Mario Acuna 1940 - 2009. Explorer 47, (IMP 7)Ulysses Explorer 50 (IMP 8)Goiotto ISEE 3 Mars Global...
-
Upload
lindsey-robertson -
Category
Documents
-
view
226 -
download
5
Transcript of Mario Acuna 1940 - 2009. Explorer 47, (IMP 7)Ulysses Explorer 50 (IMP 8)Goiotto ISEE 3 Mars Global...
Explorer 47, (IMP 7) UlyssesExplorer 50 (IMP 8) Goiotto
ISEE 3 Mars Global Surveyor
Pioneer 11 Near Earth Asteroid Rendezvous
Voyagers 1, 2 Lunar ProspectorMAGSAT ACEProject Firewheel IMEXViking (Swedish) Stereo
AMPTE Messenger
Mario Space Missions
• U.S. Project Scientist for International Solar Terrestrial Physics Program – coordinated research effort by Japan, Europe, Russia, U.S.; involved > 1000 investigators and the launch of 7 spacecraft in the middle 90’s.
• Project Scientist for SAC Cooperative Program with Argentina, Brazil, Italy and Denmark
Taken by Pioneer 11 on 29 August 1979 from a distance of 2.5 million kilometres, 58 hours before PCA. Rings illuminated from below.
Spacecraft Mass: 722 kgPower: 3 RTG (Plutonium Oxide)Antenna: 3.7 mRequires 34 m / 70 m dishBit Rate (Dlink): X-Band 160 bits/s
This is an artist's concept of the Saturnian plasma sheet based on data from Cassini magnetospheric imaging instrument.Image credit: NASA/JPL/JHUAPL
The magnetic field of Uranus (North and South Poles labeled - "N" and "S") istilted 59° away from the planet's rotation axis. The dipole component (like a bar magnet) of its magnetic field is also offset from the planet's center by about 1/3rd of the radius of Uranus.
• The Heliosheath at the nose is estimated to be 30-60 AU wide.
• At the TS, radial velocity of the solar wind will decrease by a factor of 2.4 – 4 depending on the strength of the TS, and will continue to decrease as 1/r2 where r is the heliocentric distance.
• The intensity of the transverse component of the interplanetary magnetic field jumps by the same factor and continues to increase proportional to r across the heliosheath.
Heliosheath
This image is a map of Martian magnetic fields in the southern highlands. The magnetic fields appear to be organized in bands, with adjacent bands pointing in opposite directions, giving these stripes a striking similarity to patterns seen in the Earth's crust at the mid-oceanic ridges.
Fluxgate magnetometer
GSFC-JHU/APL development.
MESSENGER
Launch: 3 Aug 2004Mercury Orbit Insertion: 18 Mar 2011
RLM 24IAC-07-A3.2.02PUBLIC DOMAIN INFORMATION. NO LICENSE
REQUIRED IN ACCORDANCE WITH ITAR 120.11(8).
Mission Trajectory
We are there!
Magnetometer 3-axis flux-gate sensor 3.6 m carbon fiber boom
– Small sunshade protects sensor Dual range:
– ±1500 and ±65000 nT– Auto-ranging
16/17-bit quantization– 0.047 nT resolution
Up to 20 samples per sec.– 10 filtered rates 10s-1 to 0.01s-1
S/C magnetic cleanliness program– Solar panel wiring– Reaction wheel shielding– Propulsion valve compensation– Battery– Largest identified SC
interference: 0.9 pT
RLM 26IAC-07-A3.2.02PUBLIC DOMAIN INFORMATION. NO LICENSE
REQUIRED IN ACCORDANCE WITH ITAR 120.11(8).
2011: DOY 084 and 085 MESSENGER Orbit
MESSENGER MagnetometerPreliminary Early Orbit Observations
A
A A A A
X Position (km)Y Position (km)
Z P
osit
ion
(k
m)
B
B
A
B BC C
C
C