alfvén waves in the solar corona s. tomczyk, s. mclntosh, s. keil, p. judge, t. schad, d. seeley,...
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Alfvén Waves in the Solar Corona
S. Tomczyk, S. Mclntosh, S. Keil, P. Judge, T. Schad, D. Seeley, J. Edmondson
Science, Vol. 317, Sep., 2007
October 31, 2007
What’s new? BIG PUZZLE: Why does the temperature of the solar atmosphere
rise from 5000 to 2 million degrees Kelvin from the photosphere outward to the corona ?
October 31, 2007
MHD Waves Modes Fast and Slow Magnetoacoustic Mode:
Compressible Susceptible to damping Intensity oscillations observed with TRACE and SOHO
Alfvén Mode: Incompressible Transverse oscillation Propagate along field line Magnetic tension as the resorting force Observed in solar wind in situ Lack definitive observation in coronal plasma
October 31, 2007
Approach and Challenge Corona and scattering light; Not visible as intensity fluctuations; Velocity fluctuations:
Doppler shifts; Spectrograph: large FOV observation take too
long time compared to the wave periods.
Infrared coronal emission line: FeXIII 1074.7 nm; Narrow-band tunable filter: Doppler and
polarimetry.
October 31, 2007
Instrument Hill-top facility at NSO/SP 20 cm One Shot Coronagraph Coronal Multi-channel Polarimeter
(CoMP) Corona emission lines: Fe XIII
1074.52, 1074.65, and 1074.78 nm
1024 x 1024 HgCdTe Detector CoMP polarimeter FOV: ± 1.4 solar radii Image scale: 4.5 arcsec/pixel Exposure time: 250 ms Bandwidth: 0.13 nm Stokes I, Q, U, V and Dopplergram
October 31, 2007
Data Acquisition Oct. 30, 2005 between 14.26 and 23.56 hour UT. Images of corona between 1.05 and 1.35 solar
radii. Fe XIII 1074.52, 1074.65, and 1074.78 nm. Stokes I+Q, I-Q, I+U, I-U. Spatial sampling: 4.5”/pixel. Cadence: 29 seconds. 70000 total images.
λ λ λ
Data
Set 1
Data
Set 2
Data
Set 3
October 31, 2007
Data Acquisition
λ λ λ
Data
Set 1
Data
Set 2
Data
Set 3
Dark and flat correction; Calibration processing; Central intensity of the line, the central
wavelength, and line width for each point in each image in the time series;
Line-of-sight (LOS) velocity; Degree of linear polarization: Azimuth angle:
Q
U1tan2
1
IUQp /)( 2/122
t
October 31, 2007
Result 3
Phase travel-time analysis
Phase speed (1.31±0.24 Mm/s); Propagation trajectory (46.2±4.0°); Correlation length (~45 Mm); Correlation width (~9 Mm);
October 31, 2007
Discussion Alfvén waves verification:
Phase speed (2 Mm/s) >> sound speed (0.2 Mm/s); Propagate along field lines; Intensity fluctuations are very small;
Presence of a 5-min signature: Tunnel through the complex chromosphere-transition region; Conversion mechanism is unknown;
Upward dominance: Energy estimation:
Energy flux not enough: Unresolved Alfvén waves ?
Coronal seismology: 1.5 ~ 5 Mm/s 8 ~ 26 gauss; Plasma density through ratio of FeXIII lines pair.
October 31, 2007
Summary An overwhelming flux of upward low-frequency wave
propagate throughout the solar corona; These waves are ubiquitous in space and time; These waves propagate at speeds typical of Alfvén
waves; Their direction of propagation mirrors the measured
magnetic field direction; The waves they resolved do not have enough energy to
heat the solar corona; They consider that these waves are indeed Alfvén waves; These waves offer the real possibility of probing the
plasma environment of the solar corona with a high degree of accuracy through coronal seismology.