The STEREO/IMPACT Magnetic Field Experiment

Abstract The magnetometer on the STEREO mission is one of the sensors in the IMPACT instrument suite. A single, triaxial, wide-range, low-power and noise fluxgate magnetometer of traditional design—and reduced volume configuration—has been implemented in each spacecraft. The sensors are mounted on the IMPACT telescoping booms at a distance of ∼3 m from the spacecraft body to reduce magnetic contamination. The electronics have been designed as an integral part of the IMPACT Data Processing Unit, sharing a common power converter and data/command interfaces. The instruments cover the range ±65,536 nT in two intervals controlled by the IDPU (±512 nT; ±65,536 nT). This very wide range allows operation of the instruments during all phases of the mission, including Earth flybys as well as during spacecraft test and integration in the geomagnetic field. The primary STEREO/IMPACT science objectives addressed by the magnetometer are the study of the interplanetary magnetic field (IMF), its response to solar activity, and its relationship to solar wind structure. The instruments were powered on and the booms deployed on November 1, 2006, seven days after the spacecraft were launched, and are operating nominally. A magnetic cleanliness program was implemented to minimize variable spacecraft fields and to ensure that the static spacecraft-generated magnetic field does not interfere with the measurements.

[1]  T. Sanderson,et al.  Observations of three‐dimensional anisotropies of 35‐ to 1000‐keV protons associated with interplanetary shocks , 1985 .

[2]  Mario H. Acuna,et al.  Near Magnetic Field Investigation, Instrumentation, Spacecraft Magnetics and Data Access , 1997 .

[3]  A. Szabo,et al.  A summary of WIND magnetic clouds for years 1995-2003: model-fitted parameters, associated errors and classifications , 2006 .

[4]  D. Aaron Roberts,et al.  Velocity shear generation of solar wind turbulence , 1992 .

[5]  M. Acuna,et al.  Fluxgate magnetometers for outer planets exploration , 1974 .

[6]  C. Russell,et al.  Multiple spacecraft observations of interplanetary shocks: ISEE three‐dimensional plasma measurements , 1983 .

[7]  A. Szabó An improved solution to the “Rankine-Hugoniot” problem , 1994 .

[8]  T. Sanderson,et al.  Tracing the topology of the October 18–20, 1995, magnetic cloud with ∼0.1–10² keV electrons , 1997 .

[9]  I. Richardson,et al.  The fraction of interplanetary coronal mass ejections that are magnetic clouds: Evidence for a solar cycle variation , 2004 .

[10]  Mario H. Acuna,et al.  Magnetic Field Experiment on the Freja Satellite , 1994 .

[11]  D. A. Roberts,et al.  Origin and evolution of fluctuations in the solar wind: Helios observations and Helios-Voyager comparisons , 1987 .

[12]  C. Russell,et al.  Physics of magnetic flux ropes , 1990 .

[13]  M. Acuna,et al.  The Giotto magnetometer experiment , 1987 .

[14]  J. Sauvaud,et al.  Mars Observer magnetic fields investigation , 1992 .

[15]  L. Burlaga,et al.  Fast ejecta during the ascending phase of solar cycle 23: ACE observations, 1998-1999 , 2001 .

[16]  J. Scudder,et al.  Fast and optimal solution to the 'Rankine-Hugoniot problem'. [for geometrical shock wave properties, conservation constants and self-consistent asymptotic magnetofluid variables of interplanetary medium] , 1986 .

[17]  H. Cane The large-scale structure of flare-associated interplanetary shocks , 1988 .

[18]  I. Richardson,et al.  Signatures of shock drivers in the solar wind and their dependence on the solar source location , 1993 .

[19]  E. Möbius,et al.  Coupled hydromagnetic wave excitation and ion acceleration at interplanetary traveling shocks and Earth's bow shock revisited , 1999 .

[20]  L. Golub,et al.  The August 11th, 1999 CME , 2004 .

[21]  C. Russell,et al.  Intercomparison of NEAR and Wind interplanetary coronal mass ejection observations , 1999 .

[22]  Fritz Primdahl,et al.  Scalar calibration of vector magnetometers , 2000 .

[23]  M. Acuna,et al.  The AMPTE CCE Magnetic Field Experiment , 1985, IEEE Transactions on Geoscience and Remote Sensing.

[24]  F. M. Neubauer,et al.  Magnetic field experiment for Voyagers 1 and 2 , 1977 .

[25]  W. R. Cook,et al.  STEREO IMPACT Investigation Goals, Measurements, and Data Products Overview , 2008 .

[26]  Mario H. Acuna,et al.  The NEAR magnetic field investigation: Science objectives at asteroid Eros 433 and experimental approach , 1997 .

[27]  Mario H. Acuna,et al.  Space-based magnetometers , 2002 .

[28]  J. Richardson,et al.  The orientation of plasma structure in the solar wind , 1998 .

[29]  S. Krucker,et al.  The source region of an interplanetary type II radio burst , 1999 .

[30]  Dusan Odstrcil,et al.  Numerical simulation of the 12 May 1997 interplanetary CME event , 2004 .

[31]  Martin A. Lee Coupled hydromagnetic wave excitation and ion acceleration at interplanetary traveling shocks , 1983 .

[32]  N. Sckopke,et al.  Observations of gyrating ions in the foot of the nearly perpendicular bow shock , 1982 .

[33]  R. Kallenbach,et al.  Hydromagnetic Wave Excitation Upstream of an Interplanetary Traveling Shock , 2004 .

[34]  D. Haggerty,et al.  Proton, helium, and electron spectra during the large solar particle events of October-November 2003 , 2005 .