A. Milillo, S. Orsini and A. Mura (INAF/Institute of Space
Astrophysics and Planetology) And the SERENA Team Slide 2 SERENA -
HEWG meeting, Rome, 13-17 May, 2013 Hermean environment (from
Milillo et al., SSR, 2005) Slide 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. Slide 4 SERENA
vs Hermean environment SERENA - HEWG meeting, Rome, 13-17 May, 2013
Slide 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 Mercurys 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 Slide 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 Slide 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. Slide 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). Slide 9 Signal simulation for
different sources BackscatteringCharge exchangeIon sputtering
SERENA - HEWG meeting, Rome, 13-17 May, 2013 Slide 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 Slide 11
South IMF case Extreme event case Parker IMF case Kallio et al.
Slide 12 Precipitation derived after Schleicher et al. 2004
Observations Mura et al. South IMF case Slide 13 IMF (-20, 0, -5)
aphelion Massetti et al. IMF (-20, 0, -5) perihelion Extreme case
IMF (-45, 16, -20) Nsw 120 cm -3 Slide 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 Slide 15
ELENA coverage for a whole Mercury season with 1.a hypothetical
uniform flux 2.uniform flux inside cusp projection Slide 16 SERENA
- HEWG meeting, Rome, 13-17 May, 2013 ELENA LT Coverage: Summer
Autumn Slide 17 SERENA - HEWG meeting, Rome, 13-17 May, 2013 ELENA
LT Coverage: Winter Spring Slide 18 SERENA - HEWG meeting, Rome,
13-17 May, 2013 ELENA Geographic Coverage: Summer Autumn Slide 19
SERENA - HEWG meeting, Rome, 13-17 May, 2013 ELENA Geographic
Coverage: Winter Spring Slide 20 2. uniform flux inside cusp
projection ELENA LT Coverage: Summer Autumn Slide 21 ELENA
Coverage: Winter Spring Slide 22 ELENA Geographic Coverage: Summer
Autumn Slide 23 ELENA Geographic Coverage: Winter Spring Slide 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 Slide 25 Summary of ELENA primary
objectives SERENA - HEWG meeting, Rome, 13-17 May, 2013 Slide 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 Slide 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 Slide 28 Summary of STROFIO primary
objectives SERENA - HEWG meeting, Rome, 13-17 May, 2013 Slide 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 Slide 30 2pi coverage total coverage sample pixel
(1 of 24) Field of view of one MIPA pixel Slide 31 SERENA - HEWG
meeting, Rome, 13-17 May, 2013 MIPA Scientific Operations Slide 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 Mercurys
Magnetosphere Slide 33 Summary of MIPA primary objectives SERENA -
HEWG meeting, Rome, 13-17 May, 2013 Slide 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
Slide 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. Slide 36 SERENA - HEWG
meeting, Rome, 13-17 May, 2013 PICAM mass analysis PICAM mass
resolution is M/M > 50 Simulations: M=39 and 40 AMU. Slide 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 Slide 38 Summary of PICAM primary
objectives SERENA - HEWG meeting, Rome, 13-17 May, 2013 Slide 39
SERENA operations vs phase Slide 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 Slide 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
Slide 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 Slide 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
Slide 44 MPO Orbit phases A LB C LD EB ED Slide 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. Slide 46 Thank you
