1. NITRO for M4: IRF (Kiruna, Sweden), IRAP (Toulouse, France), OHB-Sweden (Kista, Sweden), NASA/GSFC (USA), UNH (Durham, USA), LATMOS/IPSL (Guyancourt, France), U. Bern (Switzerland), UCL/MSSL (London, UK), IWF (Graz, Austria), IASB-BIRA (Brussels, Belgium), IAP/ASCR (Prague, Czech), LPC2E (Orleans, France), Inst Space Sci. (Bucharest, Romania), Tohoku U. (Sendai, Japan), IAXA/ISAS (Sagamihara, Japan), UCB/SSL (Berkeley, USA), SwRI (San Antonio, USA), U. Athens (Greece), LPP (Paris, France), Aalto U. (Helsinki, Finland), FMI (Helsinki, Finland), U. Tokyo (Kashiwa, Japan), SRC-PAS, (Warsaw, Poland), U Sheffield (UK), GFZ, (Potsdam, Germany),UCLA (Los Angeles, USA), etc. Nitrogen Ion TRacing Observatory (NITRO) for ESA's M-class call M. Yamauchi, I. Dandouras, H. Rème, P. Rathsman, and NITRO proposal team. 1 poster R436@ST2.1 (EGU2015-4104), Wednesday (2015-4-15)

2. NITRO for M4: Primary objective: Investigate Nitrogen budget of 2 near-Earth space in comparison with Oxygen budget, because the N/O ratio of escape is poorly understood but important for: Earth evolution / origin of life: Amino acid formation depends on oxidation state of N (NH 3 or N 2 or NO x ) and the relative abundance of N, O, & H near surface. Current measurements can be used to determine how the atmosphere evolved on geological time scales. Planetary atmosphere: N on Mars is only 0.01% of Earth ~ Venus ~ Titan). To understand the abundances on other planets, we first have to understand the Earth case. Magnetosphere: cold N + /O + escape correlates with F10.7 & Kp. With similar M/q, but with different ionospheric scale heights, they are good tracers to understand ion outflow dynamics and circulation. Exosphere and Ionosphere: Our knowledge of exosphere > 1000km is very poor, and variability of ionospheric N + /O + ratio is poorly understood. Space Plasma Physics: Different V 0 between M/q=14 and M/q=16 gives extra information on plasma energization mechanisms.

3. NITRO for M4: Nitrogen is an essential element for life 3 Miller’s experiment (Miller and Urey, 1959). Pre-biotic type atmosphere + discharges  formation of amino-acids ! The result depends on the oxydation state of N reduced form (NH 3 ) neutral form (N 2 ) oxidized form (NO x )  Formation of pre-biotic molecules is most likely related to the relative abundance of N, O, and H near the surface  (not only the amount !)

4. NITRO for M4: MarsVenus Earth 4 comet 1.N/O ratio @ ancient Earth? 2. Why N/O ratio @ Mars << @ the Earth, Venus, Titan rich in N N < 0.01% of Earth/Venus exist Open questions on Nitrogen

5. NITRO for M4: Our knowledge on Earth’s N + behavior is poor (a) Dependence on geomagnetic activities is larger for N + than O + for both 30 keV (Hamilton et al., 1988). (b) N + /O + ratio varies from <0.1 (quiet time) to ≈ 1 (large storm). What we call O + is a mixture of N + and O +. This also applies to O ++. (c) [CNO group] + at <10 keV range is abundant in the magnetosphere. (d) Ionization altitude of N (eventually N 2 ) is likely higher than for O in the ionosphere (when O + is starting to be heated, majority of N is still neutral). (e) N/O ratio at Mars (and C/O ratio at Moon) are extremely low compared to the other planets. (f) Molecular N 2 was detected even Martian soil and comet (Rosetta). (g) Isotope ratio (e.g., 15 N/ 14 N) is different between different planets/comets. (But instrumentation related to this requires M/∆M > 1000, i.e., large mass, and is outside our scope.) 5 One thing clear is that O+ behavior and N+ behavior are completely different!

6. NITRO for M4: 6 (1) Magnetospheric density distribution for N + and N 2 +, O +, H +, He +, and He ++. - Average 3D magnetospheric distribution and its orbit-to-orbit variation - Spatial and temporal variability of imaged line-of-site column density (2) Energy distribution of each species in the magnetosphere. - Energy distribution (degree of energization and its direction) - Time delay between direct low-energy filling and convective high-energy filling (3) Neutral density and ion flux in the upper exosphere/ionosphere > 1500 km - Average altitude distribution - Spatial and temporal variability - Relation between the ionospheric/exospheric density and magnetospheric density/energy: (4) Quantities that significantly controls the ion energization and escape - Correlation between wave and ion velocity distributions of N and O in the magnetosphere (5) Extra measurements that take advantage of basic spacecraft configuration - Correlation between wave and ion velocity distributions of N and O in the ionosphere: - Relation between sunward return flow and ion dynamics in the magnetosphere. - Heavy ion precipitation flux above the ionosphere. What should be observed

7. NITRO for M4: (1)In-situ method Mass Spectrometer (cold): high M/∆M Mass Spectrometer (energetic): high M/∆M Ion (Mass) Analyser (hot): high g-factor & marginal M/∆M is improving — Magnet, grid-TOF, reflection-TOF, MCP-MCP TOF, shutter-TOF, etc — Photoelectron: exact M but it gives only connectivity from ionosphere Wave (Ω O+ ≠Ω N+ ): a challenge because of ∆f/f  ∆M/M < 7% (2) Remote sensing of emission (line-of-sight integration) from above the ionosphere (>1800 km) & outside the radiation belt (>60° inv) N + (91nm, 108nm), N 2 + (391nm, 428nm), NO + (4.3 µm), NO + (123-190nm=weak), O + (83nm, 732/733 nm): exact M but must fight against contamination from ionosphere and sensitive to radiation belt background Possible methods of separating N + & O + 7 ⇒ By combining both methods (i.e., with two spacecraft), we have 3-D mapping of N/O in the magnetosphere

8. NITRO for M4: 8 Unique Orbit

9. NITRO for M4: In-situ #1 mother (spinning) * Ion mass spectrometer (ion) (Bern) * Ion mass analyzers (0.03 – 30 keV): (1) Heavy ions only (Kiruna) (2) Wide mass range (Toulouse) * Ion mass analyzer (> 30 keV) (UNH) * Magnetometer (Graz) * Langmuir Probe (Brussels) * Waves analyser (Prague) * Search Coil (Ω N ≠Ω O ) (Orleans) * Electron analyzer (London) * Radiation belt vertual detector (Athens) * ENA monitoring substorm (Berkeley) * (Potential Control=SC subsystem) Payloads Remote sensing & monitoring (3-axis) * Optical (emission) (LATMOS & TokyoU) (1) N + : 91 nm, 108 nm (2) N 2 + : 391 nm, 428 nm (3) O + : 83 nm * Mass spectrometer (cold N + and neutrals) (Goddard) * Ion analyzer (< 0.1 keV) (Kiruna) * Ionospheric optical camera (Tohoku) * Langmuir Probe (Brussels) * Magnetometer (Graz) * Electron analyzer (London) * Waves analyser (Prague) * Search Coil (Ω N ≠Ω O ) (Orleans) * Ion analyzer (< 50 keV) (ISAS) 9 * colored: nominal, * black: optional

10. NITRO for M4: 10 Mass coverage

11. NITRO for M4: With an unique orbital configuration and recently developed reliable instrumentation, NITRO can target nitrogen’s 3-D dynamics for the first time in the Earth’s magnetosphere. This is the first step in understanding of the evolution "planet Earth", which is a mandatory knowledge in estimating the ancient Earth's chemical condition for amino- acid formation (Astrobiology), as well as the nitrogen differences between the terrestrial planets (Planetology). The required instrumentation can also reveal key questions on Magnetospheric, Ionospheric, Exospheric dynamics and basic Space Plasma Physics. Summary 11

12. NITRO for M4: 12 Cold ion (lab calibration)Hot ion (lab calibration) Spectra line (Å) 12

13. NITRO for M4: 13 Remote sensing SCIn-situ SC