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January 30 2006Nobeyama radioheliograph visit Microwave Signatures of Fast CMEs Nat Gopalswamy NASA Goddard Space Flight Center Greenbelt MD 20771 USA.

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Presentation on theme: "January 30 2006Nobeyama radioheliograph visit Microwave Signatures of Fast CMEs Nat Gopalswamy NASA Goddard Space Flight Center Greenbelt MD 20771 USA."— Presentation transcript:

1 January 30 2006Nobeyama radioheliograph visit Microwave Signatures of Fast CMEs Nat Gopalswamy NASA Goddard Space Flight Center Greenbelt MD 20771 USA

2 January 30 2006Nobeyama radioheliograph visit Plan of study Select all CMEs with speed > 1500 km/s for the period 1996-2005 Look for eruptive and flare signatures If eruptive, compare kinematics from NoRH and LASCO Distinguish disk and Limb Signatures Make new images if needed

3 January 30 2006Nobeyama radioheliograph visit Motivation Fast and Wide CMEs important for space weather Identifying a microwave signature may be a useful tool to characterize these CMEs

4 January 30 2006Nobeyama radioheliograph visit Initial set of fast events (speed V > 1500 km/s) to look for Microwave activity (38 events in Nobeyama Time Window) ----------------------------------- CME first appearance V(km/s) Preliminary Survey ----------------------------------- 1998/03/31 06:12:02.000 1992 1998/04/23 05:27:07.000 1618 One frame shows eruption 5:46:20 east limb 1998/05/09 03:35:58.000 2331 03:36 - 04:26 west limb 1998/06/04 02:04:45.000 1802 NW limb NoRH PE at 1:36 (not in catalog), EIT dimming 1:58 2000/05/12 23:26:05.000 2604 NoRH Data gap? 2000/11/08 23:06:05.000 1738 double eruption (GRL), two NORH AFs 2000/11/25 01:31:58.000 2519 NE quadrant appearance of an elongated feature before flare 2001/04/03 03:26:05.000 1613 something disappears bet 3:05 &3:25 above AR EIT dim3:05 2001/04/05 02:06:06.000 1857 (narrow) diffuse behind the limb? Flare in the east 2001/04/10 05:30:00.000 2411 disk event 2001/04/18 02:30:05.000 2465 well studied. 2001/05/30 00:06:07.000 2087 PE (not cataloged) 00:00 to 00:20 east limb 2001/06/11 04:54:05.000 1647 (narrow 37 deg) 3:50-4:10 nonradial ejection? 2001/08/15 23:54:05.000 1575 backside nothing in NoRH obvious 2001/11/25 23:06:54.000 1574 onset before NoRH obs start 2002/04/21 01:27:20.000 2393 studied 2002/05/22 03:50:05.000 1557 interaction event; cataloged; need shifted HR images 2002/05/30 05:06:05.000 1625 EIT at 4:48; 4:55 noRH brightening 2002/07/23 00:42:05.000 2285 rhessi HR images available? 2002/08/24 01:27:19.000 1913 good event HR images needed 2002/09/27 01:54:05.000 1502 SW narrow; eruption at 1:30 SW 2002/10/27 23:18:13.000 2115 two events? this CME source is backside? EIT 304 2002/11/10 03:30:11.000 1670 ejecta at 3:20 SW 2003/01/22 23:54:05.000 1855 (jet) poor images 2003/05/31 02:30:19.000 1835 no EIT westward extension 17 GHz at 2:38; changes ~2:20 SW 2003/06/02 00:30:07.000 1656 eruption 00:00 to 00:10? 2003/06/15 23:54:05.000 2053 change at~23:10 above east limb; elongation of 17 Ghz at 23:56 2003/06/17 23:18:14.000 1813 flare started before obs. start 2003/10/31 04:42:50.000 2126 (narrow) PE 4:40 - 5:00 not cataloged 2003/11/09 06:30:05.000 2008 backside east limb 2004/01/07 04:06:07.000 1581 PE 4:10-4:40; first brightening at 3:50 2004/01/08 05:06:05.000 1713 elongated feature disappears near AR after brightening; same AR 2004/04/11 04:30:06.000 1645 SW quad 4:00-4:10 ejection 2004/11/10 02:26:05.000 3387 NW quad EW arcade 2005/01/15 06:30:05.000 2049 NNW quad bright arcade 2005/01/15 23:06:50.000 2861 bad images 2005/07/27 04:54:05.000 1787 4:30-510 PE not cataloged 2005/07/30 06:50:28.000 1968 PE not cataloged? ---------------------------------------------------------

5 January 30 2006Nobeyama radioheliograph visit Related issues

6 January 30 2006Nobeyama radioheliograph visit Extend the PE-CME Relationship to 2005

7 January 30 2006Nobeyama radioheliograph visit Low Frequency Type II Bursts, CMEs, and Space Weather Nat Gopalswamy NASA Goddard Space Flight Center Greenbelt MD 20771 USA Observing metric type II bursts alone is not enough to track CMEs into the Heliosphere

8 January 30 2006Nobeyama radioheliograph visit Why Study Low-frequency Type II Bursts? Among solar radio bursts, type II bursts are important for space weather because they help remote-sense large- scale mass motion Type II bursts at decameter-hectometric (DH) and longer wavelengths are indicative of fast and wide CMEs that are geoeffective & SEPeffective SEP events due to CME-driven shocks & geomagnetic storms happen when CMEs impinge on Earth’s magnetosphere Type II bursts are also indicative of large-scale interplanetary disturbances that may impact other locations in the heliosphere (e.g. at and enroute to Mars)

9 January 30 2006Nobeyama radioheliograph visit Sources of Geoeffective & SEPeffective CMEs 15W N S WE O Dst < - 200 nT O - 300nT < Dst < - 200 nT O Dst < - 300 nT 37/55 = 67% 18/55 = 33% SEP Type II bursts can detect both of these populations

10 January 30 2006Nobeyama radioheliograph visit Interplanetary (1973: Malitson et al.) Coronal (1947) Nelson & Labrum, (1985) Gap filled by Wind/WAVES At Decameter-Hectometric (DH) Wavelengths (Bougeret et al. 1995) Ionospheric Cutoff 1.5 2.5 20 Rs 214 Type II, Type III bursts Type III storms are observed in the IP medium Some type IV less complex SOHO/LASCO FOV 2-32 Rs

11 January 30 2006Nobeyama radioheliograph visit 2005/09/10 22:37 UT CME 1893 km/s PA120 Very intense type II radio bursts: Shock-driving capability of CMEs. 1-14 MHz crucial because the associated CMEs just leave the Sun Sky-plane height of the CME is ~9 Ro 8.56 Ro 800 kHz “The bow shocks of fast, large CMEs are strong interplanetary (IP) shocks, and the associated radio emissions often consist of single broad bands starting below ~4 MHz; such emissions were previously called IP type II events.” Cane & Erickson 2005

12 January 30 2006Nobeyama radioheliograph visit IP type II bursts “The bow shocks of fast, large CMEs are strong interplanetary (IP) shocks, and the associated radio emissions often consist of single broad bands starting below ~4 MHz; such emissions were previously called IP type II events.” “… metric type II bursts, unlike IP type II events, are not caused by shocks driven in front of CMEs.” Cane & Erickson 2005

13 January 30 2006Nobeyama radioheliograph visit A DH Type II & its CME f =0.85MHz  fp = 0.425 MHz  n = 2.2x10 3 cm -3 when the CME is at 30 Rs Vcme ~ 770 km/s Radio emission tracks CME beyond LASCO FOV 2.86 Rs 3.98 Rs15.58 Rs22.21Rs No Type II yet CME at edge of C3 FOV (30 Rs) at the edge of C2 FOV Type II starts

14 January 30 2006Nobeyama radioheliograph visit Type II in various Wavelength Ranges m DH km km type II Metric Type II DH Type II m-km Type II (m not shown) DH Type II (no m) Observed type II features: m – pure metric (ground); DH-decameter-hectometric; km – kilometric; some start at m and go all the way to km (m-to-km) f t

15 January 30 2006Nobeyama radioheliograph visit Type II Bursts Organized by CMEs m DH km Speeds, widths & deceleration of CMEs progressively increase for metric, DH, full- range (m-to-km) Type II Bursts, compared to the general population Purely km type IIs due to accelerating CMEs, which form shocks far away from the Sun

16 January 30 2006Nobeyama radioheliograph visit Properties of CMEs associated with m, DH and m-to-km type II’s compared to those of all CMEs CME PropertyAllmDHmkm SEP km Speed (km/s)48761011151490 1524 539 Width (deg)4596139171 186 80 Halos (%)3.33.845.271.4 72 17.2 Acceleration(m/s 2 )-2-3-7-11 +3 m-to-km (mkm) CMEs similar to SEP-producing CMEs km CMEs similar to metric CMEs, but acceleration is different m DH km

17 January 30 2006Nobeyama radioheliograph visit SEP & m-to-km Events CME PropertyAllmDHmkm SEP km Speed (km/s)48761011151490 1524 539 Width (deg)4596139171 186 80 Halos (%)3.33.845.271.4 72 17.2 Acceleration(m/s 2 )-2-3-7-11 +3 CME PropertyAllmDHmkm SEP km Speed (km/s)48761011151490 1524 539 Width (deg)4596139171 186 80 Halos (%)3.33.845.271.4 72 17.2 Acceleration(m/s 2 )-2-3-7-11 +3 Similar number of SEP and m-to-km events  same shock accelerates electrons and protons Difference due to connectivity for particle and wider beam for bursts 33.8% of m-to-km events to the east of W10; only 13.8% of SEP events to the east of W10

18 January 30 2006Nobeyama radioheliograph visit SEP Release height Leading edge of the CME at the time of GLE release

19 January 30 2006Nobeyama radioheliograph visit Shocks & Type IIs Close similarity between rates of SEP events, IP type II bursts & in situ shocks Electron and proton acceleration by the same shock IP

20 January 30 2006Nobeyama radioheliograph visit CMEs Relevant for Space Weather electron Acceleration (CME shock) proton Acceleration CME shock Plasmag Impact CME CMEs of heliospheric consequences V  1000 km/s

21 January 30 2006Nobeyama radioheliograph visit Characteristic Speeds “1980s view” of Alfven speed Region 1: Difficult to make Type II bursts – explains Type II starting f ~150 MHz Region 2: Easy to make Type IIs below 2.5 Ro (m) Region 3: IP medium – Very Fast CMEs & accelerating CMEs produce type II Krogulec et al 1994 Mann et al. 1999 Gopalswamy et al. 2001

22 January 30 2006Nobeyama radioheliograph visit Occurrence Rates 10% of CMEs & 5% of flares have type IIs m type IIs most abundant m type IIs 2-3 times more abundant than IP type IIs

23 January 30 2006Nobeyama radioheliograph visit Starting frequency & CME height Type II behind CME leading edge Type II & CME in different directions IP and metric drift rates can be Different if the acceleration Initially occurs in the Qperp region and later (IP) in the Q|| region (Holman & Pesses,1983)

24 January 30 2006Nobeyama radioheliograph visit Two possible Type II Locations Flanks: Lower Alfven speeds expected. For a given CME speed, there may be a shock at the flanks, while no shock at the nose Shock may be Quasiperp at the CME flanks while quasiparallel at the nose Flank NOSE

25 January 30 2006Nobeyama radioheliograph visit m-to-km Type II bursts and Space Weather Less than 1% of the 9000 CMEs observed during 1996-2004 were associated with the m-to- km type II bursts. Therefore, the m-to-km bursts can isolate the small fraction of CMEs that are likely to have significant impact on the inner heliosphere It takes typically about an hour for the disturbances to reach km level Very useful for ESPs and SSCs Maybe useful for SEPs

26 January 30 2006Nobeyama radioheliograph visit 2005 Jan 17 AR 720

27 January 30 2006Nobeyama radioheliograph visit Interaction Event 2548 km/s 2094 km/s

28 January 30 2006Nobeyama radioheliograph visit Summary The speed and width of CMEs progressively increase in the following order: general population, metric- associated, DH-associated m-to-km-associated m-to-km CMEs similar to SEP-producing m-to-km type IIs probe the entire Sun-Earth connected Space and the energetic CMEs propagating throughout this region. They can predict shocks of significance to Earth and other destinations in the heliosphere m type IIs alone cannot tell whether the CMEs are geoeffective. They need to have IP counterpart.

29 January 30 2006Nobeyama radioheliograph visit Additional Comments Imaging the type IIs is ideal (SIRA) Otherwise, at least we need direction finding at sufficiently high frequencies (above 1 MHz) The lower sensitivity at higher frequencies is one thing that needs to be avoided RPW should be able to measure shock strength when the shock is still closer to the Sun

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