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Particles and Fields Package (PFP) SWEA pre-CDR Peer Review Science 2011 March 28

Particles and Fields Package (PFP) SWEA pre-CDR Peer Review Science 2011 March 28. Dave Mitchell. MAVEN Level 1 Requirements. SWEA Science Goals. Magnetic Topology & Plasma Regime Crustal Magnetospheres/Cusps Draped Field Lines. o. o. o. SWEA Science Goals. MGS MAG/ER.

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Particles and Fields Package (PFP) SWEA pre-CDR Peer Review Science 2011 March 28

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  1. Particles and Fields Package (PFP) SWEA pre-CDR Peer Review Science 2011 March 28 Dave Mitchell

  2. MAVEN Level 1 Requirements

  3. SWEA Science Goals • Magnetic Topology & Plasma Regime • Crustal Magnetospheres/Cusps • Draped Field Lines o o o

  4. SWEA Science Goals MGS MAG/ER • Electron Impact Ionization • Magnetic Pileup Region • Ionosphere

  5. SWEA Science Goals Mars Express Shadow 2.35 RM Photo-ionization of CO2by solar h @ 304 Å ESCAPE PEB h-electrons MPB 5 4 3 R (MSO) 2 1 0 Escape associated with heavy ions (M> 16) -3 -2 -1 0 1 2 X (MSO)

  6. PF Level 3 Requirements

  7. In-Flight Calibration • Pre-launch: SWEA must have the right dynamic range to handle expected flux range at Mars (10 years of experience with MGS ER) • Need to know GF to a factor of ~2: pre-launch calibrations and simulations easily provide this • Primary Method: LPW measures plasma frequency in the sheath to determine absolute plasma density – compare with SWEA, SWIA, STATIC • Secondary Method: STATIC MCP efficiencies can be determined in flight by comparing START and STOP events – combine with well known mechanical geometric factor to determine absolute sensitivity – cross calibrate with SWEA in sheath • Cross Check: STATIC cross calibrated with NGIMS by measuring periapsis RAM ions – cross calibrate with SWEA in sheath

  8. Data Products FPGA provides a single science data product to the PFDPU Counts per accumulation interval for each of the 16 anodes (as a function of analyzer and deflector sweeps) Complete measurement sequence takes 2 seconds. PFDPU computes three data products, with cadence depending on altitude

  9. Spacecraft Accomodation • Boom location: • Separation from s/c potentials • Large, clear field of view • Sensor head in shadow • Electronics box in sunlight FOV: 360o x ±65o SWEA axis parallel to SC Z when deployed

  10. of the sensor at low energy can be controlled by varying the voltage bias U0 between the internal and external grids: where is the energy resolution for zero bias (0.175) and is the incident energy of the electron Thus for 1.5x finer energy resolution (and 2x smaller GF), we apply Variation of Energy Resolution / Works for apoapsis and side segments in all orbit scenarios. Works for Sun-Velocity mode at periapsis (~50% of orbits). Does not work for deep dips.

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