Xie – STEREO SWG – Dublin – March 2010 Low Mass Coronal Mass Ejections Missed by STEREO A/B or LASCO and Associated ICMEs H. Xie 1,2, O. C. St. Cyr 2,

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Presentation transcript:

Xie – STEREO SWG – Dublin – March 2010 Low Mass Coronal Mass Ejections Missed by STEREO A/B or LASCO and Associated ICMEs H. Xie 1,2, O. C. St. Cyr 2, N. Gopalswamy 2 and J. Davila 2 1 CUA 2 NASA/GSFC

Xie – STEREO SWG – Dublin – March 2010 DATA COR1 CME preliminary list : LASCO CME Catalogue: STEREO image search tool / movie maker : UCLA ICME list: STEREO level2 IMPACT magnetic and PLASTIC solar wind Data at UCLA aten.igpp.ucla.edu/forms/stereo/level2_plasma_and_magnetic_field.html aten.igpp.ucla.edu/forms/stereo/level2_plasma_and_magnetic_field.html NSSDC OMNI 2 data

Xie – STEREO SWG – Dublin – March 2010 OUTLINE 1. Scientific Background: Thomson scattering; brightness vs. CME longitude 2. Case study: faint CMEs missed by either STA or B (/LASCO) and associated ICMEs. 3. Properties and propagation of faint CMEs. 4. Statistics: CME missing rate of STA/B.

Xie – STEREO SWG – Dublin – March 2010 B e /B 0 vs  at various R in where, B 0 = B e (R in,,  ) at R in = 3 R s &  = 0. White-light brightness are from Thomson scattering of electrons in the corona (Billing, 1960): B tot = N e  B e (R in,  ), where B e (R in,  ) is the scatting function for a single electron. CME Brightness

Xie – STEREO SWG – Dublin – March 2010 CME: 2008/12/12 04:35; Speed: 252 km/s; A-B sep ang: 86.7 STB: Bright nice FR, nice EUVI 304 EP, N21W52 STA: Wider & fainter, nice EUVI 304 EP, N21E34 LASCO: Faint partial halo, MLSO H  DSP, ~DC N21W08 B (W52)A (E34)LASCO (W08)

Xie – STEREO SWG – Dublin – March D triangulation (solarsoft: scc-measure) CME heliographic loc: N21W08 Dtb: 12/16 10:36 UT ICME: 12/17 04:00-18:00UT Bmax = 9. 8 nT, Vmax = 340 km/s

Xie – STEREO SWG – Dublin – March 2010 STB/COR Not seen N03E13 LASCO/C3 2008/06/02 04:16 N03E38 STA /COR1 2008/06/01 09:05 N03E67 CASE 1: a CME missed by STB CME: 2008/06/01 not seen in B (E13) LASCO(E38), A(E67) Speed: 222 km/s Nice MC : Bmax = nT, Vmax = 430 km/s B (E13)LASCO (E38)A (E67)

Xie – STEREO SWG – Dublin – March 2010 In situ STB (IMPACT & PLASTIC)‏ Shock: 2008/06/06 15:36 ICME: 06/06 19:00 ~ 06/07 14:00 DT: 19 hr Bmax: 14.8 nT Vmax: 430 km/s Comment: Nice B-rotation, low Beta

Xie – STEREO SWG – Dublin – March 2010 STA Not seen S09E14 LASCO/C2 2009/01/21 18:54 S09W29 STB /COR1 2009/01/21 16:45 S09E76 A (E14) B (W76) LASCO (W29) CASE 2: a CME missed by STA CME: 2009/01/21 not seen in STA (E14) LASCO(W29), B(W76) Speed: 227 km/s

Xie – STEREO SWG – Dublin – March 2010 In situ STA (PLASTIC)‏ Shock: 2009/01/25 19:22 ICME: 01/25 22:00 ~ 01/27 05:00 DT: 31 hr Bmax: 11.5 nT Vmax: 400 km/s Nice B-rotation, low Beta In situ STA (PLASTIC)‏ Shock: 2009/01/25 19:22 ICME: 01/25 22:00 ~ 01/27 05:00 DT: 31 hr Bmax: 11.5 nT Vmax: 400 km/s Nice B-rotation, low Beta In situ L1 sc (OMNI)‏ Shock: 2009/01/25 20:52 ICME: 01/26 06:00 ~ 01/26 16:00 DT: 31 hr Bmax: 9.5 nT Vmax: 400 km/s Nice B-rotation, low Beta

Xie – STEREO SWG – Dublin – March 2010 In situ STB (PLASTIC)‏ Shock: 2008/12/07 ~03:46 ICME: 12/07 17:00 ~ 12/08 22:00 DT: 29 hr Bmax: 19 nT Vmax: 350 km/s Nice B rotation; compressed by a HSS at the rear of ICME CASE 3: a CME missed by COR1 and COR2-B CME: 2008/12/01 not seen by B (W02) LASCO(E41), A(E83) COR2 only Speed: 227 km/s A (E83)LASCO (E41)

Xie – STEREO SWG – Dublin – March 2010 Table 1: ICME disturbance date & time; CME date, time and location; and shock (dtb) travel time Ref: UCLA ICME list (2007/09 ~ 2009/01):

Xie – STEREO SWG – Dublin – March 2010 Statistical results Most ICMEs are associated with faint CMEs missed either by STA or B (15 out of 17), red bars in left panel, 7 missed by A and 8 missed by B; 2 CMEs (grey bars in left panel) are bright. 12 of 17 ICMEs are preceded by shocks Average speed of 15 faint CMEs: 229 km/s (left ) Average CME-driven shock or disturbance travel time: 111 hrs (middle) The predicted travel time error by ESA: 12 hr (right) Ref: ESA--Empirical Shock Arrival model(Gopalswamy et al., 2005)

Xie – STEREO SWG – Dublin – March 2010 Statistics: CME missing rate & CME total rate The missing rate reaches maximum of ~ 0.4 CMEs/day when A-B separation angle is ~100 degrees on Jun CME total rate around Jun-09 is overrated due to A & B has larger possibilities seeing different events CME separation rate of A & B rose starting on Oct-2009, consistent with SSN curve (dash line in bottom panel. SOHO LASCO CME Rate in was ~0.5 CMEs/day CME total rate vs. STA (B) rate CME total rate vs. Missing rate

Xie – STEREO SWG – Dublin – March 2010 Conclusions Faint CMEs are important sources for the shocks and ICMEs detected at 1 AU during solar minimum. CME monthly averaged daily rate has started to pick up since Oct-2009.

Xie – STEREO SWG – Dublin – March 2010 Table 2: CME (STA/B, LASCO) first appearance time and location ref CME missing rate