B.V. Jackson,
This presentation is the property of its rightful owner.
Sponsored Links
1 / 36

B.V. Jackson, and P.P. Hick, A. Buffington, J.M. Clover, N. Amirbekian PowerPoint PPT Presentation


  • 58 Views
  • Uploaded on
  • Presentation posted in: General

B.V. Jackson, and P.P. Hick, A. Buffington, J.M. Clover, N. Amirbekian Center for Astrophysics and Space Sciences, University of California at San Diego, LaJolla, CA, USA. and. D.B. Reisenfeld Department of Physics and Astronomy, University of Montana, Missoula, MT, USA. Masayoshi.

Download Presentation

B.V. Jackson, and P.P. Hick, A. Buffington, J.M. Clover, N. Amirbekian

An Image/Link below is provided (as is) to download presentation

Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.


- - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - -

Presentation Transcript


B v jackson and p p hick a buffington j m clover n amirbekian

B.V. Jackson,

and

P.P. Hick, A. Buffington, J.M. Clover, N. Amirbekian

Center for Astrophysics and Space Sciences,

University of California at San Diego, LaJolla, CA, USA

and

D.B. Reisenfeld

Department of Physics and Astronomy, University of Montana, Missoula, MT, USA

Masayoshi

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


B v jackson and p p hick a buffington j m clover n amirbekian

Introduction:

The Digital Analysis: 3-D Heliospheric Tomography – (a fit to data)

(Time-dependent view from a single observer location)

The Data Sets:

IPS (Intestellar Scintillation), SMEI (the Solar Mass Ejection Imager)

The Motive: Voyager Solar Wind Measurements, 3-D Interstellar boundary

This Project:

An inner heliospheric boundary


Stelab ips heliospheric analyses

STELab IPS Heliospheric Analyses

DATA

STELab IPS array near Fujioperating at 327 MHz


Current stelab ips heliospheric analyses

Current STELab IPS Heliospheric Analyses

New STELab IPS array at Toyokawa - photo February 17, 2007 (new 327 MHz array now operates)


Scintillation level heliospheric analysis

Scintillation Level Heliospheric Analysis

Jackson, B.V., et al., 2008, Adv. in Geosciences , 21, 339-366.

Intensity interplanetary scintillation (IPS) g-levels.

STELab IPS

IPS line-of-sight response

g = m/<m>


Heliospheric 3 d reconstruction

Heliospheric 3-D Reconstruction

Jackson, B.V., et al., 2008, Adv. in Geosciences , 21, 339-366.

The outward-flowing solar wind structure follows very specific physics as it moves outward from the Sun

LOS Weighting


Heliospheric 3 d reconstruction1

Heliospheric 3-D Reconstruction

Jackson, B.V., et al., 2008, Adv. in Geosciences , 21, 339-366.

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.

13 July 2000

14 July 2000


B v jackson and p p hick a buffington j m clover n amirbekian

Jackson, B.V., et al., 2008, Adv. in Geosciences , 21, 339-366.

The UCSD 3D-reconstruction program

The “traceback matrix”(any solar-wind model works)In the traceback matrix the location of the upper level data point (starred) is an interpolation in x of Δx2 and the unit x distance – Δx3 distance or (1 – Δx3). Similarly, the value of Δt at the starred point is interpolated by the same spatial distance. Each 3D traceback matrix contains a regular grid of values ΣΔx, ΣΔy, ΣΔt, ΣΔv, and ΣΔm that locates the origin of each point in the grid at each time and its change in velocity and density from the heliospheric model.


B v jackson and p p hick a buffington j m clover n amirbekian

http://ips.ucsd.edu/

UCSD time-dependent IPS Web forecast

Velocity model time-series

G-level sky map

Real-time tomographic analysis of the solar wind on April 29-30, 2004 showing a halo CME response in the interplanetary medium.

Web Analysis Runs Automatically Using Linux on a P.C.


B v jackson and p p hick a buffington j m clover n amirbekian

Tokumaru, M., et al., 2010, J. Geophys Res. (in press).

“Solar cycle evolution of the solar wind speed from 1985-2008”

(part of the result is shown here).

The recently past solar minimum is pretty special in that there is a large variation of solar wind speed over solar latitude.


B v jackson and p p hick a buffington j m clover n amirbekian

UCSD time-dependent IPS Velocity and density analysis (also at the CCMC)

Density ecliptic cut

Velocity ecliptic cut

Tomographic analysis of the solar wind for Carrington rotation 2085

(2009/06/26 – 2009/07/23).


B v jackson and p p hick a buffington j m clover n amirbekian

UCSD time-dependent IPS Velocity and density analysis (also at the CCMC)

Density meridional cut

Velocity meridional cut

Tomographic analysis of the solar wind for Carrington rotation 2085

(2009/06/26 – 2009/07/23).


B v jackson and p p hick a buffington j m clover n amirbekian

UCSD time-dependent IPS Velocity and density analysis (also at the CCMC)

Density remote-observer view

Velocity remote-observer view

Tomographic analysis of the solar wind for Carrington rotation 2085

(2009/06/26 – 2009/07/23).


B v jackson and p p hick a buffington j m clover n amirbekian

The Solar Mass Ejection Imager (SMEI) Mission -- Journal Article

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 Coriolis spacecraft at Vandenberg prior to flight. The SMEI baffles are circled. The large NRL radiometer Windsat is on the top of the spacecraft.


Data lots of data

Data!! Lots of Data!!

<---Sun

C1

C2

C3

Sun

|

V

Simultaneous images from the three SMEI cameras.


B v jackson and p p hick a buffington j m clover n amirbekian

Frame Composite for Aitoff Map

Blue = Cam3; Green= Cam2; Red = Cam1

D290; 17 October 2003


Smei first light composite image

SMEI first light composite image

Composite all-sky map Feb 2, 2003 from the three SMEI cameras.


The signal we observe with smei

The signal we observe with SMEI


B v jackson and p p hick a buffington j m clover n amirbekian

Images from the 3-D reconstructions

26 May – 05 June 2003, (May 28 ‘Halo’ CME)


B v jackson and p p hick a buffington j m clover n amirbekian

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

Other

2003 May 27-28 CME events

SMEI density 3D reconstruction of the 28 May 2003 halo CME as viewed from 15º above the ecliptic plane about 30º east of the Sun-Earth line.

SMEI density (remote observer view) of the 28 May 2003 halo CME


B v jackson and p p hick a buffington j m clover n amirbekian

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

SMEI &

IPS

27-28 May 2003 CME event period

IPS Velocity and SMEI proton density reconstruction of the 27-28 May 2003 halo CME sequence. Reconstructed and Windin-situ densities are compared with over one Carrington rotation.


B v jackson and p p hick a buffington j m clover n amirbekian

26 April 2008 CME/ICME

SMEI difference image

LASCO

SMEI

SMEI 3-D reconstruction of the 26 April 2008 CME as it arrives at Earth and the STEREO-B spacecraft.


B v jackson and p p hick a buffington j m clover n amirbekian

26-29 April 2008 period

SMEI

SMEI

ENLIL

SMEI proton density 3-D reconstruction of the 26 April 2008 CME as it arrives at Earth and the STEREO spacecraft compared with ENLIL.


B v jackson and p p hick a buffington j m clover n amirbekian

27-30 April 2008 period

SMEI 3-D Reconstructed densities (most of the ICME density is North and East of STEREO-B.


B v jackson and p p hick a buffington j m clover n amirbekian

27-30 April 2008 period

SMEI/STEREO-B density

SMEI/STEREO-B density

IPS/STEREO-B velocity

3-D Reconstructed and STEREO-Bin-situ densities and velocities.


B v jackson and p p hick a buffington j m clover n amirbekian

To go farther distances from the Sun:

The best procedure is to obtain an inner heliosphere boundary of physical parameters, and using the best physics, extrapolate this outward to the largest distance possible.

We expect some variation in the inner solar wind will be manifest in Voyager or ENA flux observed at large distances from the Sun.

In this way one hopes to learn more about the physics and the digital process that provides this extrapolation to the observed distant heliosphere.


B v jackson and p p hick a buffington j m clover n amirbekian

The interstellar boundary.


B v jackson and p p hick a buffington j m clover n amirbekian

The interstellar boundary.


B v jackson and p p hick a buffington j m clover n amirbekian

Possible Sources of the IBEX “Ribbon”


B v jackson and p p hick a buffington j m clover n amirbekian

4065 eV

In addition:

2008

2558 eV

1726 eV

2009

North ecliptic pole heliospheric 0.5 AU pressure.

North ecliptic pole ENAs (IBEX launch 2008 October 19)

(Dan Reisenfeld)


B v jackson and p p hick a buffington j m clover n amirbekian

Carrington Rotations 2084-2085

Speed at 0.5 AU (ecliptic coordinates).


B v jackson and p p hick a buffington j m clover n amirbekian

Carrington Rotations 2084-2085

Density at 0.5 AU (ecliptic coordinates).


B v jackson and p p hick a buffington j m clover n amirbekian

Carrington Rotations 2084-2085

Pressure at 0.5 AU (ecliptic coordinates).


B v jackson and p p hick a buffington j m clover n amirbekian

2008

2009

North ecliptic pole heliospheric 0.5 AU density and velocity from the IPS density (normalized to 1 AU).


B v jackson and p p hick a buffington j m clover n amirbekian

4065 eV

2008

2558 eV

1726 eV

2009

North ecliptic pole heliospheric 0.5 AU pressure.

North ecliptic pole ENAs (IBEX launch 2008 October 19)

(Dan Reisenfeld)


B v jackson and p p hick a buffington j m clover n amirbekian

Summary:

The analysis of IPS data provides low-resolution global measurements of density and velocity with a time cadence of about a day.

There are several data sources (IPS, SMEI), but the most long-term and substantiated (that also measure velocity globally) are the STELab arrays in Japan.

Accurate observations of inner heliosphere parameters coupled withthe best physicscan extrapolate these outward to the interstellar boundary.


  • Login