# Presentation: 446981

## CMEs OBSERVED IN THE HELIOSPHERE BY

**THE SOLAR MASS EJECTION IMAGER (SMEI)**
**David Webb, D. Mizuno & T. Kuchar, *****Boston College***
**J. Johnston & R. Radick, *****Air Force Research Lab, ***
***  ******	******	******	******	******Space Vehicles Directorate***
**B. Jackson, *****CASS; Univ. of California-San Diego***
**G. Simnett & J. Tappin, *****Univ. of Birmingham, UK***

** ****Heliospheric Mapping**
** ****Search Criteria & Data Products**
** ****Types & Characteristics of CMEs**
** ****CME Studies & Results Summary**
** ****SMEI + STEREO + Solar-B**

## SMEI Fields of View

**SMEI Fields of View**

**C1**

**C2**

**C3**

**Cam**
**3**

**Cam1**

**Cam2**

## Frame Composite for Hammer-Aitoff Projection:

**Frame Composite for Hammer-Aitoff Projection:**
**the “Standard” SMEI View**

**Cam 3**
**Cam 2**
**Cam 1**

**Every 30****th**** camera **
**frame during **
**one orbit shown**

## SMEI Aitoff View & LASCO Comparison

***Blue arrows - obscured data from particle enhancements incl. SAA, auroral light, zone of exclusion and shuttered areas. ***

***Left: SMEI composite all-sky image with LASCO coronagraph field (blue) overlaid and CME superimposed. Top: SMEI and LASCO fields overlaid.***

**SMEI Aitoff View & LASCO Comparison**

## Search Criteria & Data Products: SMEI CMEs

**A)  Limb CMEs****	****	****	****	****  50%?**
**B)  Erupting prominences with CMEs****	****>4%  (>6)**
**C)  Multiple CMEs****	****	****	****	****  25%**
**D)  Distant wide arcs****	****	****	****~30%**
**E)  Concave-outward V-shaped CMEs****	****  3%  (4)**
**F)  Earthward (“halo”) CMEs****	****	****~30%**

**Search Criteria & Data Products: SMEI CMEs**

** ****Search uses near-real time processed Aitoff all-sky maps**
**	****- ****Orbital difference movies**
** ****Observation period searched: **
**	****- 6 February 2003 – end August 2004**
**	****- Statistical study over first 1.5 years**
**	****- CME list being updated thru present**
** ****Data Products:**
**	****- ****Event files of images of each CME**
**	****- Movies of each CME**
**	****- File of comments for each CME**
**	****- Summary event list**

## (A)  A Fast Limb CME

- CCMC_2003

**(A)  A Fast Limb CME**

**31 May 2003**

**Speed:    LASCO C3:  1765 km/s   **
**	****    ****SMEI:           ~1450 km/s **

## Distance-Time Plot of 31 May Limb CME

**Distance-Time Plot of 31 May Limb CME**

## (B)  An EPL/CME: Sun Surface to 35o Elongation

**(B)  An EPL/CME: Sun Surface to 35****o ****Elongation**
***February 2004***

**EIT**
**15, 00 – 10**

**LASCO C2**
**15, 05:30**

**LASCO C3**
**15, 11:42**

**SMEI**
**Orbit diff.**
**16, 07 – 24**

## (C) Multiple CMEs & (D) Distant Arcs

***	******        ******At least 4 separate CMEs! ***
**Slow, bright, bent arc to NW  (Cam 3 into 2; lasts 2 days!)**
**Faint, wide arc over NP**
**2 wide arcs to E & NW  (NOT Halos!  Cam 2 into 1)**

## E)  Concave-outward CME Structures

***26 July 2003***
***NW of Sun***

***13 March 2003***
***NNE of Sun***

***25 April 2003***
***NNW of Sun***

**Orbit-to-orbit difference images. Sun located at ‘+’ signs. Exclusion zone circle is 20****o**** in radius.**

***28 May 2004***
***NNE of Sun***

## (F) First Earth-Directed CME Seen by SMEI

**(F) First Earth-Directed CME Seen by SMEI**
**28-29 May 2003**

***Tappin et al., GRL, ***_***31***_***, 2004***

## (F) SMEI Ecliptic “fisheye” Maps of Oct. 28-29, 2003 CME

***EIT 195A***
***Oct. 28, 11:12***

***LASCO C2***
***Oct. 28, 11:30***

## Elongations Observed for CMEs

**Elongations Observed for CMEs**

***First Observed***

***Last Observed***

## Identifying Earthward CMEs in SMEI

** ****Large Storms ******** SMEI CMEs**
**	****Study of all intense storms (peak *****Dst***** < - 100nT), **
**	****      ****Feb. 2003 - Jan. 2005; 2 years**
**	****- ****Of 21 storms, 3 inadequate SMEI obs., 1 not examined, 1 due**
**	****      ****to shock sheath;**
**	****- Of 16 remaining, ****87.5%**** (14/16) storms had assoc. SMEI CMEs. **
**	****      ****All CMEs were at large elongations (> 60****o****) at storm onset.**
**	****      ****All 16 storms had assoc. SMEI aurora.**
**	****- *****TIMINGS:***
**	****      ****ΔT, 1 AU shock arrival - SMEI first obs. = 19.2 hr. (range 9-26 hr.)**
**	****      ****ΔT, onset of storm - SMEI first obs. = 29.2 hr. (range 18-42 hr.)**
**	****Study of all moderate storms (peak *****Dst***** < - 60nT), **
**	****      ****Mar. 2003 – Feb. 2005; 2 years**
**	****- For ****85%**** (39 of 46) SMEI saw a CME within 2 days prior.**
** ****1 AU Shocks ******** SMEI CMEs****	**
**	****Study of 1 AU shocks; ACE, WIND (in-situ) & LASCO (CMEs)**
**      ****1998 - present**
**- Nearly all 1 AU shocks are assoc. with CMEs.**
** ****20 shocks assoc. with SMEI CMEs (13 also with storms).**
** ****But these CMEs not atypical; e.g., elongation, spans.**

##  Complete LASCO ↔ SMEI Comparison Study

** ****Preliminary SMEI ******** LASCO Comparison Study**
**	****- ****Simnett study:   February – December 2003**
**	****- 71% (57/80) of SMEI CMEs associated with obvious LASCO CMEs.**
**	****- ****14%**** (11/80) associated with very faint LASCO CMEs.**
**	****- The remaining ****15%**** (12/80) have no associated LASCO event.**

** ****Complete LASCO ****↔**** SMEI Comparison Study**
**	****- Underway: 3-year NASA grant;  SMEI Team with NRL**
**	****- SMEI sees fewer CMEs than LASCO over same period. Why?**
**	****	****	****	**** ****Because of operational down time for tests and calibrations.**
**	****	****	****	**** ****Partial spatial obscurations; particles, aurora, sunlight.**
**	****	****	****	**** ****Some CMEs seen in LASCO close to the Sun fade with height.**
**	****	****	****	**** ****Sequences of events in LASCO manifest as a single feature in SMEI.**

## Statistical Results Summary: SMEI CMEs

** ****SMEI has observed 139 CMEs in 1.5 years and 204 CMEs in 2.5 yr.**
**	****Est. occurrence rate = ****0.31 CMEs/day**
** ****Brightness:  Mean = 1.25 adu; ****2.3 S10**** units  (range = 0.4 - 11 S10)**
**	****(based on preliminary calibration: 1 S10 = 0.55 adu)**
**	****Helios-2*: Mean = 2.3 S10   (1.5 - 2.95; 1976-1979)**
** ****Spans (detected):  Mean ****> 42****o****;  Range = 3 – 107****o**** **
**	****LASCO*: Mean = 60****o**** (median = 42****o****)**
**	****Helios-2*: Mean = 53****o****   (1976-1979)**
** ****Durations:   Mean ****15.6 hr****.;  Range = 3 – 72 hr.**
**	****Helios-2*:  Mean = 37 hrs.   (1976-1979)**
** ****Speeds:  Angular mean = ****1.1****o****/hr****. P-approx. mean = ****482 km/sec**
**	****LASCO*: Mean = 507 km/sec**
**	****Helios-2*: Mean = ~500 km/sec   (1976-1979)**
** ****SMEI detected ~20 halo CMEs at ~1/3 of Sun to Earth distance.**
**	****Can detect CMEs 10 hr. to 1+ days before Earth arrival.**
**	***** LASCO results courtesy S. Yashiro & N. Gopalswamy; **
**	****  ****Helios-2 results from Webb & Jackson, JGR, 95, 1990.**

## SMEI Information Sources

** ****Instrument paper:  *****Eyles et al., Solar Phys., ***_***217***_***, 319, 2003***** **
*** “*****Mission” paper:*****	******Jackson et al., Solar Phys., ***_***225***_***, 177, 2004***
** ****URL for SMEI instrument description & general **
**information:**
***	******http://www.vs.afrl.af.mil/ProductLines/SMEI/***
** ****URL for SMEI images & movies:**
***	******http://smei.nso.edu/***

**SMEI Information Sources**

## Possible SMEI-STEREO-Solar-B Joint Science 

***Overlap of the Missions***
**SMEI launched on STP Coriolis mission Jan 2003**
**STEREO launch May/June 2006; Solar-B launch Sept. 2006**
**SMEI nominal mission 3 years; 5 year design lifetime**
**Main degradation: Sunward camera signal-to-noise**
**	****- Uploading bad-pixel mask**
**Continuing operations ($2M/year) depend on:**
**	****- Success of Navy Windsat experiment**
**	****- AFRL finding support if Windsat fails**
***Space Weather***
**Onset & source structure; Solar-B provides B-field**
**Different views of Earthward CME: SMEI - Head-on; STEREO HIs - Side-on**
**HIs: 3-D images early in mission; Triangulation later**
**Determine trajectory, time of arrival & strength of CME. **
**But CME rate low: CME rate at solar minimum 0.5-1/day**
***SMEI Provides Context of Heliospheric Structures***
**Movies of corotating structures & CMEs (3D recontructions)**
**Time-of arrival of structures at STEREOs**
**	****- Intercomparison of remote sensing & in-situ meas.**
**	****- Tests of heliospheric models**

## 3-Point Measurements of Large-Scale Structures

**SMEI + near-Earth/L1spacecraft + 2 STEREOs**
**	****- In-situ measurements of plasma & IMF: L1 + STEREO in-situ**
**	****- Density/Mass measurements from SMEI + STEREO HIs**
**	****  ****Comparison with Solar-B & COR1, COR2 measurements**

## THE  END

## SMEI CME Studies & Collaborations

** ****Improved calibrations & reprocessing of existing data.**
** ****3D reconstruction of IP density enhancements (CMEs **
**  ****& corotating structures) and kinematics**
** ****Some collaborations with other data sets:**
**	*****- LASCO comparison***
***	******- Ulysses on CME kinematics ***
***	******- ICMEs & Forbush decreases***
***	******- IPS comparison***
***	******- Wind/WAVES***
***	******- SOHO SWAN (St. Cyr)***
** ****Space Weather modeling: HAF & other IP model**
**  ****comparisons.**

## SMEI Presentations/Papers

_**Published**_
** “****Instrument” paper****	****	*****Eyles et al., Solar Phys., 2003***** **
** ****May 2003 Halo CME – storm****	*****Tappin et al., GRL, 2004***
*** “*****Mission” paper*****	******	******Jackson et al., Solar Phys., 2004***
** ****Oct-Nov 2003 period****	****	*****Webb & Allen, Space Weather, 2004***
_**In-press**_
** ****3D reconstr. of Oct-Nov 03 events  *****Jackson et al., JGR, 2005***
** ****Wind/WAVES – SMEI CMEs****	*****Reiner et al., JGR, 2005***
** ****Survey of Halo CMEs ****	****	****T. *****Howard et al.***
** ****CMEs & Ulysses kinematics****	*****Tappin, Solar Phys., 2005***
*** *****SMEI-IPS; Oct. 2003*****	******	******Tokumaru et al., URSI, 2005***
_**In progress**_
** ****First-year CME statistics****	*****Webb et al.***
** ****Space weather****	****	****	*****Fry et al.; Webb et al.***
** ****ICMEs & Forbush decreases****	*****Simnett, Kahler (ICRC)***
** ****Comparison SMEI & IPS data****	*****Jackson, Tokumaru***
*** *****Comet tail disconections****	*****Kuchar et al.***
_**>40 talks/abstracts**_
** ****2 AGU Special Sessions**
_**16 popular articles or press releases**_

## Some Speculation

** ****CME Morphology: **
**More structured nearer Sun (Cam 3): **
***- True limb CMEs show more structure***
***- So do CMEs with erupting prominences***
**Broad arcs far from Sun (Cams 2 & 1):**
***-***** *****Shock or shock sheath?***
***- Compressed leading edge of ejecta?***
**Distant concave-outward structures:**
***- Evolved prominence material?***
** *****CME front encountering gradient in ***
***  ******solar wind flows?***** **

** ****SMEI vs LASCO: ~half of SMEI CMEs likely assoc. with LASCO CMEs. Detailed comparison to come.**
***- But many LASCO CMEs fade < 10Rs!***
*** ******Why? Density decrease, turbulence, merge with solar wind, propagation direction, other??***

**C2**

**C3**

## UCSD Editing Sequencesfor SMEI

**SMEI Zodiacal cloud Subtraction from a model fit.**

**UCSD Editing Sequences****for SMEI**

**How to determine the zodiacal cloud.**

**How to remove it.**

**Determine an Analytical Zodiacal Light Model Best Fit from a Minimum in Elongation – Position Angle Coordinates Folded into Four Quadrants. Residuals Minimized to Give Best Fit Model.**

**Remove the Best Fit Analytic Zodiacal Model from a Sidereal Map to Determine the Stellar Background. **

**Remove the Sidereal Stellar Background from the Original Data to Determine the True Zodiacal Light Using the Minimum in Elo. – P.A. for an Average of only a Few Orbits and to Check the Zodiacal Light Model Against the True Values Of Zodiacal Light.**

**3-D Reconstruction of CMEs Using SMEI**

## UCSD Editing Sequence

**UCSD Editing Sequence**

**Zodiacal light and Removal**

**3-D Reconstruction of CMEs Using SMEI**

## UCSD Editing Sequence

**UCSD Editing Sequence**

**3-D Reconstruction of CMEs Using SMEI**

## UCSD Editing Sequences

**Aurora Removal**

**UCSD Editing Sequences**

**Aurora recognition and removal.**
**How to know where the aurora is.**

**How to remove it.**

**Aurora Removed by Recognition of their Signal on an Orbit – Temporal Sequence Map.**

**3-D Reconstruction of CMEs Using SMEI**

## Enhanced Images from Timeseries

**Enhanced Images from Timeseries**

**26 May – 05 June 2003, (May 28 ‘Halo’ CME)**

**3-D Reconstruction of CMEs Using SMEI**

## Enhanced Images from Timeseries

**Enhanced Images from Timeseries**

**Comparison with HAF model**

**3-D Reconstruction of CMEs Using SMEI**

## 3-D Reconstruction of CMEs Using SMEI

**SMEI 3D recon-struction of the 28 May CME****. **

**Electrons are contoured with an R****-2**** density fall-**
**off between 10 - 30 e****-****cm****-3****. **

**3-D Reconstruction of CMEs Using SMEI**

## 3-D Reconstruction of CMEs Using SMEI

**LASCO C2 CME image to 6 Rs. **

**SMEI enhanced Sky Map image and animation to 110****o**** elongation. **

**C2******
**image**

**Southward  ejecta******

**Southward  ejecta******

**Northeast-directed ejecta consistent with IPS g-level observations (Tokumaru *****et al*****., 2004)**

**3-D Reconstruction of CMEs Using SMEI**

## 3-D Reconstruction of CMEs Using SMEI

**SMEI 3D recon-struction of the October 28 CME****. **

**The above structure has a mass of about 0.5 ******** 10****16****g excess in the sky plane but ~ 2.0 ******** 10****16****g excess at 60****o ****(Vourlidas, private communication, 2004).**

**Mass determination ~6.7 ******** 10****16****g excess and 8.3 ******** 10****16****g total for northward directed structure within the 10 e****-****cm****-3**** contour.**

**3-D Reconstruction of CMEs Using SMEI**

## 3-D Reconstruction of CMEs Using SMEI

**SMEI 3D reconstruction of the October 28, 2003 CME. **

**The dominant structure vanishes about 45 from the Sun-Earth line. The arch-shaped structure fades to the south of Earth.**

**3-D Reconstruction of CMEs Using SMEI**

## 3-D Reconstruction of CMEs Using SMEI

**SMEI 3D recon-struction of the October 28 CME****. **

**The above structure has a mass of about 1.5 ******** 10****16****g excess in the sky plane.**

**Mass determination ~3.6 ******** 10****16****g excess and 4.2 ******** 10****16****g total within 20 e****-****cm****-3**** contour.**

**3-D Reconstruction of CMEs Using SMEI**

## 3-D Reconstruction of CMEs Using SMEI

**SMEI reconstructed density on October 30 at 03 UT 15 e****- ****cm****-3**** to 30 e****-**** cc****-3****.**

**IPS UCSD reconstructed velocity at 03 UT viewed above 1300 km s****-1****.**

**3-D Reconstruction of CMEs Using SMEI**

## 3-D Reconstruction of CMEs Using SMEI

**	****a) Modeling: Better heliospheric modeling - ****	****incorporation of 3D MHD into the forward-****	****modeling tomographic analysis ****(****Odstrcil *****et al*****.).**
**	****b) Comparisons with STELab IPS results ****(Tokumaru ****	****et al.)**** & HAF model (****Frye et al.)**
**	****c) NRT Pipeline Processing of fully calibrated****	****   ****	****images**
**	****d) Restrospective SMEI - 3D reconstruction ****	****analysis from the entire time period observed by ****	****SMEI and comparison with other CMEs.**

**Summary/Work Needed:**

**3-D Reconstruction of CMEs Using SMEI**