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

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

Masayoshihttp://smei.ucsd.edu/ http://ips.ucsd.edu/

Jets in the Heliosphere: An Indicator of a Fast 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:



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


A Jets in the Heliosphere: A Solar Wind ComponentPositions of STEREO A and B for 2011-06-17 02:40UT SW 14 Poster S1-2 (Yu et al., 2015)



STEREO COR 2A Coronal Flow

COR 2A 03:39UT

Jet


SDO AIA ~02:50 UT



Height-time plot --Jet response on the sky plane (Yu et al., 2013, Solar Wind 13)

Height-time plot --Jet response from Sun center



2011/06/17 SDO/HMI LOS MagnetogramsSW 14 Poster S1-2 (Yu et al., 2015)

Opposite polarity magnetic field emergence max (black)Brightness of the area within the box (AIA 304 - red)



Jet Response in SMEI 3D density Reconstruction

Jet Response in IPS 3D speed

Reconstruction

5x1014g




Study of jet responses in Hinode from Sept. 2007 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.



This Study Gets Even More Interesting


A Jets in the Heliosphere: A Solar Wind ComponentJet analysis:

07:14:48

07:14:48 07:18:48 07:22:48 (from Shimojo and Tsuneta, 2009)



What do jets tell us about solar wind?2D Cross Correlation of LASCO

C2 Optical Coronal Flow

Jet Response > 400km/s

Jet

2007 SEP 1408:30:04 – 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.





COR2-A

High speed solar wind component.

(~1.5 Rs x ~3º)(Correlations limited to >0.5) LASCO C2

2007 Sep 1017:37:30 – 17:07:30

poor correlations

Jackson, et al., 2014, Astrophys. J., 793, 54.



Comparison of Speed Structure C2 – COR2A

Overlap Region




Comparison of Speed Structure C2 – COR2A

Overlap Region



A Jets in the Heliosphere: A Solar Wind ComponentJackson, et al., 2014, Astrophys. J., 793, 54.



High-speed patches – slightly brighter in general

Comparison of Speed Structure and BrightnessJackson, et al., 2014, Astrophys. J., 793, 54.



Average speed with solar distance.

2007 Sept. 10C2/COR2-AJackson, et al., 2014, Astrophys. J., 793, 54.



Average speed with solar distance.

2007 Sept. 14C2/COR2-AJackson, et al., 2014, Astrophys. J., 793, 54.



C2/COR2-AAverage solar wind speed with solar distance PA: -60° -- +60°

2007 Sept. 10


Munro & Jackson, 1977, ApJ, 213, 874 – Skylab data in 1973Kohl et al., 1998, ApJL, 501, L127 – SOHO/UVCS



Average solar wind speed with solar distance PA: -60° -- +60°


C2/COR2-A 2007 Sept. 14

Munro & Jackson, 1977, ApJ, 213, 874 – Skylab data in 1973Kohl et al., 1998, ApJL, 501, L127 – SOHO/UVCS



So What Does This Mean?

(A Summary)



2011 June 17 SDO/AIA Jet LASCO C2 Coronal Flow

LASCO C2 03:30UT

Jet


SDO AIA ~02:50 UT


A Jets in the Heliosphere: A Solar Wind ComponentSpeed 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.

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.

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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.

Documents

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