Set the Controls for the Heart of the Sun

Transcription

1 Sixty Years of Satellites Parker Solar Probe Set the Controls for the Heart of the Sun Matthew STUTTARD, Advanced Systems Architect Science Museum, London, 5 October 2018

2 Why Study the Sun? Understand how stars work Develop high energy plasma physics (fusion) Understand solar activity to improve forecasts of severe space weather 2 5 October, 2018 Solar Missions, Science Museum, Stuttard

3 Saint Patrick s Day Storm: March 17, October, 2018 Solar Missions, Science Museum, Stuttard

4 Solar Orbiter a close-up high resolution study of the sun 4 5 October, 2018 Solar Missions, Science Museum, Stuttard

5 What is Solar Orbiter? A spacecraft that will study the Sun and inner heliosphere for 7 years instruments to study surface and atmosphere imagers, spectrometers instruments to measure environment around the spacecraft particle detectors, magnetometers Adding to knowledge gained from past missions SOHO, Ulysses, STEREO A & B, SDO..and current missions Parker Solar Probe Procured by: European Space Agency with NASA participation Prime contractor: Airbus Defence and Space Ltd Solar Orbiter exploring the Sun's realm; Copyright: ESA/AOES Launch Window: 6-24 February 2020 Determined by Earth-Venus geometry 5 5 October, 2018 Solar Missions, Science Museum, Stuttard

6 What questions will it answer? How solar eruptions produce energetic particle radiation that fills the heliosphere How the sun dynamo works and drives connections between the Sun and the heliosphere How and where the solar wind plasma and magnetic field originate in the corona How solar transients drive heliospheric variability 6 5 October, 2018 Solar Missions, Science Museum, Stuttard

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8 What will Solar Orbiter do that previous missions haven t? In-situ measurements close to the Sun 20 fly-bys Pristine solar wind streams Reduced scattering of energetic particles Quasi co-rotating vantage point Solar Orbiter tracks the same features as it orbits Can watch magnetic activity building up that can lead to flares/ CMEs Remote Sensing observations High data rate acquisition In situ observations low data rate acquisition Max heliospheric latitude +/- 5 days Perihelion +/- 5 days Simultaneous high-res imaging and spectroscopic observations North and South Solar Pole observations We cannot see the polar regions from Earth s orbit Min heliospheric latitude +/- 5 days Synergies with Solar Probe measurements Simultaneous In-situ measurements of particle fluxes at 9 and 59 solar radii Earth GAM Venus GAM Science Window LEOP 7 days NECP ~2 months CP ~3 years NMP ~3.5 years EMP ~2.5 years Launch 8 5 October, 2018 Solar Missions, Science Museum, Stuttard

9 How Does it Work? Spacecraft Sub-systems PYR (A+B) Communication System X/Ka- HGA X-MGA PYR (A+B) X-LGA 1 X-LGA 2 MGA Safe Pos. DC/DC X/Ka- Bd Feed HDs Status (A+B) HDs Status (A+B) HGA Safe Pos. HGAPM (2-axis) MGAPM (3-axis) Drv A+B (3-axis) APME RT N R Drv A+B (2-axis) RT N R DC/DC RFDA WGS -4 WGS -3 WGS -1 WGS -2 WGS-6 Short X - Dipl.1 Ka-RFI-1 Ka-RFI-2 X- Dipl. 2 X-RFI-1 X-RFI-2 WGS-5 WGS-1 Ka-TWTA-1 EPC Ka-TWTA-2 EPC X-TWTA-1 EPC X-TWTA-2 EPC WGS-2 WGS-1 A Pos 1 WGS-1 B Pos 1 WGS-1 A Pos 2 WGS-1 B Pos 2 WGS-1 A Status WGS-1 B Status WGS-2 A Pos 1 WGS-2 B Pos 1 WGS-2 A Pos 2 WGS-2 B Pos 2 WGS-2 A Status WGS-2 B Status LCL(A) TC/TM LCL(B) TC/TM LCL(A) TC/TM LCL(B) TC/TM WGS-3 WGS-3 A Pos 1 WGS-3 B Pos 1 WGS-3 A Pos 2 WGS-3 B Pos 2 WGS-3 A Status Ka- Coupler 3 db Coupler WGS-4 WGS-3 B Status WGS-4 A Pos 1 WGS-4 B Pos 1 WGS-4 A Pos 2 WGS-4 B Pos 2 WGS-4 A Status WGS-4 B Status Ka-Band Trans. X-Band Trans. A A X-Band Receiver /Demod DST-1 Ka-Band Trans. X-Band Trans. B A WGS-5 WGS-5 A Pos 1 WGS-5 B Pos 1 WGS-5 A Pos 2 WGS-5 B Pos 2 WGS-5 A Status WGS-5 B Status Ka-TM 1A Ka-TM 1B LCL DC/DC X-TM 1A X-TM 1B FCL DC/DC X-TC 1A X-TC 1B Discrete TM/TC B X-Band Receiver /Demod B DST-2 RT N R Ka-TM 2A Ka-TM 2B LCL DC/DC X-TM 2A X-TM 2B FCL DC/DC X-TC 2A X-TC 2B Discrete TM/TC RT N R WGS-6 WGS-6 A Pos 1 WGS-6 B Pos 1 WGS-6 A Pos 2 WGS-6 B Pos 2 WGS-6 A Status WGS-6 B Status X-TC (Test) X-TC (Test) DMS RIU EHP ANP (24) ANY (80) AN2 (12) AN1 (8) BLD (12) RSA (48) SHP (64) PTA (8) ANT LCL DC/DC EHP ANP (24) ANY (80) AN2 (12) AN1 (8) BLD (12) RSA (48) SHP (64) PTA (8) ANT CD/DC ANP (24) ANY (80) AN2 (12) AN1 (8) BLD (12) RSA (48) SHP (64) CD/DC STD I/O A STD I/O B STD I/O C C (2) C (2) C (2) C (2) ZZ 9 5 October, 2018 Solar Missions, Science Museum, Stuttard

10 Four local environment (In-situ) instruments MAG, SWA, EPD, RPW Provide data on the local Solar plasma environment particles, mag fields, plasma flux, radio bursts EPD: Measuring properties of accelerated energetic particles emitted from the Sun RPW: Studying local electromagnetic and electrostatic waves and Solar radio bursts SWA: Sampling constituents of the Solar wind MAG: High precision measurements of the heliospheric magnetic field 10 5 October, 2018 Solar Missions, Science Museum, Stuttard

11 Six Remote sensing instruments EUI, METIS, PHI, SolOHI, SPICE, STIX Match in-situ observations with their source regions on the Sun SPICE: Spectroscopy of the solar disk and corona in UV. EUI: UV imaging of the Solar corona (studying eruptions as they propagate out from the Solar surface). METIS: High resolution UV and EUV coronagraphy PHI: Full disk and high-resolution visible light imaging of the Sun. STIX: Provides imaging spectroscopy of solar thermal and non-thermal X-ray emission. Also acts as a flare monitor for the other instruments SolOHI: Observe light scattered by the solar wind to pinpoint coronal mass ejections (CMEs) October, 2018 Solar Missions, Science Museum, Stuttard

12 Remote sensing instruments on the MY panel PHI METIS EUI STIX SPICE Demanding alignment requirement (0.03 ) 12 5 October, 2018 Solar Missions, Science Museum, Stuttard

13 Fields of View SPICE PHI HRT EUI HRI METIS STIX/ PHI FDT EUI FSI 13 5 October, 2018 Solar Missions, Science Museum, Stuttard

14 Design Challenges: Communications (X-band) High data rate is just 180kbs Transfer rates are less than a standard 3G or Wifi link Instruments rely on on-board data processing and compression to meet the telemetry requirements Many instruments are prioritising data for download Instruments are capable of overwriting data Non-contact periods of up to 64 days Spacecraft implements a store and forward approach on-board Spacecraft must be autonomous and able to cope autonomously with FDIR Management of three different antennas: LGAs (LEOP and backup) 4π sr MGA (Survival Mode, Strobing) HGA (Nominal) Distortion and pointing error in spec LGA 2 MGA GEU OBC IMU SSMM PCDU Comms Structure LGA 1 RIU Comms IMU SADE Battery Other design challenges Thermal environment From +600C to -180C Pointing stability Power generation Densely packed payloads Cleanliness on ground Cleanliness in orbit Electro-magnetic cleanliness 14 5 October, 2018 Solar Missions, Science Museum, Stuttard HGA

15 Solar Orbiter - Flight Build Completed in Stevenage Solar Orbiter is now entering the next key phase: one year in Environmental Test at IABG, Munich 15 5 October, 2018 Solar Missions, Science Museum, Stuttard

16 Parker Solar Probe Magnetometer Boom Deployed 16 5 October, 2018 Solar Missions, Science Museum, Stuttard

17 NASA Mission: Parker Solar Probe Understand origin /evolution of solar wind energy flows structure and dynamics of magnetic fields. mechanisms that accelerate and transport energetic particles Launch: 12 Aug VGAs over 7 years Science phase of 24 solar orbits Will enter the Sun s outer atmosphere (corona) 4 million miles (~9Rs) from surface photosphere Where solar wind speeds up from subsonic to supersonic and highest energy particles originate Four instrument suites Fields Coronal imager (WISPR) Particles (SWEAP) Particles (ISʘIS) Technologies : 11.5cm thick carbon composite heat shield External temp 1377C, 650kW/sq.m Close approach (<0.25AU) solar array uses pumped fluid cooling 5 October, 2018

18 Solar Orbiter and Parker Solar Orbiter Parker Closest approach 43m km (59 Rs) 7m km (9Rs) Particles & Fields measured Synergistic data Solar feature imaging/spectroscopy Solar Polar Observation Coronal Entry 5 October, 2018

19 Thank You!