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CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere B.V. Jackson Center for Astrophysics and Space Sciences, University of California at San Diego, La Jolla,

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Presentation on theme: "CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere B.V. Jackson Center for Astrophysics and Space Sciences, University of California at San Diego, La Jolla,"— Presentation transcript:

1 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere B.V. Jackson Center for Astrophysics and Space Sciences, University of California at San Diego, La Jolla, CA, USA Masayoshi http://smei.ucsd.edu/ http://ips.ucsd.edu/ The 3D Analysis of the Heliosphere Using Interplanetary Scintillation and Thomson-Scattering Observations With inputs from: Andrew Buffington, P. Paul Hick, John Clover, Mario Bisi, Tamsen Dunn Masayoshi Kojima, Munetoshi Tokumaru, Ken’ichi Fujiki, Maria Hirota Masumi Shimojo, Nobuharu Sako, Sako Tsuneta, Kazunari Shibata Katsuhide Marubashi, Kevin Schenk, Joe Gurman, P.K. Manoharan Igor Chasey, Americo Gonzalez, Julio Mejia Craig DeForest, Tim Howard Nikolai Pogorelov, Gary Zank Chris Eyles, Dave Webb

2 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere The Big Question: How does the Sun do it? Motivation: To figure it out. The Data: Spacecraft, ground-based input – Hinode, SDO, SOHO LASCO, STEREO, SMEI, IBEX, Ground-based magnetograms, Ground-based IPS The Analysis: To make 2D images into 3D measurements over time. Conclusions: Are we there yet? Introduction:

3 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere Hinode XRT observations Shimojo and Tsuneta, ApJ, 706, L145, 2009 Munro and Jackson, ApJ, 213, 877, 1977 What energizes the solar wind to expel it? Do coronal jets somehow play a major role?

4 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere NASA spacecraft imagers STEREO-A COR2STEREO-B COR2 SDO AIA 7 June 2011 CMEs LASCO C3

5 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere NASA spacecraft imagers STEREO-A COR2STEREO-B COR2 SDO AIA 7 June 2011 CMEs LASCO C3 What powers CMEs?

6 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere NASA spacecraft imagers Integrated video from STEREO-A imagers ( Courtesy of Craig DeForest, Tim Howard, SWRI, Boulder, CO) HI-2 HI-1 COR2 Howard & DeForest, ApJ, 2011 (submitted)

7 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere SMEI (The Solar Mass Ejection Imager) SMEI_2003 (A precision photometer that can view the whole sky from Earth) Jackson, B.V., et al., 2004, Solar Phys., 225, 177

8 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere SMEI (The Solar Mass Ejection Imager) SMEI_2003 (A precision photometer that can view the whole sky from Earth) CME on 31 May 2003

9 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere World-Wide IPS observation network Japan Mexico India Russia UK/EISCAT US-Australia Ooty 327MHz 、 16,000 ㎡ Pushchino103MHz 20,000 ㎡ MEXART 140MHz 、 10,000 ㎡ MWA 80-300MHz STEL Multi-Station 327MHz 2000 ㎡ ×3, 3500 ㎡ IPS

10 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere Let’s start with what we observe in IPS STELab IPS array near Mt. Fuji DATA STELab IPS array systemsIPS line-of-sight response How do we obtain a 3D depiction from these data?

11 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere Heliospheric C.A.T. analyses: example line-of-sight distribution for each sky location to form the source surface of the 3D reconstruction. STELab IPS IPS line-of-sight response Jackson, B.V., et al., 2008, Adv. in Geosciences 21, 339

12 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere 13 July 200014 July 2000 Heliospheric C.A.T. Analyses: example line-of-sight distribution for each sky location to form the source surface of the 3D reconstruction. STELab IPS IPS line-of-sight response Jackson, B.V., et al., 2008, Adv. in Geosciences 21, 339

13 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere All-Sky g-maps 2008/11/04 Toyokawa Kiso

14 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere IPS C.A.T. analysis “Bastille Day” event 14 July 2000 Jackson, B.V., et al., 2002, Solar Wind 10, 31Jackson, B.V., et al., 2008, Adv. in Geosciences 21, 339

15 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere Heliospheric C.A.T. Analyses: example line-of-sight distribution for each sky location to form the source surface of the 3D reconstruction. Thomson scattering IPS line-of-sight response Jackson, B.V., et al., 2008, Adv. in Geosciences 21, 339 LOS Weighting 30º 60º 90º

16 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere Brightness fall-off with distance Jackson, B.V., et al., 2004, Solar Phys., 225, 177

17 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere B. V. Jackson, A. Buffington, P. P. Hick Center for Astrophysics and Space Sciences, University of California at San Diego, LaJolla, CA. R.C. Altrock, S. Figueroa, P.E. Holladay, J.C. Johnston, S.W. Kahler, J.B. Mozer, S. Price, R.R. Radick, R. Sagalyn, D. Sinclair Air Force Research Laboratory/Space Vehicles Directorate (AFRL/VS), Hanscom AFB, MA G.M. Simnett, C.J. Eyles, M.P. Cooke, S.J. Tappin School of Physics and Space Research, University of Birmingham, UK T. Kuchar, D. Mizuno, D.F.Webb ISR, Boston College, Newton Center, MA P.A. Anderson Boston University, Boston, MA S.L. Keil National Solar Observatory, Sunspot, NM R.E. Gold Johns Hopkins University/Applied Physics Laboratory, Laurel, MD N.R. Waltham Space Science Dept., Rutherford-Appleton Laboratory, Chilton, UK The Solar Mass Ejection Imager (SMEI) Mission -- Journal Article The Coriolis spacecraft at Vandenberg prior to flight. The SMEI baffles are circled. The large NRL radiometer Windsat is on the top of the spacecraft. Jackson, B.V., et al., 2004, Solar Phys., 225, 177

18 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere Simultaneous images from the three SMEI cameras. The Solar Mass Ejection Imager (SMEI) C1 C2 C3 Sun Jackson, B.V., et al., 2004, Solar Phys., 225, 177 Launch 6 January 2003 1 gigabyte/day; now ~4 terabytes A joint US Air Force - NASA Project

19 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere Frame composite for Aitoff map Blue = Cam3; Green = Cam2; Red = Cam1 D290; 17 October 2003 Jackson, B.V., et al., 2008, J. Geophys Res., 113, A00A15, doi:10.1029/2008JA013224

20 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere Heliospheric direct images (differenced) SMEI difference images Jackson, B.V., et al., 2008, J. Geophys Res., 113, A00A15, doi:10.1029/2008JA013224

21 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere 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. Jackson, B.V., et al., 2008, J. Geophys Res., 113, A00A15, doi:10.1029/2008JA013224

22 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere SMEI brightness with a long-term (~30 day) base removed. (1 S10 = 0.46 ± 0.02 ADU) 27-28 May 2003 CME events brightness time series for select sky sidereal locations SMEI data Jackson, B.V., et al., 2008, J. Geophys Res., 113, A00A15, doi:10.1029/2008JA013224

23 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere Heliospheric 3D reconstruction Line of sight “crossed” components on a reference surface. Projections on the reference surface are shown. These weighted components are inverted to provide the time-dependent tomographic reconstruction. Jackson, B.V., et al., 2008, Adv. in Geosciences 21, 339 >10,000 lines of sight /orbit >5,000,000 /month!

24 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere SMEI density (remote observer view) of the 27-28 May 2003 halo CMEs 2003 May 27-28 CME events Jackson, B.V., et al., 2008, J. Geophys Res., 113, A00A15, doi:10.1029/2008JA013224 SMEI density 3D reconstruction of the 27-28 May 2003 halo  CMEs as viewed from 30º above the ecliptic plane about 30º west of the Sun-Earth line. LASCO C3 Do CMEs move outward from the Sun to 1 AU?

25 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere SMEI proton density reconstruction for the 27-28 May 2003 halo CME sequence. Reconstructed and Wind in-situ densities are compared over one Carrington rotation. 27-28 May 2003 CME event period Jackson, B.V., et al., 2008, J. Geophys Res., 113, A00A15, doi:10.1029/2008JA013224 12-hour cadence, 7º x 7º lat, long If so, what is their mass and interplanetary consequences?

26 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere SMEI proton density reconstruction for the 27-28 May 2003 halo CME sequence. Reconstructed and Wind in-situ densities are compared over one Carrington rotation. 27-28 May 2003 CME event period Jackson, B.V., et al., 2008, J. Geophys Res., 113, A00A15, doi:10.1029/2008JA013224 12-hour cadence, 7º x 7º lat, long Associated IPS 3D velocity

27 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere SMEI proton density reconstruction for the 27-28 May 2003 halo CME sequence. Reconstructed and ACE L2 in-situ densities are compared over one Carrington rotation. 27-28 May 2003 CME event period Jackson, B.V., et al., 2008, J. Geophys Res., 113, A00A15, doi:10.1029/2008JA013224 Full SMEI data set, 6-hour cadence, 3º x 3º lat, long

28 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere 2003 May 27-28 CME events CME mass Jackson, B.V., et al., 2008, J. Geophys Res., 113, A00A15, doi:10.1029/2008JA013224

29 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere Often ICMEs contain magnetic flux ropes near their onset in the IM 2010 January 14 ICME flux rope (STEREO-B) What is the mechanism that powers CMEs? Marubashi flux rope cylinder fitMarubashi flux rope toroidal fit

30 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere 2010 January CME events SMEI analysis Brightness differenceDensity ecliptic cut 12-hour cadence, 7º x 7º lat, long

31 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere 2010 January CME events SMEI analysis Brightness differenceDensity ecliptic cut 12-hour cadence, 7º x 7º lat, long

32 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere 2010 January CME events SMEI, STEREO-B in-situ analysis 12-hour cadence, 7º x 7º lat, long

33 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere 2010 January CME events SMEI LASCO C3 coronagraph simulation Late 14 January CME17 January CME 12-hour cadence, 7º x 7º lat, long Fall 2011 AGU special session: “How do heliospheric remote- sensing observations limit magnetic flux rope models?”

34 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere SPD Meeting, 16 June 2011 5 Ooty IPS 3D reconstruction (10 September 2005) Is there other 3D evidence of loop-like heliospheric structure? Manoharan, P.K., 2010, Solar Phys., 265, 137

35 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere SPD Meeting, 16 June 2011 5 Ooty IPS 3D reconstruction (10 September 2005) Manoharan, P.K., 2010, Solar Phys., 265, 137 AOGS special special session ST14 Thursday 4:00-6:00 pm (Be sure to come!)

36 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere Skymap view Web analysis runs automatically using Linux on a P.C. http://ips.ucsd.edu/ UCSD IPS forecast So, you think we’re good at research? How about trying to forecast heliospheric structure arrival at Earth?

37 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere Remote observer viewhttp://ips.ucsd.edu/ UCSD IPS forecast Web analysis runs automatically using Linux on a P.C. CASS/UCSD AOGS 2011

38 3D Analysis of the Heliosphere Velocity and density Web analysis runs automatically using Linux on a P.C. http://ips.ucsd.edu/ UCSD IPS forecast Typhoon! Lightening!

39 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere Jets in Hinode XRT observations 3D IPS reconstruction program at the CCMC LASCO C2 observations But what about the jets? We haven’t answered their role.

40 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere SMEI pseudo coronagraph observations in 3D 07:14:48 07:18:48 07:22:48 07:26:48 Hinode jet(2007-SEP-14) One jet of hundreds! jet (Sako, M., et al., 2010, 38 th COSPAR Scientific Assembly, E21-0018-10)

41 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere SMEI pseudo coronagraph observations in 3D 07:14:48 07:18:48 07:22:48 07:26:48 Hinode jet(2007-SEP-14) jet Jet energy analysis portion of 2007-SEP-14 jet (Sako, M., et al., 2010, 38 th COSPAR Scientific Assembly, E21-0018-10) jet (Sako, M., et al., 2010, 38 th COSPAR Scientific Assembly, E21-0018-10) jet

42 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere 07:14:48 07:18:48 07:22:48 07:26:48 Hinode jet(2007-SEP-14) jet Jet energy analysis portion of 2007-SEP-14 SMEI pseudo coronagraph observations in 3D (Sako, M., et al., 2010, 38 th COSPAR Scientific Assembly, E21-0018-10) jet

43 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere Jets (polar plumes) can be observed moving outward in the solar polar regions often at speeds >3 times ambient LASCO C2 north polar hole example (left, north) shows outward motion of plume onset >2.0 Rs in 37 min. This implies an outward plane-of-the-sky speed of ~600 km s -1.

44 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere Jets (polar plumes) can be observed moving outward in the solar polar regions often at speeds >3 times ambient LASCO C2 north polar hole example (left) shows outward motion of plume onset >2.0 Rs in 37 min. This implies an outward plane-of-the-sky speed of ~600 km s -1. Why doesn’t Ulysses see them?

45 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere Hinode Observing Proposal (HOP 187) 17 June 2011 00:00 - 06:00 UT 07 August 2011 00:00 - 08:00 UT (canceled) Rerun (TBD) (Hinode XRT, EIS, SDO, LASCO C2, STEREO, IPS, SMEI) “Jets from the solar surface to interplanetary space” Current participants: B.V. Jackson, M. Shimojo, N. Sako, D. Brooks, A. Sterling, M.Tokumaru, P.K. Manoharan, K. Schenk, R. Howard, J. Gurman, P. Liewer, K. Shibata, W. Pesnell, Nikolai Pogorelov

46 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere 46 The heliopause colored by the total pressure, ISMF lines draping the HP, and the surface B·R=0 in the MHD-kinetic simulation from Pogorelov et al. (2009). The ISMF is from λ ≈ 236º and b ≈ 30º. The direction =224  and b=41  fits the IBEX observations better. In both cases, the BV-plane is parallel to the HDP. Heliopause simulation (Pogorelov, N, et al., 2009, Adv. in Space Res., 44, 1337)

47 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere IBEX ENA Flux The ribbon is highly sensitive to variations in the ISMF direction! 47 Simulation (4.5 kev) ENA Image Heliopause simulation (Pogorelov, N, et al., 2009, Adv. in Space Res., 44, 1337)

48 CASS/UCSD AOGS 2011 3D Analysis of the Heliosphere The 3D heliosphere: We can reconstruct it globally in fundamental parameters, velocity and density. CMEs, co-rotating structures, shock sheaths, the largest jets? We can forecast its arrival at Earth. We’ve learned many things: The extent, shape, 3D mass of CMEs. The relationship of density and velocity to the in-situ manifestation of these structures. We are getting better! Are we there yet? (Have we answered the most fundamental questions?) Summary:

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