CASS/UCSD - Jeju 2015 A Jets in the Heliosphere: A Solar Wind Component B.V. Jackson, H.-S. Yu, P.P. Hick, and A. Buffington, Center for Astrophysics and.

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CASS/UCSD - Jeju 2015 A Jets in the Heliosphere: A Solar Wind Component B.V. Jackson, H.-S. Yu, P.P. Hick, and A. Buffington, Center for Astrophysics and Space Sciences, University of California at San Diego, LaJolla, CA, USA Masayoshi Jets in the Heliosphere: An Indicator of a Fast Solar Wind Component

CASS/UCSD - Jeju 2015 A Jets in the Heliosphere: A Solar Wind Component Solar Jets : Outflow evidence for a high-speed (and faster than ambient) solar wind structure component. Coronagraph images: Optical flow techniques used to measure coronagraph speeds. Characteristics of the dynamic flow: High speed patches, vs. brightness, C2 – COR2 comparisons. Averages with position angle and height. The mean value is the true solar wind speed. Speculation on what this means. Jets a tracer of a more ubiquitous solar wind process. Introduction:

CASS/UCSD - Jeju 2015 A Jets in the Heliosphere: A Solar Wind Component 2011 June 17 SDO/AIA Jet LASCO C2 Coronal Flow LASCO C2 03:30UT Jet SW 14 Poster S1-2 (Yu et al., 2015) SDO AIA ~02:50 UT

CASS/UCSD - Jeju 2015 A Jets in the Heliosphere: A Solar Wind Component Positions of STEREO A and B for :40UT SW 14 Poster S1-2 (Yu et al., 2015)

CASS/UCSD - Jeju 2015 A Jets in the Heliosphere: A Solar Wind Component STEREO COR 2A Coronal Flow COR 2A 03:39UT Jet SW 14 Poster S1-2 (Yu et al., 2015) SDO AIA ~02:50 UT

CASS/UCSD - Jeju 2015 A Jets in the Heliosphere: A Solar Wind Component Height-time plot -- Jet response on the sky plane (Yu et al., 2013, Solar Wind 13) Height-time plot -- Jet response from Sun center Sun center

CASS/UCSD - Jeju 2015 A Jets in the Heliosphere: A Solar Wind Component 2011/06/17 SDO/HMI LOS Magnetograms SW 14 Poster S1-2 (Yu et al., 2015) Opposite polarity magnetic field emergence max (black) Brightness of the area within the box (AIA red)

CASS/UCSD - Jeju 2015 A Jets in the Heliosphere: A Solar Wind Component Jet Response in SMEI 3D density Reconstruction Jet Response in IPS 3D speed Reconstruction 5x10 14 g SW 14 Poster S1-2 (Yu et al., 2015)

CASS/UCSD - Jeju 2015 A Jets in the Heliosphere: A Solar Wind Component Study of jet responses in Hinode from Sept data (Yu et al., 2013, Astrophys. J., 784, 166.) Sako et al., 2013, Astrophys. J, 775, 22. If the amount of mass in a jet response is related to the jet fall-off in brightness with number, then jets provide ~2.5% of the total mass of the solar wind.

CASS/UCSD - Jeju 2015 A Jets in the Heliosphere: A Solar Wind Component This Study Gets Even More Interesting

CASS/UCSD - Jeju 2015 A Jets in the Heliosphere: A Solar Wind Component Jet analysis: 07:14:48 07:14:48 07:18:48 07:22:48 (from Shimojo and Tsuneta, 2009)

CASS/UCSD - Jeju 2015 A Jets in the Heliosphere: A Solar Wind Component What do jets tell us about solar wind? 2D Cross Correlation of LASCO C2 Optical Coronal Flow Jet Response > 400km/s Jet 2007 SEP 14 08:30:04 – 08:06:04 Yu, H.-S., et al., 2013, Solar Wind 13. Jackson, B.V. et al., 2013, Solar Wind 13. Yu, H.-S., et al., 2014, Ap. J., 784, 166. Jackson, et al., 2014, Ap. J., 793, 54.

CASS/UCSD - Jeju 2015 A Jets in the Heliosphere: A Solar Wind Component

CASS/UCSD - Jeju 2015 A Jets in the Heliosphere: A Solar Wind Component COR2-A  High speed solar wind component. (~1.5 Rs x ~3º) (Correlations limited to >0.5) LASCO C Sep 10 17:37:30 – 17:07:30 poor correlations Jackson, et al., 2014, Astrophys. J., 793, 54.

CASS/UCSD - Jeju 2015 A Jets in the Heliosphere: A Solar Wind Component Comparison of Speed Structure C2 – COR2A Overlap Region Jackson, et al., 2014, Astrophys. J., 793, 54.

CASS/UCSD - Jeju 2015 A Jets in the Heliosphere: A Solar Wind Component Comparison of Speed Structure C2 – COR2A Overlap Region Jackson, et al., 2014, Astrophys. J., 793, 54.

CASS/UCSD - Jeju 2015 A Jets in the Heliosphere: A Solar Wind Component Jackson, et al., 2014, Astrophys. J., 793, 54.

CASS/UCSD - Jeju 2015 A Jets in the Heliosphere: A Solar Wind Component High-speed patches – slightly brighter in general Comparison of Speed Structure and Brightness Jackson, et al., 2014, Astrophys. J., 793, 54.

CASS/UCSD - Jeju 2015 A Jets in the Heliosphere: A Solar Wind Component Average speed with solar distance Sept. 10 C2/COR2-A Jackson, et al., 2014, Astrophys. J., 793, 54.

CASS/UCSD - Jeju 2015 A Jets in the Heliosphere: A Solar Wind Component Average speed with solar distance Sept Sept. 14C2/COR2-A Jackson, et al., 2014, Astrophys. J., 793, 54.

CASS/UCSD - Jeju 2015 A Jets in the Heliosphere: A Solar Wind Component C2/COR2-A Average solar wind speed with solar distance PA: -60° ° 2007 Sept. 10 Jackson, et al., 2014, Astrophys. J., 793, 54. Munro & Jackson, 1977, ApJ, 213, 874 – Skylab data in 1973 Kohl et al., 1998, ApJL, 501, L127 – SOHO/UVCS

CASS/UCSD - Jeju 2015 A Jets in the Heliosphere: A Solar Wind Component Average solar wind speed with solar distance PA: -60° ° Jackson, et al., 2014, Astrophys. J., 793, 54. C2/COR2-A 2007 Sept. 14 Munro & Jackson, 1977, ApJ, 213, 874 – Skylab data in 1973 Kohl et al., 1998, ApJL, 501, L127 – SOHO/UVCS

CASS/UCSD - Jeju 2015 A Jets in the Heliosphere: A Solar Wind Component So What Does This Mean? (A Summary)

CASS/UCSD - Jeju 2015 A Jets in the Heliosphere: A Solar Wind Component 2011 June 17 SDO/AIA Jet LASCO C2 Coronal Flow LASCO C2 03:30UT Jet SW 14 Poster S1-2 (Yu et al., 2015) SDO AIA ~02:50 UT

CASS/UCSD - Jeju 2015 A Jets in the Heliosphere: A Solar Wind Component Speed summary plots 2D-correlation Speed summary plots obtained from 2D-correlation of the same high speed jet-associated response (at 2011 June 17 02:50 UT by the SDO/AIA) in both LASCO C2 and STEREO COR2 observations 90° in longitude from each other. material flow This sequence of bright high-speed patches can be directly tracked as brightness enhancements of about the same speed and size, and thus are a good indication that these measurements are of material flow in the corona. Distance From Sun

CASS/UCSD - Jeju 2015 A Jets in the Heliosphere: A Solar Wind Component Probably what we are seeing is evidence of an energy deposition at height that moves some small portions of the corona outward at high speeds and is associated with the emergence of oppositely directed flux from what is normal at that region on the solar surface. Jets illuminate this process, but are probably only a tracer of the effect taking place, since they are not numerous or massive enough to provide the total outward-flowing solar wind. That both the high and low speed structure fills the polar regions of the Sun and can be shown to average to the increasing solar wind speed in the large polar regions, probably means that this is evidence of the major source of solar wind acceleration in the corona.