1. The Space Environment II: Characteristics of the Plasma and Radiation Environments Dr. Andrew Ketsdever MAE 5595 Lesson 5

2. Plasma Environment Magnetosphere –Geomagnetic field around Earth –Interacts with solar wind –Deflects most of the plasma flow Ring Current –Encircles magnetic equator (3-6 R E ) –Formed by the drift of charged particles Ions (+) move westward Electrons (-) move eastward –Energies from 10 to 250 keV (85 keV average) Plasma Sheet –Current system which separates oppositely directed magnetic fields emanating from N and S poles –Energies Electrons: 0.5 to 1.0 keV Ions: 2 to 5 keV

3. Plasma Environment

4. Ionosphere Charge neutrality exists above the D Layer Ions and electrons are almost always created or destroyed in pairs Some regions (eg. F1) disappear completely after local sunset Regions are described by radio frequencies (highest frequency reflected by the layer)

5. Ionosphere

6. Plasma Environment

7. Plasma Interactions Electron and Ion interactions with surfaces –Augering Desorption of inner core electrons –Sputtering Removal of material from surface –Penetration Absorption at a depth from the surface –Secondary electron emission Removal of electrons from surface –EM emission Emission of highly energetic (x-ray) photons

8. Secondary Electron Yield

10. Secondary Electron Emission

12. Plasma Interactions

13. LEO Plasma Environment Quasi-neutral plasma At 300 km, n ~ 10 5 cm -3 T e,i ~ 1000 K (quasi-equilibrium) J e ~ 1 mA/m 2 Photoemission ~ 10  A/m 2 Secondary electron emission ~ 0.01 J e Sputtering yield is negligible LEO major source is incident ambient plasma Enhancement of plasma environment at high inclinations (auroral zones) –High density –High energy (several keV)

14. GEO Plasma Environment Plasma is not quasi-neutral At GEO, n ~ 1 cm -3 Energies –Ions: 10 keV (H + ) –Electrons 2.4 keV J e ~ 10 nA/m 2 Photoemission ~ 10  A/m 2 Secondary electron emission and sputtering yield are not negligible Enhanced by solar storms / events

15. Spacecraft Charging

16. Unbiased Spacecraft Charging in LEO

18. Biased Spacecraft Charging

20. GEO Charging

21. GEO Charging: SEU SCATHA Data

22. SCATHA Launched 31 JAN 1975 to study effects of high altitude charging Perigee: 5.3 R E Apogee: 7.8 R E –GEO: 6.6 R E Inclination: 8º Period: 23.6 hours Drift around Earth every 70 days

23. SCATHA Data

26. Radiation Environment: GCR

27. Radiation Environment: Solar

29. Radiation Environment: Trapped

30. Radiation Environment: Van Allen Radiation Belts

31. Solar Min Solar Max 5e6 1e7

32. Radiation Environment: Van Allen Radiation Belts

33. Earth Radiation Environment

34. Radiation Terminology RAD: Radiation absorbed dose –1 rad = 0.01 J/kg (about the energy to lift a paper clip 1 mm off a table) RBE: Relative biological effectiveness –Represents destructive power of dose on living tissue REM: Roentgen equivalent mean –Product of RAD and RBE –Cumulative over the lifetime of the subject

35. Radiation Effects Effects of radiation dosage on humans –Blood count changes (15-50 REM) –Vomiting (100 REM) –Mortality (150 REM) –Leathal Dosage 50% of population (320-360 REM) Common event dosage –Transcontinental roundtrip (0.004 REM) –Chest X-ray (0.01 REM) –Living in Los Angeles (0.1 REM) –Living in Denver (0.2 REM) –Space Shuttle Mission (0.65 REM) –Skylab 3 for 84 days (17.85 REM)

36. Radiation Interactions

37. Permanent radiation effects –Change in material that persists after material removed from radiation source –Typically caused by atomic displacements in the material Transient radiation effects –Change in material does not persist after material removed from radiation source –Alters material properties during exposure

38. Radiation Interactions: Photons Photoelectric effect: Incident photon imparts energy to material electron Compton scattering: Photon loses part of its energy to electron, remaining energy is released in lower energy photon Pair production: Photon materializes into an electron-positron pair

39. Current Photon Radiation Environment

40. Radiation Effects: Electrons

41. Radiation Interaction: Ions

42. Radiation Interactions

43. Radiation Shielding Low Z material is better.

44. Radiation Shielding

45. Radiation Effects Degradation –Human –Optical Surfaces –Solar Arrays –Thermal Properties –Mechanical Properties Sensors and Processors –False readings –SEU –Latch ups Solar proton event 11/1997

46. 1989 Solar Event

47. Historical Solar Events

48. Solar Array Degradation

49. Stardust Mission Stardust Craft Tested for Damage After Solar Storm By Lee Siegel Science Writer posted: 07:05 pm ET 08 August 2000 Originally posted 4:45 p.m., 8/8/00 Lee Siegel A test performed Tuesday August 8 ruled out fears that solar flares damaged the camera on the Stardust spacecraft, which is due to photograph Comet Wild 2 and collect collect comet dust in 2004. Now engineers will try to fix another problem that threatens to degrade Stardusts comet pictures.Comet Wild 2comet dust "The flares didnt do a thing to us," said Ray Newburn, who heads the Stardust imaging team at NASAs Jet Propulsion Laboratory in Pasadena, Calif.Stardust NASA earlier had feared possible solar radiation damage to the NAVCAM camera s electronic sensor. The agency had said the July solar flares might increase background "noise" that could "mask" Stardusts images of dim stars and Comet Wild 2.solar radiation Engineers tested the camera by turning on the electronic sensor -- known as a CCD or charge couple device -- without opening the shutter. A test image showing a known uniform shade of gray would indicate there was no damage, while brighter gray would indicate there was damage, said Tom Duxbury, Stardusts acting project manager. Newburn said the lack of solar radiation damage means engineers now will proceed with a two-week effort to use the cameras heater to burn off contaminants coating the sensor. That repair was delayed while engineers first checked for radiation damage.

50. Effects of the Plasma and Radiation Environments