J. Todd Hoeksema Stanford University

Slides:



Advertisements
Similar presentations
The Solar Polar Field Reversal Observed By SOHO/MDI Yang Liu, J. Todd Hoeksema, X-P Zhao – Stanford University
Advertisements

Estimating the magnetic energy in solar magnetic configurations Stéphane Régnier Reconnection seminar on Thursday 15 December 2005.
An overview of the cycle variations in the solar corona Louise Harra UCL Department of Space and Climate Physics Mullard Space Science.
Reviewing the Summer School Solar Labs Nicholas Gross.
1 Diagnostics of Solar Wind Processes Using the Total Perpendicular Pressure Lan Jian, C. T. Russell, and J. T. Gosling How does the magnetic structure.
STEREO AND SPACE WEATHER Variable conditions in space that can have adverse effects on human life and society Space Weather: Variable conditions in space.
Modeling the Magnetic Field Evolution of the December Eruptive Flare Yuhong Fan High Altitude Observatory, National Center for Atmospheric Research.
Heliospheric MHD Modeling of the May 12, 1997 Event MURI Meeting, UCB/SSL, Berkeley, CA, March 1-3, 2004 Dusan Odstrcil University of Colorado/CIRES &
Flows in Active Regions Inferred from the Time-distance and the DAVE4VM.
High-latitude activity and its relationship to the mid-latitude solar activity. Elena E. Benevolenskaya & J. Todd Hoeksema Stanford University Abstract.
August 2006 IAU Assembly Halo CMEs and Configuration of Magnetic Field Yang Liu – Stanford University
M3 Session AIA/HMI Science Meeting D-1 : M3-Magnetic Field Data Products Data Product Development Session Chairs: R. Larsen/Y. Liu Status: [draft]
HMI/AIA Science Team Meeting, HMI Science Goals Alexander Kosovichev & HMI Team.
The Hunt for a Link : Quantitative Connections Between Magnetic Fields and EIT Coronal Wave/CME Properties Prepared by James R. Robertson J.R. In conjunction.
Understanding Magnetic Eruptions on the Sun and their Interplanetary Consequences A Solar and Heliospheric Research grant funded by the DoD MURI program.
Understanding Magnetic Eruptions on the Sun and their Interplanetary Consequences A Solar and Heliospheric Research grant funded by the DoD MURI program.
September 2007LWS 2007 Halo CMEs and Configuration of the Ambient Magnetic Field Yang Liu – Stanford University
Prediction of Central Axis Direction of Magnetic Clouds Xuepu Zhao and Yang Liu Stanford University The West Pacific Geophysics Meeting, Beijing, China.
Relationship Between Magnetic Clouds and Earth-Directed CMEs: Space Weather Research in Stanford Solar Group Xuepu Zhao The Second International Space.
1 Synoptic Maps of Magnetic Field from MDI Magnetograms: polar field interpolation. Y. Liu, J. T. Hoeksema, X. P. Zhao, R. M. Larson – Stanford University.
1Yang Liu1997 May 12 Event The 1997 May 12 Event Yang Liu – Stanford University
C. May 12, 1997 Interplanetary Event. Ambient Solar Wind Models SAIC 3-D MHD steady state coronal model based on photospheric field maps CU/CIRES-NOAA/SEC.
The May 1,1998 and May 12, 1997 MURI events George H. Fisher UC Berkeley.
Flows in Active Regions Inferred from the Time-distance and the DAVE4VM.
Observations of December 2006 events Yang Liu – Stanford University
AR 10759/ May Event Overview
1 July 31, 2007 SHINE 2007 – Heliospheric Plasma Sheet The Unusual Heliospheric Current Sheet at the End of Cycle 23 A Comparison of Cycles 21,22,& 23.
February 26, 2007 KIPAC Workshop on Magnetism Modeling/Inferring Coronal And Heliospheric Field From Photospheric Magnetic Field Yang Liu – Stanford University.
Space Weather Forecast With HMI Magnetograms: Proposed data products Yang Liu, J. T. Hoeksema, and HMI Team.
A particularly obvious example of daily changing background noise level Constructing the BEST High-Resolution Synoptic Maps from MDI J.T. Hoeksema, Y.
C. May 12, 1997 Interplanetary Event. May 12, 1997 Interplanetary Coronal Mass Ejection Event CU/CIRES, NOAA/SEC, SAIC, Stanford Tatranska Lomnica, Slovakia,
Sung-Hong Park Space Weather Research Laboratory New Jersey Institute of Technology Study of Magnetic Helicity and Its Relationship with Solar Activities:
Photospheric Sources of Very Fast (>1100km/s) Coronal Mass Ejections Recent studies show that only very fast CMEs (> 1100 km/s) are capable of producing.
Coronal and Heliospheric Modeling of the May 12, 1997 MURI Event MURI Project Review, NASA/GSFC, MD, August 5-6, 2003 Dusan Odstrcil University of Colorado/CIRES.
UCB MURI Team Introduction An overview of ongoing work to understand a well observed, eruptive active region, along with closely related studies…..
Page 1Hinode4 October 11-15, 2010 Studying Emerging Flux Regions With The SDO Data Yang Liu and HMI Team Stanford University and Other Places
The May 1997 and May 1998 MURI events George H. Fisher UC Berkeley.
LINE OF SIGHT MAGNETIC FIELD EVOLUTION & DATA ANALYSIS Dandan Ye.
Thomas Zurbuchen University of Michigan The Structure and Sources of the Solar Wind during the Solar Cycle.
The Asymmetric Polar Field Reversal – Long-Term Observations from WSO J. Todd Hoeksema, Solar Observatories H.E.P.L., Stanford University SH13C-2278.
Proxies of the Entire Surface Distribution of the Photospheric Magnetic Field Xuepu Zhao NAOC, Oct. 18, 2011.
1Yang Liu/Magnetic FieldHMI Science – 1 May 2003 Magnetic Field Goals – magnetic field & eruptive events Yang Liu Stanford University.
A Presentation to the SHINE ’02 Workshop by J.G. Luhmann (August 19, 2002) CME initiation: A zoo not an animal (Images from the on-line CDAW CME catalogue.
SHINE SEP Campaign Events: Long-term development of solar corona in build-up to the SEP events of 21 April 2002 and 24 August 2002 A. J. Coyner, D. Alexander,
Stream interface slope near 1 AU and the configuration of the heliospheric current sheet at 2.5 solar radii K.D.C. Simunac STEREO SWG October 2009.
Coronal and Interplanetary Magnetic Fields in October-November 2003 and November CMEs Vasyl Yurchyshyn Big Bear Solar Observatory,
Anemone Structure of AR NOAA and Related Geo-Effective Flares and CMEs A. Asai 1 ( 浅井 歩 ), T.T. Ishii 2, K. Shibata 2, N. Gopalswamy 3 1: Nobeyama.
Heliospheric Simulations of the SHINE Campaign Events SHINE Workshop, Big Sky, MT, June 27 – July 2, 2004 Dusan Odstrcil 1,2 1 University of Colorado/CIRES,
On Coronal Mass Ejections and Configurations of the Ambient Magnetic Field Yang Liu Stanford University 3/17/ COSPAR 2008.
State of NOAA-SEC/CIRES STEREO Heliospheric Models STEREO SWG Meeting, NOAA/SEC, Boulder, CO, March 22, 2004 Dusan Odstrcil University of Colorado/CIRES.
October-November CMEs Yang Liu – Stanford University
BBSO 2007 Science Planning. Focal Plane Instruments AO (Wenda, Nicolas, Deqing, Patricia and Park) AO (Wenda, Nicolas, Deqing, Patricia and Park) IRIM.
Helicity Thinkshop 2009, Beijing Asymmetry of helicity injection in emerging active regions L. Tian, D. Alexander Rice University, USA Y. Liu Yunnan Astronomical.
Long-term measurements of the Sun’s poles show that reversal of the dominant magnetic polarity generally occurs within a year of solar maximum. Current.
Large-Scale Solar Magnetic Fields – How is Solar Cycle 24 Different?
Carrington Rotation 2106 – Close-up of AR Mr 2106 Bt 2106
Orientations of Halo CMEs and Magnetic Clouds
Orientations of Halo CMEs and Magnetic Clouds
Anemone Structure and Geo-Effective Flares/CMEs
Magnetic Topology of the 29 October 2003 X10 Flare
Exploring Large-scale Coronal Magnetic Field Over Extended Longitudes With EUVI EUVI B EIT EUVI A 23-Mar UT Nariaki Nitta, Marc DeRosa, Jean-Pierre.
Corona Mass Ejection (CME) Solar Energetic Particle Events
How does the solar atmosphere connect to the inner heliosphere?
Observations of December 2006 events
Anemone Structure of AR NOAA and Related Geo-Effective Flares and CMEs
SIDC Space Weather briefing
Do Now 12/9/09 What is the sun made of???
Space Weather: Science, Effects, Forecasts and Services.
A Presentation to the SHINE ’02 Workshop by J.G. Luhmann
Closing the Books on Cycle 24 J
Presentation transcript:

J. Todd Hoeksema Stanford University Causes and Effects of Superstorms Associated with the Magnetic Field in the Corona and the Heliosphere J. Todd Hoeksema Stanford University

Premonition of Activity 14 Days Before CMP!

Observations of Regions 486 & 488 14D Before Central Meridian 14D Later Far Side

The Photosphere

The Magnetic Field

Another View of the Surface

The Coronal Response Tom Bridgman NASA/Goddard Space Flight Center Scientific Visualization Studio

The Heliospheric Field

The Heliospheric Field

Several Rotations -3 +1 -1 +2 +6

Did the open field line connections change? Thanks to Yang Liu at Stanford For the following figures

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

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. Flares (Preliminary) 10/21/03 03:54 1853 -226.5 AR0484 C8/SF 10/28/03 11:30 2319 -135.8 AR0486 X17/4B 10/29/03 20:54 2093 -186.6 X10/2B 11/02/03 17:30 2986 -193.3 X8/2B 11/04/03 12:06 1020 -40.6 C6 19:54 2996 -385.5 X28/3B 11/07/03 15:54 2233 -85.0 11/11/03 13:54 2436 -340.0 AR0498 M1/SF 11/18/03 08:50 1663 -69.2 AR0501 M3.9 09:50 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

AR0464 (0484, 0501) and large-scale magnetic field CR2007:290: Sept 4 CR2008:290: Oct 1 0464 0464 0464

AR0486, AR0488 and large-scale magnetic field CR2008:290: Oct 1 CR2009:290: Oct 28 0488 0486

Extremely fast halo CMEs and active regions Date (mm/dd/yy) Time (UT) Speed (cone) Accel. Flares (Preliminary) 10/21/03 03:54 1853 -226.5 AR0484 C8/SF 10/28/03 11:30 2319 -135.8 AR0486 X17/4B 10/29/03 20:54 2093 -186.6 X10/2B 11/02/03 17:30 2986 -193.3 X8/2B 11/04/03 12:06 1020 -40.6 C6 19:54 2996 -385.5 X28/3B 11/07/03 15:54 2233 -85.0 11/11/03 13:54 2436 -340.0 AR0498 M1/SF 11/18/03 08:50 1663 -69.2 AR0501 M3.9 09:50 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.

AR0498 and large-scale magnetic field CR2009:160 0498

Conclusions The photospheric field changed dramatically in CR 2009; October 2003 Numerous dramatic high-speed CME’s 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.