Characterization of Coronal Mass Ejection Deflection using Coronagraph Image Sequences Jenna L. Zink, GMU Undergraduate Research Scholars Program, Rebekah.

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Characterization of Coronal Mass Ejection Deflection using Coronagraph Image Sequences Jenna L. Zink, GMU Undergraduate Research Scholars Program, Rebekah M. Evans, NASA/GSFC, ORAU and GMU, and Karin Muglach, NASA/GSFC Jenna – HSD is heliophysics science division at GSFC, it’s the logo for me and Karin

When analyzing CMEs in real time for space weather forecasting, a lack of sufficient coronagraph images can make it difficult to determine the CME’s position (latitude and longitude). In these cases, usually the location of strong disk signatures (e. g., an associated flare, filament eruption, and coronal dimming) is used to estimate the CME’s propagation direction. Although not an unreasonable assumption, many observational and modeling studies have shown that CMEs can deflect by ten or more degrees from the source location – E. g. MacQueen et al. 1986, Filippov, Gopalswamy & Lozhechkin 2001; Gopalswamy et al. 2009, 2010, Kilpua et al. 2009, Xie et al. 2009, Byrne et al. 2010, Lugaz et al. 2011, Zuccarello et al. 2012, Kay, Opher, & Evans 2013, Liu et al Many of these previous works are single event studies Introduction and Motivation

Sources of CME deflection – Magnetic forces (coronal holes, heliospheric current sheet) – Ambient solar wind interactions – CME-CME interactions Usually it is assumed that deflection ends after low corona, but Liu et al. (2014) recently found deflection continued into the inner heliosphere Space weather forecasting impacts – CME ensemble modeling by the Space Weather Research Center at NASA/GSFC shows that variation of the CME’s position by ten degrees can change the arrival time at 1 AU by several hours. In this work we measure the deflection of many events, and will compare the deflection with the properties of nearby coronal holes

Event Selection Criteria CCMC’s Database of Notifications, Knowledge and Information (DONKI) – searched during Isolated event – not overlapping with another CME 2.Each event had to have a minimum of six images in two out of three SC (SOHO, STEREO A and B) 3.Pairs of images from different SC have ΔT<10 min 4.We want a range of CME widths and positions, so we did not restrict these parameters. Average CME speed in coronagraph FOV (binned by 100 km/s) Number of events Initial DONKI queries: 1.CMEs with speeds greater than 1,000 km/s 2.CMEs with Interplanetary Shock arrivals at Earth, STA or STB Later, expanded search to include C- type events and two events were included from Hess & Zhang, SPD 2014 C-type O-type R-type S-type

A web-based and public CME Analysis tool used to measure CMEs as they propagate away from the Sun – Measures half-width, latitude, longitude, speed, and arrival time at 21.5 solar radii – Frameseries mode: width is allowed to vary with time – Used in space weather forecasting models We assume that a change in the CME’s position is deflection – Not accounting for rotation or non-uniform expansion CCMC’s StereoCat Analysis Tool

DateTime Source Lon/Lat Average Speed Averag e Width 1 st Lon/Lat Final Lon/Lat Average Lon/Lat Deflection in Corona Total Deflection Year /08 5:00 -1, , -83, -60, /13 11: , 4043, 3945, /24 14:54 18, , -610, Year /14 0:00 22, , 226, 235, Year /0215:12100, , , , /1915:10-27, , , 46-35, /234:0020, , 22 0, 3713, /265:3078, , 65 70, 7269, /0411:24-65, , , 23-54, /13 14:00 -21, , , ,

DateTime Source Lon/Lat Average Speed Averag e Width 1 st Lon/Lat Final Lon/Lat Average Lon/Lat Deflection in Corona Total Deflection 06/1414:09-6, , -23 2, -23-3, /1216:542, , , -18-5, /1714:2588, , , -3055, /232:36136, , 1 124, -4128, /05 3: , -228, -1810, /09 15:24 -20, , -14-5, -11-7, Year /2312:39-175, , , , /2116:39125, , 9 112, 14111, /132:54-89, , 6 -73, 6-79, /179:24-36, , 9 -41, 14-44, /2213:24 75, , 562, 560, /13 4:09-172, , ,

DateTime Source Lon/Lat Average Speed Averag e Width 1 st Lon/Lat Final Lon/Lat Average Lon/Lat Deflection in Corona Total Deflection 07/22 6:24162, , , 27147, /17 19:2430, , , -1968, /07 10:39-153, , , , /084:24 Not Clear , , , /1910: , , , /2919:39 139, , , , /12 3:5440, , , -3855, /26 3:40-171, , , , Year /029:36 141, , , , /148: , -7132, -8123, /2212: , , , /2423: , , ,

DateTime Source Lon/Lat Average Speed Averag e Width 1 st Lon/Lat Final Lon/Lat Average Lon/Lat Deflection in Corona Total Deflection 02/251:25 -77, , , /04 19: , 82149, 82151, /059: , , , /1214: , , /069:48 140, , 27133, 32132, /07 21: , -3595, -3898, /08 11:12 135, , 45152, 41149, /090:00-156, , , , Summary of 42 events in data set – Range of speeds: 489 – 2,326 km/s – Average speed: 1,133 km/s – Range of widths: 21 – 81° – Average width: 48° Source location determined by: 1)Flare location (if known) 2)EUV signatures in 195 and 304 Å (if possible) 3)If no clear signature could be found, box contains “-”

Preliminary Results I 4 events with x>10 degrees; 13 event >20 degrees Lots of scatter – as to be expected Due to availability of overlapping images between the different spacecraft, the height of the first and last measurements varies between events. Total Deflection and Average CME Speed

Preliminary Results II 3D deflection exceeding >40 ° in 3 events Due to availability of overlapping images between the different spacecraft, the height of the first and last measurements varies between events. Deflection (in corona) and Average CME Width

Preliminary Results III Lots of scatter with changes in all 4 quadrants of the graph Due to availability of overlapping images between the different spacecraft, the height of the first and last measurements varies between events. Change in Latitude and Change in Longitude Using the CME Source Location as Initial Value

Preliminary Results IV Scattering due to the difference between the source and final (measured) latitude Due to availability of overlapping images between the different spacecraft, the height of the first and last measurements varies between events. Source Latitude and Change in Latitude

Preliminary Results V Lots of scatter due to selection of locations of CMEs Scatter also due to difference between source and final (measured) longitude Due to availability of overlapping images between the different spacecraft, the height of the first and last measurements varies between events. Source Longitude and Change in Longitude

Preliminary Results VI CME follows expected path due to presence of coronal holes Total deflection is 22.7 °, just in the corona 12° Tracking One Event from the Sun to 15 Rs Source location CME measurements Coronal holes Mid and low latitude coronal holes within 90° in longitude of source locations were indentified by eye (not yet cross checked with magnetogram data or filament catalogs) Synoptic EUV map constructed from SDO, STA and STB EUVI

Discussions, Conclusions, and Future Work We analyzed 42 CMEs from and found deflections range from less than 5 degrees to greater than 20 degrees from the source location to the edge of COR2 field of view For one event, we identified nearby coronal holes. The measured path of the CME matches expected behavior Limitations of our approach: – StereoCat is a simple tool that does consider the geometry of CME – Next step is to use other CME analysis tools (such as SWPC_CAT and GCS) In progress: – Rigorous identification of coronal holes and the Coronal Hole Influence Parameter (Gopalswamy et al. 2009, 2010) Use the results of this study to select appropriate ranges of latitudes and longitudes in CME ensemble modeling based on CME speed, width, location How to incorporate coronal hole observations more systematically in real time CME analysis for space weather forecasting? J. Zink would like to thank the NSF for travel support to attend this meeting through the CCMC Student Research Contest. J. Zink was supported by the GMU USRP. R. Evans was supported through an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA.