Mario Acuna1940 - 2009

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

Fluxgate Magnetometers

Wiring diagram and picture of the Magnetometer used on Mars Global Surveyor

Pioneer 11

Taken by Pioneer 11 on 29 August 1979 from a distance of 2.5 million kilometres, 58 hours before PCA. Rings illuminated from below.

Voyager’s

Spacecraft Mass: 722 kgPower: 3 RTG (Plutonium Oxide)Antenna: 3.7 mRequires 34 m / 70 m dishBit Rate (Dlink): X-Band 160 bits/s

April 01, 2011: Voyager 1 116.6 AU 34.91° N

Voyager 2 95.0 AU33.57° 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

Mars Global Surveyor

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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

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