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C osmic dust R eflectron for I sotopic A nalysis (CRIA)

C osmic dust R eflectron for I sotopic A nalysis (CRIA). Conceptual Design Review. Laura Brower: Project Manager Drew Turner: Systems Engineer Loren Chang Dongwon Lee Marcin Pilinski Mostafa Salehi Weichao Tu. Presentation Overview. Introduction to Problem – Loren Chang

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C osmic dust R eflectron for I sotopic A nalysis (CRIA)

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  1. Cosmic dust Reflectron for Isotopic Analysis (CRIA) Conceptual Design Review Laura Brower: Project ManagerDrew Turner: Systems EngineerLoren ChangDongwon LeeMarcin PilinskiMostafa SalehiWeichao Tu

  2. Presentation Overview • Introduction to Problem – Loren Chang • Previous Dust Analyzers – Loren Chang • LAMA Overview – Marcin Pilinski • Introduction to CRIA – Weichao Tu • Requirements – Drew Turner • Verification – Marcin Pilinski • Risk – Laura Brower • Current Analyses and Trades – Mostafa Salehi • Schedule – Dongwon Lee

  3. Space is Dusty! • Space is filled with particles ranging in size from molecular to roughly 1/10th of a millimeter. • Dust absorbs EM radiation and reemits in the IR band. • Dust can have different properties and concentrations, ranging from diffuse interstellar medium dust to dense clouds, and planetary rings. Loren Chang

  4. Comets, asteroids, and collisions in the new planetary system produce interplanetary dust. Interstellar dust is believed to be produced by older stars and supernovae, which expel large amounts of oxygen, silicon, carbon, and other metals from their outer layers. Clouds of dust and gas cool and contract to form the basic building blocks for new stars and planetary systems.

  5. Heritage • Past instruments have focused primarily on understanding the flux and chemical composition of cosmic dust. • Missions have focused on in-situ measurement and sample return. Aerogel Collector CIDA CDA SDC Loren Chang

  6. Student Dust Counter (New Horizons) • Polyvinylidene fluoride (PVDF) film sensors. • In-situ measurement of dust flux, mass, and relative velocity. • Cannot resolve smaller particles (< 10-12 g) nor measure elemental composition. lasp.colorado.edu/sdc

  7. Cosmic Dust Analyzer (Galileo, Ulysses, Cassini) • Incoming dust particles ionized, then accelerated through electric field to detector. • Time of Flight (TOF) used to infer elemental masses of constituents. • Parabolic target is difficult to manufacture precisely. Low mass resolution (20-50 m/Δm) Target R. Srama et al., The Cosmic Dust Analyzer (Special Issue Cassini, Space Sci. Rev., 114, 1-4, 2004, 465-518)

  8. Stardust • Interstellar and interplanetary dust particles trapped in aerogel. • Direct sample return for analysis of elemental composition on Earth. • Requires highly specialized mission. stardust.jpl.nasa.gov

  9. Cometary and Interstellar Dust Analyzer(Stardust) • Uses impact ionization principle similar to CDA, electric field in reflectron is parabolic, eliminating the need for a parabolic target. Improved mass resolution over CDA (250 m/Δm) • Small target area compared to previous instruments. Roughly 1/20th target area of CDA. J. Kissel et al., The Cometary and Intersteller Dust Analyzer (Science., 304, 1-4, 2004, 1774-1776) Loren Chang

  10. Large Area Mass AnalyzerLAMA Concept: Sub-systems IONIZER Target Marcin Pilinski

  11. LAMA Concept: Sub-systems ANALYZER (Ion Optics) Annular Grid Electrodes Ring Electrodes Grounded Grid Target

  12. LAMA Concept: Sub-systems DETECTOR Detector

  13. Example Spectrum LAMA Concept: Operation incoming dust particle Example Dust Composition Key Species-1 Species-2 Species-3 Target Increasing mass

  14. Example Spectrum LAMA Concept: Operation dust passing through annular electrodes dust passing through grounded grid Data collection from detector started t0

  15. Example Spectrum LAMA Concept: Operation negative ions and electrons accelerated to target target material also ionizes dust impacts target and ionizes (trigger- t0) t0

  16. Example Spectrum LAMA Concept: Operation positive ions accelerated towards grounded grid (trigger- t1) Ions of Species-1, Species-2, Species-3, and Target Material t0 t0 t1 t1

  17. Example Spectrum LAMA Concept: Operation positive focused towards detector t0 t1

  18. Example Spectrum LAMA Concept: Operation positive ions arrive at detector Ions of the same species arrive at the detector at the same time with some spread Species-1 arrives at detector t0 t1 t2

  19. Example Spectrum LAMA Concept: Operation positive ions arrive at detector Species-2 arrives at detector t3 t0 t1 t2

  20. Example Spectrum LAMA Concept: Operation positive ions arrive at detector Species-3 arrives at detector t3 t4 t0 t1 t2

  21. Example Spectrum LAMA Concept: Operation positive ions arrive at detector Ionized Target Material Target material has characteristic peak t3 t4 t5 t0 t1 t2

  22. LAMA is promising, but… • Several tasks have yet to be completed: • Dust triggering system not yet implemented. • No decontamination system. • System has not yet been designed for or tested in the space environment. Marcin Pilinski

  23. Hi, I’m LLAMA Cosmic dust Reflectron for Isotopic Analysis (a cria is a baby llama) Hi, I’m CRIA. Am I Cute? Weichao Tu

  24. CRIA Project Motivation • LAMA Development • To scale down the LAMA instrument to a size better suited for inclusion aboard missions of opportunity. Technology Readiness Level (TRL) of LAMA can be further improved from level 4 to level 5 • Mission opportunity • A universal in-situ instrument design is needed for future mission that can incorporate high performance and large sensitivity and can be adapted to various missions. Weichao Tu

  25. CRIA Project Goals • Mission Goal • Design an instrument capable of performing in-situ measurements of the elementary and isotopic composition of space-borne dust particles • Science Goal • Detect dust particles and determine their mass composition and isotopic ratios • Engineering Goals • Design an instrument based on the LAMA concept that achieves the following: reductions in size, mass, and power in order to be compatible with possible missions of opportunity • Achieve a Technology Readiness Level (TRL) of five or higher for the instrument • To investigate the limits of scalability of the instrument and determine the upper and lower limits of sensitivity (size: between 50% and 125%) in order to provide statistical data and options for a variety of possible missions Weichao Tu

  26. Baseline Design • Inherited from LAMA concept • Triggering system • Scaling LAMA by a factor of 5/8 • Capable of heating the target area for decontamination • Capable of interfacing with a dust trajectory sensor (DTS) • A closed design with a cover • MCP detector may be changed to a large area detector Heater t2 Cover DTS t1 Heater t0 t-1

  27. Baseline Design װ • Specifications of CRIA and LAMA Weichao Tu

  28. Previous Instrument Comparison

  29. Requirements: Top Level 28 Drew Turner

  30. Requirements Flowdown Level 1: Top Level Requirements Analyzer Ionizer Each includes: -Functional Reqs -Performance Reqs -Design Constraints -Interface Reqs • Level 2: System Requirements • - Functional Requirements • - Performance Requirements • - Design Constraints • - Interface Requirements Detector Electronics/CDH Structural/Mechanical Level 3: Subsystem Requirements Thermal Drew Turner

  31. Requirements: Levels 2 and 3 • Functional Reqs: Define system functions; answer “what”, “when”, “where”, and “how many” type questions about the system. CRIA Example: 2.FR5: The instrument shall be capable of detecting positive and negative ion species. • Performance Reqs: Define how well system is to perform its various tasks; answer “how well”, “how often”, and “within how long” type questions. CRIA Example: 2.PR6: The instrument shall be able to record a mass spectrum from Hydrogen to at least m = 300 (amu) and be independent of the triggering method. Drew Turner

  32. Requirements: Levels 2 and 3 • Design Constraints: Defines factors that put limits on the system, such as environment and budget. CRIA Example: 2.DC1: The instrument shall have a closed design such that no light can enter the interior except through the field of view. • Interface Reqs: Defines system inputs, outputs, and connections to other parts of the system or to some other, external system. CRIA Example: 2.IR1: The instrument shall provide a mechanical interface for the Dust Trajectory Sensor (w/ given mass, dimensions and COG). Drew Turner

  33. Requirement Verification Resources Marcin Pilinski

  34. System Level Risk Assessment Sources Solar UV Prelaunch Contamination Micro-meteroid Radiation / Plasma Mechanical Malfunction Material Outgassing Events Detector damaged Contaminated spectra Detector damaged Instrument charging Inaccurate spectra / no spectra recorded Contaminated spectra Noise in spectra Target area damaged Electronics malfunction Arcing Mitigation UV reflective electrodes Aperture Cover Shielding in annular electrode design Use rad-hard electronics and rad protect electronics Vaporize contaminants with heater Use clean room On/Off detector mode Use low outgassing mt’ls Technol. Risk UV impact on detector unknown Risk Level High Low Medium Medium High Low • High probability of impacts • Instrument charging not understood • No risk mitigation • Technology limits unknown • Common practice • Materials known • Heater temp range can be large Laura Brower

  35. Current Analyses and Trades • Arcing Preliminary calculation: • Breakdown electric field as a function of pressure for air • Maximum electric field as a function of gap distance for inner electrode • Reduced size increases risk of arcing • Unexplored area: The arcing in the plasma • Material outgassing - Material selection to low outgassing specification (G-10, Noryl, ceramic, etc.) - More details on other material properties (thermal expansion, tensile strength, density, etc.)

  36. Current Analyses and Trades • Thermal power required • Preliminary calculation on power require to heat target area to 100 oC is on going • Target design is thermally conductive • Detector protection against UV and Micrometeoroids • We calculated micrometeoroid flux at 1 AU • UV reflection / absorption by coating instrument interior • Determine impact of UV on detector performance

  37. Schedule Dongwon Lee

  38. Schedule Dongwon Lee

  39. Questions?

  40. Backup Slides

  41. Previous Instrument Comparison

  42. Mass Resolution (m/m) • Mass resolution describes the ability of the mass spectrometer to distinguish, detect, and/or record ions with different masses by means of their corresponding TOFs. • m/m will be affected by: • The energy and angular spread of emitted ions • Sampling rate m/m= t/2t CRIA: dt=2ns • Electronic noise FWHM: full width at half maximum

  43. Arcing • Electric field required for arcing in a neutral dielectric given by Paschen’s Law. Nonlinear function of pressure and gap distance.

  44. Expected Impacts For randomly tumbling object. Per NASA Technical Memorandum 4527, p.7-3

  45. Possible Questions • What is the elemental composition of cosmic dust? • What is the dust flux and its mass dependence? • What direction is the dust coming from? • What are the differences in composition and size between interstellar and interplanetary dust?

  46. Schedule Dongwon Lee

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