1. A. Milillo, S. Orsini and A. Mura (INAF/Institute of Space Astrophysics and Planetology) And the SERENA Team

2. SERENA - HEWG meeting, Rome, 13-17 May, 2013 Hermean environment (from Milillo et al., SSR, 2005)

3. SERENA - HEWG meeting, Rome, 13-17 May, 2013 SERENA Search for Exospheric Refilling and Emitted Natural Abundances NPA: ELENA investigates the Hermean escaping neutral gas (strongly linked to its surface), and the processes responsible of such a population. STROFIO investigates the exospheric gas composition. IS: PICAM investigates the exo-ionosphere extension and composition. MIPA investigates the plasma precipitation toward the surface of Mercury.

4. SERENA vs Hermean environment SERENA - HEWG meeting, Rome, 13-17 May, 2013

5. 1.Chemical and elemental composition of the exosphere 2.Neutral gas density asymmetries 3.Exo-ionosphere composition 4.Exo-ionosphere spatial and energy distribution 5.Plasma precipitation rate 6.Surface emission rate and release processes 7.Particle loss rate from Mercury’s environment Remote sensing of the surface composition Magnetosphere structure and dynamics Planetary response to SW variations ENA imaging applications for comparative solar- planetary relationship) Heavy ion sputtering products Primary scientific objectives of SERENA. Support to other Bepi experiments. Challenging goals. SERENA scientific objectives SERENA - HEWG meeting, Rome, 13-17 May, 2013

6. ELENA is a Time-of-Flight neutral atom detector which provides direction and velocity of neutral particles at energy >10 eV. ELENA SERENA - HEWG meeting, Rome, 13-17 May, 2013

7. ELENA Scientific Operations SERENA-ELENA will detect released particles from the surface of the planet ( Orsini et al. 2008 ) providing angular distribution and ToF spectra.

8. ELENA surface scanning SERENA - HEWG meeting, Rome, 13-17 May, 2013 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 ion sputtering and back-scattering The s/c motion will allow a mapping of released particles from the surface of the planet (Orsini et al. 2008).

9. Signal simulation for different sources BackscatteringCharge exchangeIon sputtering SERENA - HEWG meeting, Rome, 13-17 May, 2013

10. We have simulated the ELENA coverage of surface ion interaction by using different precipitation referenced models and cases: Kallio et al., 2003: Hybrid model Mura et al., 2005: Luhman model Massetti et al., 2007: Toffoletto- Hill model ELENA estimated outcomes

11. South IMF case Extreme event case Parker IMF case Kallio et al.

12. Precipitation derived after Schleicher et al. 2004 Observations Mura et al. South IMF case

13. IMF (-20, 0, -5) aphelion Massetti et al. IMF (-20, 0, -5) perihelion Extreme case IMF (-45, 16, -20) Nsw 120 cm -3

14. Mura et al., 2005 Mura et al., 2008 Kallio et al., 2003 Massetti et al., 2007 SERENA - HEWG meeting, Rome, 13-17 May, 2013 Estimated ENA distributions

15. ELENA coverage for a whole Mercury season with 1.a hypothetical uniform flux 2.uniform flux inside cusp projection

16. SERENA - HEWG meeting, Rome, 13-17 May, 2013 ELENA LT Coverage: Summer Autumn

17. SERENA - HEWG meeting, Rome, 13-17 May, 2013 ELENA LT Coverage: Winter Spring

18. SERENA - HEWG meeting, Rome, 13-17 May, 2013 ELENA Geographic Coverage: Summer Autumn

19. SERENA - HEWG meeting, Rome, 13-17 May, 2013 ELENA Geographic Coverage: Winter Spring

20. 2. uniform flux inside cusp projection ELENA LT Coverage: Summer Autumn

21. ELENA Coverage: Winter Spring

22. ELENA Geographic Coverage: Summer Autumn

23. ELENA Geographic Coverage: Winter Spring

24. SERENA-PDR, Rome, 2-3 December, 2008 Global charge-exchange ENA imaging from two vantage points MMO-ENA MPO-ELENA MPO close to the apoherm in the nightside

25. Summary of ELENA primary objectives SERENA - HEWG meeting, Rome, 13-17 May, 2013

26. STROFIO is a novel mass spectrograph that determines particle mass-per-charge (m/q) by a time-of-flight (ToF) technique. STROFIO concept SERENA - HEWG meeting, Rome, 13-17 May, 2013

27. STROFIO measures the in-situ neutral particles with low energies (exospheric particles) with good mass resolution. For details see Desai presentation…. Spectrum of H 2, He, Ne, N 2, Ar, O 2, CO 2 STROFIO Scientific Operations

28. Summary of STROFIO primary objectives SERENA - HEWG meeting, Rome, 13-17 May, 2013

29. MIPA (Miniature Ion Precipitation Analyser) is a simple ion mass analyser optimised to provide monitoring of the precipitating ions and to measure the main groups of ions present in the magnetosphere. To obtain a full measurement, a scanning in energy and in angle will be operated within a duty cycle less than 1 minute. MIPA scientific operations SERENA - HEWG meeting, Rome, 13-17 May, 2013

30. 2pi coverage total coverage sample pixel (1 of 24) Field of view of one MIPA pixel

31. SERENA - HEWG meeting, Rome, 13-17 May, 2013 MIPA Scientific Operations

32. SERENA - HEWG meeting, Rome, 13-17 May, 2013 PA distribution low-latitudesPA distribution high-latitudes precipitating (PA 90°) Example: IMF (–20, 0, –5) nT at aphelion SW inside the Mercury’s Magnetosphere

33. Summary of MIPA primary objectives SERENA - HEWG meeting, Rome, 13-17 May, 2013

34. PICAM is optimized to measure low energy ions. Its main objective is to detect and characterize the exo-ionosphere and thereby complete the analysis of the composition of ions released from the surface/exosphere and ionized in the Hermean environment. To obtain a full measurement, a scanning in energy will be operated within a duty cycle about 1 minute PICAM concept SERENA - HEWG meeting, Rome, 13-17 May, 2013

35. PICAM pixel SERENA - HEWG meeting, Rome, 13-17 May, 2013 PICAM was illuminated by an N 2 + ion beam at 1 keV, coming from 50° elevation from the top right azimuth.

36. SERENA - HEWG meeting, Rome, 13-17 May, 2013 PICAM mass analysis PICAM mass resolution is M/ΔM > 50 Simulations: M=39 and 40 AMU.

37. SERENA - HEWG meeting, Rome, 13-17 May, 2013 Na + density distribution (in Log 10 of Na + /cm 3 at TAA=150° in the equatorial plane) for average and idealysed solar wind conditions. Exo-ionosphere characterization

38. Summary of PICAM primary objectives SERENA - HEWG meeting, Rome, 13-17 May, 2013

39. SERENA operations vs phase

40. SERENA-HEWG meeting, Santa Fe, 12-14 May, 2008 SERENA objectives 1 and 2: STROFIO SERENA objectives 3 and 4: PICAM SERENA objective 5: MIPA SERENA objective 6: ELENA, MIPA and STROFIO SERENA objective 7: ELENA Winter and Summer dayside SERENA objectives

41. SERENA-HEWG meeting, Santa Fe, 12-14 May, 2008 SERENA objectives 1 and 2: STROFIO SERENA objectives 3 and 4: PICAM SERENA objective 6: STROFIO SERENA objective 7: ELENA and PICAM Winter nightside SERENA objectives

42. SERENA-HEWG meeting, Santa Fe, 12-14 May, 2008 SERENA objectives 1 and 2: STROFIO SERENA objectives 3 and 4: PICAM SERENA objective 6d: STROFIO Summer nightside SERENA objectives In the light of new MESSENGER results, plasma precipitation and ion sputtering can efficiently occur also in the night side, hence in the learning phase also ELENA should be operated

43. SERENA-HEWG meeting, Santa Fe, 12-14 May, 2008 SERENA objectives 1 and 2: STROFIO SERENA objectives 3 and 4: PICAM SERENA objective 5: MIPA SERENA objective 6: ELENA, MIPA and STROFIO SERENA objective 7: ELENA and PICAM at periherm Autumn and Spring SERENA objectives

44. MPO Orbit phases A LB C LD EB ED

45. 45 SERENA timeline SERENA timeline has been developed and discussed within the team and ESA (SERENA TL meeting, Sept. 2011). “Late” and “Early” B and D phases are introduced.

46. Thank you