measuring the magnetic field in the sun and the interstellar medium steven r. spangler… university...
TRANSCRIPT
Measuring the Magnetic Field in the Sun and the Interstellar Medium
Steven R. Spangler… University of Iowa
Why is the coronal B field of interest?
• Temperature of corona is 1-2 X 106 K• Magnetic fields probably involved via DC
currents or MHD waves• Assessment of theories requires measurements
Physics of Faraday Rotation
Phase speed of R&L waves
Phase shift (cm) after prop.
Phase shift (radians)
Rotation of polarization position angle
The Instrument: The Very Large Array Radiotelescope
Operated by the National Radio Astronomy Observatory (NRAO)
How one measures polarization position angles and Faraday
rotation with the VLA
• Polarization map of a radio galaxy at 1465 MHz
The background sources (signal generators for propagation expmts)
Extragalactic radio sources
EG sources provide many “drillholes” through corona
Extragalactic sources provide “constellations” of background
objects
Mancuso & Spangler, Astrophys. J. 539, 480, 2000
Measuring the Coronal Magnetic Field from a set of Faraday
Rotation Measurements• Adopt “forward
problem” approach• Specify model density
function n• Specify model B field• Iterate to obtain optimum
agreement with observations
Plasma Contributions to the Faraday Rotation Integral
We need enough observations to sort out various contributions to coronal density and magnetic field
Conclusions
• Measurements consistent with coronal field of 30-80mG at r=6R. (Paetzold et al 1987)
• Future observations could more effectively constrain the functional form of the coronal magnetic field.
• Rotation measure changes substantially on timescales of a few hours; too slow to be turbulence. Thus “Mesoscale Plasma Structures”.
• Smaller, faster fluctuations attributable to waves seen in spacecraft beacon data.