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.

Slides:



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

An overview of the cycle variations in the solar corona Louise Harra UCL Department of Space and Climate Physics Mullard Space Science.
Interaction of coronal mass ejections with large-scale structures N. Gopalswamy, S. Yashiro, H. Xie, S. Akiyama, and P. Mäkelä IHY – ISWI Regional meeting.
Study of Galactic Cosmic Rays at high cut- off rigidity during solar cycle 23 Partha Chowdhury 1 and B.N. Dwivedi 2 1 Department of Physics, University.
Global Distribution of Slow Solar Wind N. U. Crooker, S. W. Antiochos, X. Zhao, Yi-M. Wang, and M. Neugebauer.
Weaker Solar Wind Over the Protracted Solar Minimum Dave McComas Southwest Research Institute San Antonio, TX With input from and thanks to Heather Elliott,
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.
1 Grades 3 - 5: Introduction. 2 Better Observation Of The Sun And Earth Importance of Space Technology.
Comparing the Large-Scale Magnetic Field During the Last Three Solar Cycles Todd Hoeksema.
Evolution of the Large-Scale Magnetic Field Over Three Solar Cycles Todd Hoeksema.
AGU – Fall 2006 The Solar Polar Field – Cycles 21 – 23 The Solar Polar Field During Solar Cycles J. Todd Hoeksema, Yang Liu, XuePu Zhao & Elena Benevolenskaya.
High-latitude activity and its relationship to the mid-latitude solar activity. Elena E. Benevolenskaya & J. Todd Hoeksema Stanford University Abstract.
A particularly obvious example of daily changing background noise level Constructing the BEST High-Resolution Synoptic Maps from MDI J.T. Hoeksema, Y.
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.
Relationship between the High and mid latitude Solar Magnetic Field Elena E. Benevolenskaya J. Todd Hoeksema Stanford University.
Helicity as a Component of Filament Formation D.H. Mackay University of St. Andrews Solar Theory Group.
Absence of a Long Lasting Southward Displacement of the HCS Near the Minimum Preceding Solar Cycle 24 X. P. Zhao, J. T. Hoeksema and P. H. Scherrer Stanford.
1 Interpolation of polar field Y. Liu, J. T. Hoeksema, X. P. Zhao, R. M. Larson – Stanford University
A particularly obvious example of daily changing background noise level Constructing the BEST High-Resolution Synoptic Maps from MDI J.T. Hoeksema, Y.
Session 6 Key Questions for Understanding This Unusual Solar Minimum Alan Gabriel Todd Hoeksema Janet Luhmann Bill Matthaeus Neil Sheeley.
1. Background2. Flux variation3. Polarity reversal4. Electron evolution5. Conclusions The role of coronal mass ejections in the solar cycle evolution of.
Predictions of Solar Wind Speed and IMF Polarity Using Near-Real-Time Solar Magnetic Field Updates C. “Nick” Arge University of Colorado/CIRES & NOAA/SEC.
Thomas Zurbuchen University of Michigan The Structure and Sources of the Solar Wind during the Solar Cycle.
A topological view of 3D global magnetic field reversal in the solar corona Rhona Maclean Armagh Observatory 5 th December 2006.
The Asymmetric Polar Field Reversal – Long-Term Observations from WSO J. Todd Hoeksema, Solar Observatories H.E.P.L., Stanford University SH13C-2278.
Solar Rotation Lab 3. Differential Rotation The sun lacks a fixed rotation rate Since it is composed of a gaseous plasma, the rate of rotation is fastest.
1 C. “Nick” Arge Space Vehicles Directorate/Air Force Research Laboratory SHINE Workshop Aug. 2, 2007 Comparing the Observed and Modeled Global Heliospheric.
Katya Georgieva Boian Kirov Simeon Asenovski
Flares in and their associations with CMEs N.V. Nitta, J.P.Wuelser, M. J. Aschwanden, J. R. Lemen (LMSAL), D. M. Zarro (Adnet, Inc.)
Proxies of the Entire Surface Distribution of the Photospheric Magnetic Field Xuepu Zhao NAOC, Oct. 18, 2011.
Study of Local Heliospheric Current Sheet Variations from Multi-Spacecraft Observations D. Arrazola · J.J. Blanco · J. Rodríguez-Pacheco · M.A. Hidalgo.
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,
The Solar Wind.
Introduction to Space Weather Jie Zhang CSI 662 / PHYS 660 Spring, 2012 Copyright © The Heliosphere: The Solar Wind March 01, 2012.
Propagation Trends Dayton 2014 Solar Maximum! But the slow decline to solar minimum in 2020 is likely to begin later this year.
Seasonal Climate Cycles Solar Radiation at the Earth’s Surface.
Solar Maximum ! A Double Peaked Sunspot Cycle ?
1 The Geo-Response to Extreme Solar Events: How Bad Can it Get? Leif Svalgaard Stanford University, California, USA AOGS,
1 Abramenko V.I., 1 Yurchyshyn, V., 2 Linker, J., 2 Mikic, Z. 1 - Big Bear Solar Observatory of NJIT; 2 – Predictive Science Inc., San Diego Anomalous.
1 The Mean Field of the Sun Leif Svalgaard Stanford University Sept. 2, 2011.
Polar Magnetic Field Elena E. Benevolenskaya Stanford University SDO Team Meeting 2009.
Global Structure of the Inner Solar Wind and it's Dynamic in the Solar Activity Cycle from IPS Observations with Multi-Beam Radio Telescope BSA LPI Chashei.
WSM Whole Sun Month Sarah Gibson If the Sun is so quiet, why is the Earth still ringing?
SHINE 2009 Workshop, August What is an Extreme Solar Minimum? W. Dean Pesnell NASA, Goddard Space Flight Center.
Ahmed A. HADY Astronomy Department Cairo University Egypt Deep Solar Minimum of Cycle23 and its Impact and its Impact.
Introduction to Space Weather Jie Zhang CSI 662 / PHYS 660 Fall, 2009 Copyright © The Heliosphere: Solar Wind Oct. 08, 2009.
Chapter 0: Charting the Heavens. Units of Chapter 0 The “Obvious” View Earth’s Orbital Motion The Motion of the Moon The Measurement of Distance Science.
Monday Seminar Talk (short) 17 November, 2003 Taro Morimoto.
CSI 769/ASTR 769 Topics in Space Weather Fall 2005 Lecture 03 Sep. 20, 2005 Surface Magnetic Field Aschwanden, “Physics of the Solar Corona” Chap. 5, P.
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.
The Decline to Solar Minimum 2014 through about 2020
HMI-WSO Solar Polar Fields and Nobeyama 17 GHz Emission
Review Question Why does the Sun shine?.
Predictions for solar cycle 25
Large-Scale Solar Magnetic Fields – How is Solar Cycle 24 Different?
Carrington Rotation 2106 – Close-up of AR Mr 2106 Bt 2106
Current HMI Polar Fields
How does the solar atmosphere connect to the inner heliosphere?
Lecture 5 The Formation and Evolution of CIRS
MDI Global Field & Solar Wind
Solar Activity Chapter 8 Section 3.
Solar and Heliospheric Physics
Solar Activity Chapter 8 Section 3.
Grades 3 - 5: Introduction
The Solar Cycle 24 Consensus Prediction
J. Todd Hoeksema Stanford University
Grades 3 - 5: Introduction
A Presentation to the SHINE ’02 Workshop by J.G. Luhmann
Closing the Books on Cycle 24 J
Presentation transcript:

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 J. Todd Hoeksema Stanford University

2 July 31, 2007 SHINE 2007 – Heliospheric Plasma Sheet Comparison of Solar Cycles 21 – 22 – 23 – Consistent observations from WSO since 1976 – the beginning of Cycle 21 Typical evolution of model heliospheric current sheet follows pattern through cycle Minimum HCS resembles dipole – until now

3 July 31, 2007 SHINE 2007 – Heliospheric Plasma Sheet Potential Field – Source Surface Simple Model of Coronal Field Carrington Rotation 1912 – August 1996 Whole Sun Month – Elephant’s Trunk

4 July 31, 2007 SHINE 2007 – Heliospheric Plasma Sheet Typical Solar Cycle – 22 Minimum 1986 Rising 1988 Max & Polar Reversal 1989 Early Decline 1991 Later Decline 1993 Pre-Min 1995

5 July 31, 2007 SHINE 2007 – Heliospheric Plasma Sheet Solar Cycle Every 8 th Rotation X2 CR

6 July 31, 2007 SHINE 2007 – Heliospheric Plasma Sheet Solar Cycle Every 8 th Rotation X2 CR

7 July 31, 2007 SHINE 2007 – Heliospheric Plasma Sheet Solar Cycle Every 8 th Rotation X2 CR

8 July 31, 2007 SHINE 2007 – Heliospheric Plasma Sheet Comparison of Cycles 21 & 22 Every 9 th Rotation X – 1986 CR 1650 – – 1996 CR 1790 – 1916

9 July 31, 2007 SHINE 2007 – Heliospheric Plasma Sheet Comparison of Cycles 22 & 23 Every 9 th Rotation X – 1996 CR 1790 – – 2006 CR

10 July 31, 2007 SHINE 2007 – Heliospheric Plasma Sheet Comparison of Cycles 21 & 23 Every 9 th Rotation X – 1986 CR 1645 – – 2006 CR 1920 – 2046

11 July 31, 2007 SHINE 2007 – Heliospheric Plasma Sheet Comparison of Minima at Start of Cycles – Cycle – Cycle – Cycle – Cycle 23.95(?)

12 July 31, 2007 SHINE 2007 – Heliospheric Plasma Sheet

13 July 31, 2007 SHINE 2007 – Heliospheric Plasma Sheet Polar Field Measured at WSO from

14 July 31, 2007 SHINE 2007 – Heliospheric Plasma Sheet Summary Each solar cycle follows a similar pattern of evolution Each cycle shows different features depending on AR emergence Polar field dominates minimum Polar field at end of Cycle 23 is very weak HCS reaches higher latitude and has more structure in 2007 than expected

15 July 31, 2007 SHINE 2007 – Heliospheric Plasma Sheet North Polar Field Strength