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The formation heights of CME-driven The formation heights of CME-driven shocks using empirical Alfvén maps of the shocks using empirical Alfvén maps of the
solar coronasolar corona
Pietro Zucca, Eoin Carley, Shaun Bloomfield, Peter
Gallagher
Trinity College Dublin
School of Physics, Trinity College Dublin, Ireland
OverviewOverview
• Shocks in the solar corona and their radio signature
• Density and Alfvén speed of the solar corona
• Study of 2011 September 22 Type II radio burst
• Results and conclusions
Type II radio burstType II radio burstPlasma Emission Shock Condition
Rosse Solar Terrestrial Observatory (RSTO; Zucca et al. 2012)
(ne,t) (r,t)ne(r) model
From density to heightFrom density to height
2 orders of magnitude
Density Map with SDO/AIA and Density Map with SDO/AIA and SOHO/LASCOSOHO/LASCO
B-Field with PSFFB-Field with PSFF
Emission MeasureEmission Measure
Aschwanden et al. (2011)
1918 20 21 22 23
Emission Measure to Emission Measure to DensityDensity
Menzel (1936)
The density can be estimated if we know the LOS length S(x,y)
Plane Parallel Solution
Combined Model
Density ModelsDensity Models
Spherical Symmetric Solution
SDO/AIA data
SOHO/LASCO data
Polar density MapPolar density Map
SDO/AIA 1-1.3 R
SOHO/LASCO 2.5-6 R
Model 1.3 - 2.5 R
Electron Density [cm-3][email protected]
Density / Position Density / Position AngleAngle
Alfvén Speed MapAlfvén Speed Map
2 RSun
150 300 600 1250 2500 5000
[email protected] et al. 2013, A&A in prep
Study of 2011 Sep 22 Type II radio burstStudy of 2011 Sep 22 Type II radio burst
Using the 2D density and Alfvén maps
Height-time Height-time comparisoncomparison
EUV propagating feature Type II radio burst
ConclusionsConclusions
• 2D density and Alfvén maps
• Non-radial study of Type II burst – CME
• Shock formed in the ‘Upper-flank’ region
