cass/ucsd - jeju 2015 a jets in the heliosphere: a solar wind component b.v. jackson, h.-s. yu, p.p....
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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
Masayoshihttp://smei.ucsd.edu/ http://ips.ucsd.edu/
Jets in the Heliosphere: An Indicator of a Fast Solar Wind Component
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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:
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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
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CASS/UCSD - Jeju 2015
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)
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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
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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
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CASS/UCSD - Jeju 2015
A Jets in the Heliosphere: A Solar Wind Component
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)
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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
5x1014g
SW 14 Poster S1-2 (Yu et al., 2015)
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CASS/UCSD - Jeju 2015
A Jets in the Heliosphere: A Solar Wind Component
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.
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CASS/UCSD - Jeju 2015
A Jets in the Heliosphere: A Solar Wind Component
This Study Gets Even More Interesting
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CASS/UCSD - Jeju 2015
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)
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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 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.
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CASS/UCSD - Jeju 2015
A Jets in the Heliosphere: A Solar Wind Component
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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 C2
2007 Sep 1017:37:30 – 17:07:30
poor correlations
Jackson, et al., 2014, Astrophys. J., 793, 54.
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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.
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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.
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CASS/UCSD - Jeju 2015
A Jets in the Heliosphere: A Solar Wind ComponentJackson, et al., 2014, Astrophys. J., 793, 54.
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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 BrightnessJackson, et al., 2014, Astrophys. J., 793, 54.
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CASS/UCSD - Jeju 2015
A Jets in the Heliosphere: A Solar Wind Component
Average speed with solar distance.
2007 Sept. 10C2/COR2-AJackson, et al., 2014, Astrophys. J., 793, 54.
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CASS/UCSD - Jeju 2015
A Jets in the Heliosphere: A Solar Wind Component
Average speed with solar distance.
2007 Sept. 14C2/COR2-AJackson, et al., 2014, Astrophys. J., 793, 54.
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CASS/UCSD - Jeju 2015
A Jets in the Heliosphere: A Solar Wind Component
C2/COR2-AAverage solar wind speed with solar distance PA: -60° -- +60°
2007 Sept. 10
Jackson, et al., 2014, Astrophys. J., 793, 54.
Munro & Jackson, 1977, ApJ, 213, 874 – Skylab data in 1973Kohl et al., 1998, ApJL, 501, L127 – SOHO/UVCS
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CASS/UCSD - Jeju 2015
A Jets in the Heliosphere: A Solar Wind Component
Average solar wind speed with solar distance PA: -60° -- +60°
Jackson, et al., 2014, Astrophys. J., 793, 54.
C2/COR2-A 2007 Sept. 14
Munro & Jackson, 1977, ApJ, 213, 874 – Skylab data in 1973Kohl et al., 1998, ApJL, 501, L127 – SOHO/UVCS
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CASS/UCSD - Jeju 2015
A Jets in the Heliosphere: A Solar Wind Component
So What Does This Mean?
(A Summary)
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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
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CASS/UCSD - Jeju 2015
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.
Dis
tan
ce F
rom
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un
Dis
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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.