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Pietro Zucca, Eoin Carley, Shaun Bloomfield, Peter Gallagher
Trinity College Dublin The formation heights of CME-driven shocks using empirical Alfvén maps of the solar corona Pietro Zucca, Eoin Carley, Shaun Bloomfield, Peter Gallagher School of Physics, Trinity College Dublin, Ireland
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Overview 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
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Type II radio burst Plasma Emission Shock Condition
Rosse Solar Terrestrial Observatory (RSTO; Zucca et al. 2012)
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From density to height (ne,t) ne(r) model (r,t) 2 orders of magnitude
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Alfvén Speed Mann et al. 2002
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Alfvén Speed 2D Model Warmuth et al. (2005)
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Density Map with SDO/AIA and SOHO/LASCO
B-Field with PSFF Density Map with SDO/AIA and SOHO/LASCO
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Emission Measure 18 19 20 21 22 23 Aschwanden et al. (2011)
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Emission Measure to Density
The density can be estimated if we know the LOS length S(x,y) Menzel (1936)
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Density with SOHO/LASCO
Hayes et al. (2001)
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Density Models SDO/AIA data Spherical Symmetric Solution
Combined Model SOHO/LASCO data Plane Parallel Solution
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Polar density Map SDO/AIA 1-1.3 R Model 1.3 - 2.5 R SOHO/LASCO
Electron Density [cm-3]
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Density / Position Angle
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Electron Density Map LASCO 2.5 R MODEL 1.3 R SDO
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Magnetic Field zuccap@tcd.ie Magnetic field [Gauss] 0.1 0.5 2.5 15 90
500 Magnetic field [Gauss]
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Alfvén Speed Map zuccap@tcd.ie 2 RSun Zucca et al. 2013, A&A in prep
150 300 600 1250 2500 5000 2 RSun Zucca et al. 2013, A&A in prep
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Study of 2011 Sep 22 Type II radio burst
Using the 2D density and Alfvén maps
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CME eruption
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Non-radial kinematics
EUV Height time Type II Height Time
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Height-time comparison
EUV propagating feature Type II radio burst
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Matching Kinematics 90-70 MHz
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Matching Kinematics 150 MHz
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Matching Kinematics 150 MHz 150 MHz from NRH
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Alfven Speed
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Matching Kinematics 90-70 MHz
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Conclusions 2D density and Alfvén maps
Non-radial study of Type II burst – CME Shock formed in the ‘Upper-flank’ region
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