Voyager Magnetometer
fields in pT, for 1 pT field, the angular gyrofrequency is 95.785e-6 radians/second
Voyager 1 |
|||||||||||
AU |
V1 Date |
Decimal |
F1 |
elev |
az |
F2 |
mHz |
||||
40 |
1990 11 |
90.03014 |
93 |
51.0 |
270.5 |
92 |
8.8 |
||||
49 |
1992 182 |
92.49863 |
86 |
-31.7 |
202.1 |
85 |
8.2 |
||||
50 |
1992 284 |
92.77808 |
43 |
33.1 |
62.5 |
42 |
4.1 |
||||
51 |
1993 18 |
93.04932 |
41 |
60.0 |
33.3 |
40 |
3.9 |
||||
60 |
1995 194 |
95.50411 |
21 |
-54.6 |
275.5 |
19 |
1.9 |
||||
Voyager 2 |
proton km/s |
eV |
radius |
||||||||
AU |
V2 Date |
Decimal |
F1 |
elev |
az |
F2 |
mHz |
min |
max |
max |
km |
40 |
1993 127 |
93.35068 |
113 |
-35.2 |
122.6 |
113 |
10.8 |
6.95 |
42.76 |
9.5 |
4000 |
49 |
1996 160 |
96.44110 |
38 |
8.8 |
96.2 |
36 |
3.5 |
9.74 |
24.72 |
3.2 |
7100 |
50 |
1996 282 |
96.77534 |
45 |
-31.2 |
59.3 |
44 |
4.3 |
10.44 |
19.24 |
1.9 |
4500 |
51 |
1997 38 |
97.10685 |
49 |
-29.5 |
33.5 |
48 |
4.6 |
9.68 |
28.75 |
4.3 |
6300 |
60 |
2000 27 |
100.07671 |
93 |
65.9 |
247.3 |
92 |
8.9 |
7.67 |
25.60 |
3.4 |
2900 |
49 AU fields vary from 36 pT to 86 pT 50 AU fields vary from 42 pT to 45 pT 51 AU fields vary from 40 pT to 49 pT
Assuming ALL (doubtful) of the Sun's maximum solar wind reaches the 50 AU shell (7e26 m²), (7e35 protons), that's 1e9 protons per square meter carrying perhaps 1 picowatt total energy. The shell will get more energy as short wavelength UV and soft X rays.
dates: http://spdf.sci.gsfc.nasa.gov/pub/data/voyager/voyager2/plasma/sedr/v2_sedr_1996.asc
protons: http://spdf.sci.gsfc.nasa.gov/pub/data/voyager/voyager2/plasma/daily
1. decimal year |
2. day |
3. V2-Sun-Earth angle |
4. V2 heliolatitude |
5. Earth heliolatitude |
6. V2 heliolongitude |
7. Earth heliolongitude |
8. VR (km/s, RTN coordinate system) |
9. VT |
10. VN |
11. Den (cm-3, moment) |
12. Den (cm-3, fit) These are best values to use |
13. W (thermal speed, km/s, moment) T(ev)=0.0052*W*W |
14. W (thermal speed, km/s, fit) T(ev)=0.0052*W*W These are best values to use |
15. R (AU, distance from Sun) |
spreadsheet |
radius |
Vsum |
energy |
flux |
line |
AU |
km/s |
eV |
Pr/m2 |
6 |
1.01235 |
353 |
650 |
1.6e12 |
94 |
1.50322 |
384 |
765 |
5.0e8 |
812 |
2.00335 |
395 |
812 |
3.5e8 |
6641 |
50.00465 |
566 |
1668 |
5.2e8 |
Damage Repair, WAG
So at 50 AU. the particle flux is 520/mm²-s. Assume a 1700 eV particle damages 2000 atomic bonds or atom spacings, and each needs 1000 eV worth of work to precisely repair. So the repair energy is 1e9 eV /mm²-s, or 1e15 eV /m²-s. The incoming sunlight is 0.5 W/m², or 3.1e18 eV /m²-s. Damage control will use 0.03% of that energy.