Causes and Effects of Superstorms Associated with the Magnetic Field in the Corona and the Heliosphere

1
Causes and Effects of SuperstormsAssociated with
the Magnetic Field in the Corona and the
Heliosphere

• J. Todd Hoeksema
• Stanford University

2
Premonition of Activity
14 Days Before CMP!
3
Observations of Regions 486 488
14D Before
Central Meridian
14D Later
Far Side
4
The Photosphere
5
The Magnetic Field
6
Another View of the Surface
7
The Coronal Response
Tom Bridgman NASA/Goddard Space Flight Center
Scientific Visualization Studio
8
The Heliospheric Field
9
The Heliospheric Field
10
Several Rotations
-3
1
-1
2
6
0
11
Did the open field line connections change?
Thanks to Yang Liu at Stanford For the following
figures
12
Evolution of magnetic field in this period
Central meridian CR2007_290 degree in
Longitude (Sept. 4)
Central meridian CR2008_290 degree in
Longitude (Oct. 1)
0464
0488
Central meridian CR2009_290 degree in
Longitude (Oct. 28)
0484
0486
Central meridian CR2010_290 degree in
Longitude (Nov. 25)
0501
Not usual 180 centering
13
Evolution of magnetic field in this period
Central meridian CR2007_290 degree in Longitude
(Sept. 4)
Central meridian CR2008_290 degree in Longitude
(Oct. 1)
0464
Date (mm/dd/yy) Time (UT) Speed (cone) Accel. (cone) Flares (Preliminary) Flares (Preliminary) Flares (Preliminary) Flares (Preliminary)
10/21/03 0354 1853 -226.5 AR0484 C8/SF
10/28/03 1130 2319 -135.8 AR0486 X17/4B
10/29/03 2054 2093 -186.6 AR0486 X10/2B
11/02/03 1730 2986 -193.3 AR0486 X8/2B
11/04/03 1206 1020 -40.6 AR0486 C6
11/04/03 1954 2996 -385.5 AR0486 X28/3B
11/07/03 1554 2233 -85.0 AR0486
11/11/03 1354 2436 -340.0 AR0498 M1/SF
11/18/03 0850 1663 -69.2 AR0501 M3.9
11/18/03 0950 2720 210.1 M4.5
0488
Central meridian CR2009_290 degree in Longitude
(Oct. 28)
0484
0486
Central meridian CR2010_290 degree in Longitude
(Nov. 25)
0501
14
AR0464 (0484, 0501) and large-scale magnetic
field
CR2007290 Sept 4
CR2008290 Oct 1
0464
0464
0464
15
AR0486, AR0488 and large-scale magnetic field
CR2008290 Oct 1
CR2009290 Oct 28
0488
0486
16
Extremely fast halo CMEs and active regions
Date (mm/dd/yy) Time (UT) Speed (cone) Accel. (cone) Flares (Preliminary) Flares (Preliminary) Flares (Preliminary) Flares (Preliminary)
10/21/03 0354 1853 -226.5 AR0484 C8/SF
10/28/03 1130 2319 -135.8 AR0486 X17/4B
10/29/03 2054 2093 -186.6 AR0486 X10/2B
11/02/03 1730 2986 -193.3 AR0486 X8/2B
11/04/03 1206 1020 -40.6 AR0486 C6
11/04/03 1954 2996 -385.5 AR0486 X28/3B
11/07/03 1554 2233 -85.0 AR0486
11/11/03 1354 2436 -340.0 AR0498 M1/SF
11/18/03 0850 1663 -69.2 AR0501 M3.9
11/18/03 0950 2720 210.1 M4.5
AR0486, together with AR0488, produced a big open
field area after they emerged.
AR0464 (a.k.a. 0484, 0501) emerged within/close
to an area with large-scale open magnetic field .
?
The active regions associated with these high
speed halo CMEs are closely associated with
sources of already open magnetic flux, except
AR0498. In this way the open magnetic field
provides an avenue for CMEs to blow out.
17
AR0498 and large-scale magnetic field
CR2009160
0498
18
Conclusions

• The photospheric field changed dramatically in CR
  2009 October 2003
• Numerous dramatic high-speed CMEs blasted
  through the corona and heliosphere
• New flux emerged in such a way as to reinforce
  the existing structure
• New open flux regions had easy access to the
  heliosphere
• The ambient large-scale structure of the
  heliospheric current sheet changed very little!
• This is consistent with earlier results of Zhao
  Hoeksema, JGR, 1996.