dc electric field, plasma waves, radio waves *electric field (DC~10MHz) *magnetic field (0.1Hz~640kHz) *electron density and temperature MMO/MPPE MEA, HEP-ele, MIA, MSA, HEP-ion, and ENA electrons (3eV-30keV, keV), ions (5eV/q-30keV/q, 5eV/q-40keV/q, 30keV-1.5MeV), and energetic neutral atoms (<25eV-3.3keV) MPO/SERENA ELENA ENA ( eV) (2°x2° ang. res., 10% velocity res.) STROFIO Neutral atoms (60 M/DM mass res.) MIPA Ions (10 eV-15keV) (Energy and ang. res. Rough mass res.) PICAM Ions (10 eV-3keV) (variable energy and ang. res., 100 M/DM mass res.) MPO/PHEBUS Exospheric emission between 55 nm and 315 nm (spectral res. between 1 and 1.5 nm) MMO/MSASI dayside Na emission (spectral resolution ( /  ) is ~90,000, field of view 30°) MMO/MDM Dust impact momentum, speed, direction, and the number of impacts MPO/SIXS X-ray (spectral range: ~ 1 keV -20 keV; including X-ray flare parameters), protons (spectral range: ~ MeV) and electrons (spectral range: ~ 100 keV – 3 MeV) MPO/MIXS MIXS-C MIXS-T X-ray fluorescence ( keV range) MPO/SIMBIO-SYS STC stereo global mapping (50 m spatial res. at 400 km altitude) HIRC high spatial res. mapping of selected areas (5 m spatial res. at 400 km altitude) VIHI global mineralogical mapping (spectral res  m; <500 m spatial res.) and compositional characterization of selected areas (100 m spatial res.) MPO/MERTIS global mineralogical mapping: spectrometer channel (spectral range 7-14μm, spectral res. < 200nm) radiometer channel (spectral range up to 40 μm).

HEWG - Padova, 29 September, 2006 Energetic Neutrals Planetary Surface EXOSPHERE INTERPLANETARY SPACE Solar wind Low-Energy Neutrals Magnetospheric Ions Energetic Neutrals MPO/SERENA MPO/PHEBUSMMO/MPPEMPO/MIXS MPO/SimbioSys MAGNETOSPHERE MPO/SIXS MPO/SERENA MPO/MERTISMMO/MSASI Electromagetic fields MPO/MAG MMO/MGF MMO/MDMMMO/PWI

A two spacecraft mission SERENA-HEWG meeting, Santa Fe, May, 2008 The inter-instrument collaborations planned onboard each spacecraft and the opportunities afforded to perform two-point simultaneous measurements at Mercury constitute exciting features of the mission. A 1:4 resonant orbit configuration for the two spacecraft is currently considered so that the closest approach between the two satellites will be a few 1000 km. Before that during the first two weeks in orbit, the two spacecraft will have a few close encounters

SERENA-HEWG meeting, Santa Fe, May, 2008

The Solar wind and IMF at Mercury SERENA-HEWG meeting, Santa Fe, May, 2008 The Parker spiral forms an angle of about 20° with the solar wind radial direction, less than half of the value at the Earth’s orbit (~45°); this implies a change of the relative ratio of the Interplanetary Magnetic Field (IMF) components with respect to the near-Earth conditions, and an increase of the weight of the IMF B x component. The average solar wind density is about ten times higher than that at the Earth, but this value varies considerably due to the high eccentricity of the orbit of the planet (from 32 cm -3 to 73 cm -3 ). B The IMF intensity changes by a similar factor. Which are the effects of these different conditions? Bv v

Mercury has an internal magnetic field SERENA-HEWG meeting, Santa Fe, May, 2008 The Mariner 10 observations seem to proove the existence of an internal dipolar-like magnetic field (Ness et al, 1975). The estimated dipole moment ranges between 284 and 358 nT R M 3, Nothward oriented, (confirmed by recent MESSENGER results). Hermean magnetosphere is only 5% of that of the Earth. In a zero order analysis, the spatial dimensions must be scaled by a factor of ~7. (Milillo et al, 2005)

Typical scale magnitudes. SERENA-HEWG meeting, Santa Fe, May, 2008 k map at the magnetopause (Massetti et al., 2006) The time scale variations of the magnetospheric processes are few minutes at Mercury (compared with 1 hour at the Earth) The field variation length scale of the Hermean magnetosphere is comparable to the gyroradii of the heaviest ions. Adiabaticity parameter < 3 in the cusp regions where the B field is lower; thus, the SW can enter in a non- adiabatic manner inside the magnetosphere (Massetti et al., 2006) Effects of the ExB drift paths curvature are no more negligible (Delcourt et al., 2002)

Direct entry through the cusps SERENA-HEWG meeting, Santa Fe, May, 2008 The IMF orientation and intensity and the weak internal magnetic field of Mercury likely produce a direct entry through the cusps inside the Hermean dayside magnetosphere. Solar wind plasma circulates inside the magnetosphere and eventually may hit the surface. (Mura et al, 2005) (Kallio et al, 2008) (Kallio et al, 2003)

SERENA-HEWG meeting, Santa Fe, May, 2008 SW precipitation: high SW pressure (Kabin et al., 2000) Extreme events produce precipitation in the whole dayside hemisphere (Kallio and Janhunen, 2003) (V sw = 860 km/s)(V sw = 1100 km/s) The observations of SEPs from the Sun by MPO/SIXS could provide a useful index for a kind of near-real-time forecast of solar activity that could be used to alert other MPO instruments, such as SERENA, MIXS and PHEBUS (which aim to evaluate the planet’s response to solar disturbances)

SERENA-HEWG meeting, Santa Fe, May, 2008 Dayside coordinated measurements 1 MPPE SERENA SIXS MGF MAG PWI Joint measurements of MPPE-MEA and MIA, MGF and PWI, on the MMO spacecraft and SIXS, SERENA-MIPA and PICAM and MAG on the MPO spacecraft, will confirm plasma penetration inside the magnetosphere.

SERENA-HEWG meeting, Santa Fe, May, 2008 (Mura et al, PSS, 2005) SW Plasma circulation inside the magnetosphere (Mura et al., 2005)

Energetic electrons flow inside the magnetosphere SERENA-HEWG meeting, Santa Fe, May, 2008 Energetic electron fluxes are registered by Mariner 10. Are they magnetic fluxes as observed during substorms at the Earth or direct solar wind coupling? Are there also solar wind protons and heavy ions of planetary origin circulating inside the Hermean magnetosphere? Is any ionosphere present there? Dipolarization event ? (Christon et al, 1986)

SERENA-HEWG meeting, Santa Fe, May, 2008 SERENA MGF MAG MPPEPWI First the magnetic field measurements of MMO/MGF and MPO/MAG will register signatures of stretching and dipolarization of the magnetic field lines as well as disturbances related to magnetotail reconnection plasmoids, and field-aligned currents. Also, the ion and electron sensors of MMO/MPPE will provide important information about the time-scale of substorms, carriers of field-aligned currents and the effects of heavy ions. Plasma injections will be monitored at two points, MMO/MPPE and MPO/SERENA, during its evolution. To catch a substorm event by two spacecraft in the night-side magnetosphere

SERENA-HEWG meeting, Santa Fe, May, 2008

Oxygen H, He, and O were detected in the atmosphere by the onboard UV spectrometer (Broadfoot et al., 1974). Later, Na, K, and Ca were detected through ground-based observations (Potter and Morgan, 1985, 1986; Bida et al., 2000). SERENA-HEWG meeting, Santa Fe, May, 2008 The small amount of observed atmospheric oxygen relative (< cm -3 ) relative to the surface stoichiometry (≈50%) may indicate that atmospheric oxygen is bound in molecules, or it may indicate inefficient release (Morgan and Killen, 1997), or it may efficiently charge exchange with solar wind and magnetospheric protons. Exosphere

Sodium and Potassium observations SERENA-HEWG meeting, Santa Fe, May, 2008 (Killen et al. SSR, 2007) The mid latitudes intensification of exospheric Na and K seems to be related to solar wind precipitation through the cusp. Another possible explanation is the association of Na and K with radar and visible bright spots on Mercury's surface (Sprague et al. 1998; Sprague and Massey 2007). However, the images of Na emission obtained from 1997 to 2003 by Potter et al. (2006) showed no evidence of a topographic effect.

Calcium The neutral Calcium was observed by Bida et al. (2000). It is likely that Ca is released in the molecular form, possibly as CaO. If so, CaO could be dissociated in the atmosphere, for instance by Ly  photons, giving the Ca atom excess energy as observed (Killen et al., 2005). SERENA-HEWG meeting, Santa Fe, May, 2008

Sodium observations variability tail Dawn-dusk asymmetries SERENA-HEWG meeting, Santa Fe, May, 2008 (Schleicher et al. A&A, 2004) (Potter et al., 1999) (Potter et al., 2002)

SERENA-HEWG meeting, Santa Fe, May, 2008 Exospheric coordinated measurements MSASI PHEBUS The exospheric configuration and composition will be measured by MPO/PHEBUS, and MMO/MSASI and MPO/SERENA-STROFIO in terms of column density, composition and profile variations. STROFIO, in particular, will be the only instrument able to determine the night side exospheric composition. SERENA

SERENA-HEWG meeting, Santa Fe, May, 2008 Dayside coordinated measurements 2 SERENA MIXS PHEBUS Together with plasma penetration measurements described above, other dedicated instruments will observe the response of the planet in term of radiation and particles release. MIXS will observe the X-Ray emission of planetary aurorae while SERENA-ELENA will monitor the emission of neutral atoms. SERENA-STROFIO and PHEBUS and MSASI will observe the exospheric response of Mercury in terms of column density, composition and profile variations. MSASI

Remote sensing the surface properties from exospheric measurements SERENA-HEWG meeting, Santa Fe, May, 2008 Due to the strong link between the exosphere and the surface it is possible by measuring neutrals and ions at relatively low altitudes to obtain information regarding the composition of the upper surface of the regolith. However, some release processes are non-stoichiometric and involve only selected species. Eventually, to be able to successfully infer a source composition from exospheric measurements, it is really important to know the mechanism of ejection and the properties of the particular surface.

Particle release processes invesigation SERENA-HEWG meeting, Santa Fe, May, 2008 TD PSD IS MIV (Environment Simulation Tool (EST) at IFSI)

Ion sputtering analysis SERENA-ELENA will produce a kind of mapping of ion sputtering action on the surface of the planet ( Orsini et al ). SERENA-HEWG meeting, Santa Fe, May, 2008 This measurement correlated with the observation of ion flux to the surface seen by MPO/SERENA-MIPA will provide the surface efficiency in particle releasing via IS

SERENA-HEWG meeting, Santa Fe, May, 2008 Impulsive event (meteoroid 0.1 m) Frequency ~ 2 events/day (Marchi et al., 2005) Duration ~ min Amplitude ~ 2000 km (Mangano et al., 2007)

SERENA-HEWG meeting, Santa Fe, May, 2008 MPO/SERENA Planetary Surface MPO/PHEBUSMPO/MIXS EXOSPHERE Surface signature in the environment nearby the surface: MPO/SimbioSys MMO/MSASI MPO/MERTIS The surface elemental abundances mapped by MIXS, the surface mineralogy mapped by MERTIS and the surface cratering mapped by SIMBIO-SYS will allow released exospheric atoms to be related to the constitution of the surface. MMO/MDM

Exo-ionosphere The photo-ionisation of exospheric atoms creates an ionised thermal plasma population, especially on the dayside. Confirmed by MESSENGER observation. (Leblanc et al., 2004) SERENA-HEWG meeting, Santa Fe, May, 2008 The ions produced at thermal energies are energised and become part of the magnetospheric ion populations. Part of this plasma is eventually lost to the SW.

The close-to-planet observations of SERENA-PICAM will provide the composition and velocity distribution of planetary ions. Electron and ion phase space densities by MPPE-HEP-e and MEA can be obtained at different distances from the planet. Magnetic fields observations at two vantage points by MAG and MGF and of the electric fields (PWI) will complement the measurements of particle dynamics and currents (Delcourt et al., 2003) Planetary ions circulation SERENA-HEWG meeting, Santa Fe, May, 2008 MPO/SERENA MMO/MPPEMMO/PWI

BepiColombo: an outstanding tool for Hermean environment investigstion SERENA-HEWG meeting, Santa Fe, May, 2008 Co-ordinated measurements made by different onboard instruments will answer important key questions regarding the planet’s environment. The opportunity offered by the BC mission to perform two-point simultaneous measurements provides a powerful and unique investigative tool at a location other than the Earth. The interaction processes acting at Mercury are present also in other interplanetary environments. For example, the plasma-surface interaction is present wherever a body in the Solar System lacks an atmosphere (Moon, asteroids, Jupiter’s satellites and many other satellites of the giant planets).

SERENA-HEWG meeting, Santa Fe, May, 2008