Relation between Type II Bursts and CMEs Inferred from STEREO Observations N. Gopalswamy, W. Thompson, J. Davila, M. Kaiser NASA Goddard Space Flight Center,

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Relation between Type II Bursts and CMEs Inferred from STEREO Observations N. Gopalswamy, W. Thompson, J. Davila, M. Kaiser NASA Goddard Space Flight Center, Greenbelt, MD S. Yashiro Interferometrics, Herndon, VA P. Mäkelä, G. Michalek The Catholic University of America, Washington, DC J.- L. Bougeret Paris Observatory, Meudon, France R. Howard Naval Research Laboratory, Washington, DC STEREO SWG February 3-5, 2009 Pasadena Solar Physics – under review

Motivation CME leading edge at metric type II burst onset: the height of shock formation LASCO: CME leading edge associated with ~130 limb type IIs 2.2 Ro [Gopalswamy et al., 2005, JGR] – extrapolation of height-time ~1.6 Ro for type II bursts in GLE events Exploit COR1 capability: minimal or no extrapolation (FOV inner edge ~1.4 Ro) LASCO/C2 misses the early evolution Explain the universal drift-rate spectrum

Motivation: CME height at metric type II onset is generally extrapolated. SECCHI/COR1 can solve this problem Gopalswamy et al More type II bursts have spatial overlap with CMEs

Type II GLE >40 MeV >13 MeV Heliocentric Distance (Rs) Fast Mode Speed (km/s) DH 1.6 Ro4.4 Ro5.6 Ro7 Ro Gopalswamy et al., 2001, 2008 Onset of Shock, Type II, Particle Release

Speed increase in the metric corona  = 2.3  = 1.4 |df/dt| ~ f  Aguilar-Rodriguez et al., 2005; Vrsnak et al., 2001

Overview No type II since 4/26/08 10 m type IIs 6 had SWAVES (DH) 1 m to km (interplanetary) 8 in in 2008 Mostly small S/C separation (0 – 50 degrees)

Metric type II and CME Properties Date Time range f e –f s (MHz) df/dt MHz/s DH IIV C km/s V L km/s W deg AR flr Loc BE AE AB deg 07/01/25 06: : :30DG C6.3 S08E /02/19 00:18- 00: N186DG 0943 C1.1 S12E /05/19 12:51- 13: ?0.2513: B9.5 N07W /05/22 14:36- 14: ?0.05N B3.9 N02W42* /05/23 07:22- 07: N B5.3 N02W55* /06/03 09:28- 09: Y? C5.3 S08E /08/06 09:16- 09: ?0.08N C1.5 S05E /12/31 00:53- 01: ?0.1101: C8.3 S08E /03/25 18:52- 19: : M1.7 S13E /04/2614:12- 14: ? : ?? B3.8 N08E

General Results Extremely weak flares: 4 B, 5 C & 1 M Energetic CMEs: ~774 km/s, W ≥66 o V m ~ 534 km/s V DH 808 km/s V mkm 1367 km/s V COR1 < V LASCO [2 exceptions: 1 impulsive] Six of the 10 metric type II bursts had CME observation when the burst was in progress

Metric Type II 118 MHz 25 MHz 00:5201:12 df/dt ~0.1 MHz/s 01:22 DH Type II end

SWAVES Type II F H

DH Type II Type III Type II Shock?

CME at the Time of Type II DH SA COR1 01:00: :50: /12/31 COR1 & EUVI Shock CME - 01:12 SA, E, SB View: E101, S08E81, E Ro

COR1 + EUVI 284 images of the CME m-type II End m-type II Start LE 1.77 RoLE 1.6 Ro LE 2.51RoLE 2.4 Ro COR1/EUVI images available at several instances during type II The CME was in the height range 1.4 – 3.3 Ro when the type II started in the metric domain and ended in the DH domain Disturbances around the CME became clear after the type II ended

Disturbance Surrounding the CME A C B DH end 2007/12/31 COR1 & EUVI COR1 01:25: :25:53 SB

CME Speed & Va Profiles DH end 1:22 UT Va CME Speed peaks at 1:20 UT

Alfven Speed can vary by a factor of 5 N = 3.3×10 5 r – ×10 6 r – ×10 7 r –6 cm –3 2 G, 1x

Speed increase in the metric corona  = 2.3  = 1.4 Shock travels with a speed V emitting at successively lower f determined by the local plasma density: n ~ r -  or f ~ r -  /2 |df/dt| = V(df/dr) ~ Vf (  +2)/  = Vf 2 if V=const. &  =2 (Vrsnak et al., 2001) V may be slowly varying far away from the Sun, but not in the COR1 FOV  =2 may not be true Deviations imply speed increase near the Sun and decrease in the IP medium |df/dt| ~ f 

Drift – Rate Spectrum (metric) If speed varies as V~r -  ~ f 2  /  [since f ~ r -  /2 ] |df/dt| ~ f (  +2  +2)/  = f  with  = (  +2  +2)/ 

β = β = STEREO A Limb View  = (  +2  +2)/  β =   = 1.04 for  = 6 β =   = 1.05 Consistent with the observed  = 1.07

Low frequency Part If speed varies as V~r -  ~f 2  /  [since f ~ r -  /2 ] |df/dt| ~ f (  +2  +2)/  = f  with  = (  +2  +2)/ 

IP Type II Type II

Type II not Reported! 40 – 24 MHz 0.08 MHz/s

metric to kilometric Type II

Combining dynamic Spectrum with CME Height –Time F H Frequency of emission ~ CME leading edge

 = Confirms r dependence of density.  = 2.32  = (  +2  +2)/  β = 0.12   = 1.97 for  = 2.32 Consistent with the observed  = 1.85 β = 0,  = 2   = 2 Speed is ~constant within C3 FOV Try this with HI

Impulsive Event 2007 June 3 H F IZMIRAN

DH end 09:54 UT Impulsive Events CME at a height of 1.87 CME observed when metric type II in progress F

Impulsive Events DH CME peak speed at 1.5 Ro! Type II start near flare peak, speed peak Speed drops from ~925 km/s to 700 km/s during m type II and ~500 km/s at end of DH Close connection between CME speed and SXR flare light curve even for an impulsive event

Summary Metric type II burst starts at a height where the VA is minimum (~1.4 Ro) The CME height at type II onset ~1.5 Ro compared to 2.2 Ro from LASCO -Min to Max density variation (factor of 4)? -LASCO does not capture initial speed variation? Type II ends when the shock becomes subcritical or dissipates Deviations from the universal drift rate spectrum are a direct consequence of the CME speed increase in the inner corona and decrease in the IP medium GOES light curve and CME speed follow each other even for impulsive flares

Double Peak in the Event