cass/ucsd aogs 2011 3d analysis of the heliosphere b.v. jackson center for astrophysics and space...

CASS/UCSD AOGS 2011

3D Analysis of the Heliosphere

B.V. JacksonCenter for Astrophysics and Space Sciences, University of California at San Diego, La Jolla, CA, USA

Masayoshihttp://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 DunnMasayoshi Kojima, Munetoshi Tokumaru, Ken’ichi Fujiki, Maria HirotaMasumi 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 HowardNikolai Pogorelov, Gary ZankChris Eyles, Dave Webb

CASS/UCSD AOGS 2011


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:

CASS/UCSD AOGS 2011


Hinode XRT observations

Shimojo and Tsuneta, ApJ, 706, L145, 2009Munro and Jackson, ApJ, 213, 877, 1977

What energizes the solar wind to expel it? Do coronal jets somehow play a major role?

CASS/UCSD AOGS 2011


NASA spacecraft

imagers

STEREO-A COR2 STEREO-B COR2

SDO AIA

7 June 2011

CMEs

LASCO C3

CASS/UCSD AOGS 2011


NASA spacecraft

imagers

STEREO-A COR2 STEREO-B COR2

SDO AIA

7 June 2011

CMEs

LASCO C3

What powers CMEs?

CASS/UCSD AOGS 2011


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)

CASS/UCSD AOGS 2011


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

CASS/UCSD AOGS 2011


SMEI (The Solar Mass Ejection Imager)

SMEI_2003

(A precision photometer that can view the whole sky from Earth)

CME on 31 May 2003

CASS/UCSD AOGS 2011


World-Wide IPS observation network

JapanMexico

India

RussiaUK/EISCAT

US-Australia

Ooty 327MHz 、 16,000㎡

Pushchino103MHz20,000 ㎡

MEXART140MHz 、 10,000㎡

MWA80-300MHz

STEL Multi-Station 327MHz2000 ㎡ ×3, 3500 ㎡

IPS

CASS/UCSD AOGS 2011


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?

CASS/UCSD AOGS 2011


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

CASS/UCSD AOGS 2011


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


CASS/UCSD AOGS 2011


All-Sky g-maps 2008/11/04

Toyokawa Kiso

CASS/UCSD AOGS 2011


IPS C.A.T. analysis“Bastille Day” event

14 July 2000

Jackson, B.V., et al., 2002, Solar Wind 10, 31 Jackson, B.V., et al., 2008, Adv. in Geosciences 21, 339

CASS/UCSD AOGS 2011


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


LOS Weighting

30º

60º

90º

CASS/UCSD AOGS 2011


Brightness fall-off with distanceJackson, B.V., et al., 2004, Solar Phys., 225, 177

CASS/UCSD AOGS 2011


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. TappinSchool of Physics and Space Research, University of Birmingham, UK

T. Kuchar, D. Mizuno, D.F.WebbISR, Boston College, Newton Center, MA

P.A. AndersonBoston University, Boston, MA

S.L. KeilNational Solar Observatory, Sunspot, NM

R.E. GoldJohns Hopkins University/Applied Physics Laboratory, Laurel, MD

N.R. WalthamSpace 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.


CASS/UCSD AOGS 2011


Simultaneous images from the three SMEI cameras.

The Solar Mass Ejection Imager

(SMEI)C1

C2

C3

Sun

Sun


Launch 6 January 2003

1 gigabyte/day; now ~4 terabytes

A joint US Air Force - NASA Project

CASS/UCSD AOGS 2011


Frame composite for Aitoff mapBlue = Cam3; Green = Cam2; Red = Cam1

D290; 17 October 2003

Jackson, B.V., et al., 2008, J. Geophys Res., 113, A00A15, doi:10.1029/2008JA013224

CASS/UCSD AOGS 2011


Heliospheric direct images (differenced)

SMEI difference images


CASS/UCSD AOGS 2011


0 50 100 150 200 250 3000

50

100

150

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- 4 . 5

- 4

- 3 . 5

- 3

- 2 . 5

- 2

- 1 . 5

- 1

- 0 . 5

0

0 . 5

1

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2

2 . 5

3

3 . 5

4

4 . 5

5

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.

0 50 100 150 200 250 3000

50

100

150

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- 4 . 5

- 4

- 3 . 5

- 3

- 2 . 5

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CASS/UCSD AOGS 2011


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 seriesfor select sky sidereal locations

SMEI data


CASS/UCSD AOGS 2011


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!

CASS/UCSD AOGS 2011


SMEI density (remote observer view) of the 27-28 May 2003 halo CMEs

2003 May 27-28 CME eventsJackson, 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?

CASS/UCSD AOGS 2011


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


12-hour cadence, 7º x 7º lat, long

If so, what is their mass and interplanetary consequences?

CASS/UCSD AOGS 2011


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.




Associated IPS 3D velocity

CASS/UCSD AOGS 2011


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.



Full SMEI data set, 6-hour cadence, 3º x 3º lat, long

CASS/UCSD AOGS 2011


2003 May 27-28 CME events

CME mass


CASS/UCSD AOGS 2011


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

CASS/UCSD AOGS 2011


2010 January CME events

SMEI analysis

Brightness difference Density ecliptic cut12-hour cadence, 7º x 7º lat, long

CASS/UCSD AOGS 2011



SMEI, STEREO-B in-situ analysis


CASS/UCSD AOGS 2011



SMEI LASCO C3 coronagraph simulation

Late 14 January CME 17 January CME12-hour cadence, 7º x 7º lat, long

Fall 2011 AGU special session: “How do heliospheric remote-sensing observations limit magnetic flux rope models?”

CASS/UCSD AOGS 2011


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

CASS/UCSD AOGS 2011


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!)

CASS/UCSD AOGS 2011

3D Analysis of the HeliosphereSkymap 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?

CASS/UCSD AOGS 2011

3D Analysis of the HeliosphereRemote observer viewhttp://ips.ucsd.edu/

UCSD IPS forecast

Web analysis runs automatically using Linux on a P.C. CASS/UCSD AOGS 2011

CASS/UCSD AOGS 2011

3D Analysis of the HeliosphereVelocity and density

Web analysis runs automatically using Linux on a P.C.

http://ips.ucsd.edu/

UCSD IPS forecast

Typhoon!Lightening!

CASS/UCSD AOGS 2011


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.

CASS/UCSD AOGS 2011

3D Analysis of the HeliosphereSMEI 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

jet(Sako, M., et al., 2010, 38th COSPAR Scientific Assembly, E21-0018-10)

CASS/UCSD AOGS 2011

3D Analysis of the HeliosphereSMEI pseudo coronagraph

observations in 3D

07:14:48 07:18:48 07:22:48 07:26:48


jet

jet

Jet energy analysisportion of 2007-SEP-14



jet

CASS/UCSD AOGS 2011


07:14:48 07:18:48 07:22:48 07:26:48


jet

jet

Jet energy analysisportion of 2007-SEP-14

SMEI pseudo coronagraph observations in 3D

(Sako, M., et al., 2010, 38th COSPAR Scientific Assembly, E21-0018-10)

jet

CASS/UCSD AOGS 2011


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.

CASS/UCSD AOGS 2011


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?

CASS/UCSD AOGS 2011


Hinode Observing Proposal (HOP 187)

17 June 2011 00:00 - 06:00 UT07 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

CASS/UCSD AOGS 2011


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)

CASS/UCSD AOGS 2011


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)

CASS/UCSD AOGS 2011


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:

cass/ucsd aogs 2011 3d analysis of the heliosphere b.v. jackson center for astrophysics and space...

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