Long Term Measurements of Solar Wind Fe Charge States Mark Popecki, A. Galvin, L. M. Kistler,H. Kucharek, E. Moebius, K. Simunac, P. Bochsler, L. M. Blush,

Slides:



Advertisements
Similar presentations
Uncovering the Global Slow Solar Wind Liang Zhao and Thomas H. Zurbuchen Department of Atmospheric, Oceanic and Space Sciences, University of Michigan.
Advertisements

The Radial Variation of Interplanetary Shocks C.T. Russell, H.R. Lai, L.K. Jian, J.G. Luhmann, A. Wennmacher STEREO SWG Lake Winnepesaukee New Hampshire.
Coronal Responses to Explosive Events Adria C. Updike Smith College / Harvard-Smithsonian Center for Astrophysics Amy Winebarger and Kathy Reeves, Center.
4/18 6:08 UT 4/17 6:09 UT Average polar cap flux North cap South cap… South cap South enter (need to modify search so we are here) South exit SAA Kress,
Interaction of coronal mass ejections with large-scale structures N. Gopalswamy, S. Yashiro, H. Xie, S. Akiyama, and P. Mäkelä IHY – ISWI Regional meeting.
An Analysis of Heliospheric Magnetic Field Flux Based on Sunspot Number from 1750 to Today and Prediction for the Coming Solar Minimum Introduction The.
Reviewing the Summer School Solar Labs Nicholas Gross.
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,
Long Term Measurements of Solar Wind Fe Charge States: Charge State Distributions Mark Popecki, A. Galvin, L. M. Kistler,H. Kucharek, E. Moebius, K. Simunac,
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.
Five Spacecraft Observations of Oppositely Directed Exhaust Jets from a Magnetic Reconnection X-line Extending > 4.3 x 10 6 km in the Solar Wind Gosling.
RHESSI/GOES Observations of the Non-flaring Sun from 2002 to J. McTiernan SSL/UCB.
Jonathan A. Constable University of St Andrews Solar REU Presentation 2009 A flux rope model for CME initiation over solar cycle 23 Jonathan Constable.
RHESSI/GOES Observations of the Non-flaring Sun from 2002 to J. McTiernan SSL/UCB.
Synoptic maps and applications Yan Li Space Sciences Laboratory University of California, Berkeley, CA HMI team meeting, Jan 27, 2005, Stanford.
The Non-Flare Temperature and Emission Measure Observed by RHESSI and SXI J.McTiernan (SSL/UCB) J.Klimchuk (NRL) Fall 2003 AGU Meeting.
He+ Suprathermal Tails as Observed by STEREO/PLASTIC Mark Popecki (UNH) and Berndt Klecker (MPE) Kennebunkport June 10, 2010.
Prediction of Central Axis Direction of Magnetic Clouds Xuepu Zhao and Yang Liu Stanford University The West Pacific Geophysics Meeting, Beijing, China.
Identifying and Modeling Coronal Holes Observed by SDO/AIA, STEREO /A and B Using HMI Synchronic Frames X. P. Zhao, J. T. Hoeksema, Y. Liu, P. H. Scherrer.
Study of magnetic helicity in solar active regions: For a better understanding of solar flares Sung-Hong Park Center for Solar-Terrestrial Research New.
Plasma in the Heliosheath John Richardson M.I.T. Collaborators: J. Belcher, J. Kasper, E. Stone, C. Wang.
Sung-Hong Park Space Weather Research Laboratory New Jersey Institute of Technology Study of Magnetic Helicity and Its Relationship with Solar Activities:
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.
From Maunder Minimum to the recent Grand Solar Maximum 11:45 Tuesday November 18 auditorium Roger Session: 6. Key solar observables for assessing long-term.
1 Hinode Monthly Highlights – Slow Solar Wind Sources Derived from recent publication from the Hinode/EIS team through the Naval Research Laboratory EIS.
The Effect of Solar Wind on Pulsar Observations Xiaopeng YOU Southwest University, Chongqing, China.
The Asymmetric Polar Field Reversal – Long-Term Observations from WSO J. Todd Hoeksema, Solar Observatories H.E.P.L., Stanford University SH13C-2278.
The Sun and the Heliosphere: some basic concepts…
The Sun. Solar Prominence Sun Fact Sheet The Sun is a normal G2 star, one of more than 100 billion stars in our galaxy. Diameter: 1,390,000 km (Earth.
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
Proxies of the Entire Surface Distribution of the Photospheric Magnetic Field Xuepu Zhao NAOC, Oct. 18, 2011.
Magnetic Storm Generation by Various Types of Solar Wind: Event Catalog, Modeling and Prediction N. S. Nikolaeva, Yu.I. Yermolaev, and I. G. Lodkina Space.
Locating the solar source of 13 April 2006 Magnetic Cloud K. Steed 1, C. J. Owen 1, L. K. Harra 1, L. M. Green 1, S. Dasso 2, A. P. Walsh 1, P. Démoulin.
1 THE RELATION BETWEEN CORONAL EIT WAVE AND MAGNETIC CONFIGURATION Speakers: Xin Chen
Comparison of the 3D MHD Solar Wind Model Results with ACE Data 2007 SHINE Student Day Whistler, B. C., Canada C. O. Lee*, J. G. Luhmann, D. Odstrcil,
Case Studies of Interplanetary Coronal Mass Ejections Interplanetary Coronal Mass Ejections – Different Phases of the Cycle Of particular interest to the.
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,
Solar Cycle Trends and Case Studies of Interplanetary Coronal Mass Ejections Interplanetary Coronal Mass Ejections During Different Phases of the Cycle.
The Solar Wind.
The Sun 1 of 200 billion stars in the Milky Way. Our primary source of energy.
Coronal Sources of Impulsive Fe-Rich Solar Energetic Particle Events S. W. Kahler AFRL Space Vehicles Directorate, Kirtland AFB, NM, USA D. V. Reames IPST,
Conclusions Using the Diffusive Equilibrium Mapping Technique we have connected a starting point of a field line on the photosphere with its final location.
Suprathermal Tails in Solar Wind Oxygen and Iron Mark Popecki University of New Hampshire STEREO SWG 11/2007.
ACE Page 1 ACE ACE PresentorInstitution. ACE Page 2 ACE Mass Fractionation in the Composition of Solar Energetic Particles Although it is well known that.
NoRH Observations of Prominence Eruption Masumi Shimojo Nobeyama Solar Radio Observatory NAOJ/NINS 2004/10/28 Nobeyama Symposium SeiSenRyo.
Small-scale transients in the slow solar wind during solar activity minimum K.E.J. Huttunen 1,2, J.G. Luhmann 1, J.T. Gosling 3, Y. Li 1, D. Larson 1,
He + Increase in SEP Events with a High Source Temperature and Implication for Acceleration Site ICRC, 2011, Beijing Z. Guo; E. Moebius; M. Popecki Space.
SHINE SEP Campaign Events: Detailed comparison of active regions AR9906 and AR0069 in the build-up to the SEP events of 21 Apr 2002 and 24 Aug 2002 D.
NoRH Observations of RHESSI Microflares M.R. Kundu, Dept. of Astronomy, University of Maryland, College Park, MD E.J.Schmahl, Dept. of Astronomy, University.
Composition and spectral properties of the 1 AU quiet- time suprathermal ion population during solar cycle23 M Al-Dayeh, M I Desai, J R Dwyer, H K Rassoul,
Analysis of Suprathermal Events Observed by STEREO/PLASTIC with a Focus on Upstream Events STEREO SWG - 20 Meredith, NH October 27-29, 2009 Josh Barry,
Chapter 4 Histograms Stem-and-Leaf Dot Plots Measures of Central Tendency Measures of Variation Measures of Position.
ORIGIN OF THE SLOW SOLAR WIND K. Fujiki , T. Ohmi, M. Kojima, M. Tokumaru Solar-Terrestrial Environment Laboratory, Nagoya University and K. Hakamada Department.
Origins of Solar Minimum CMEs with ICMEs Yan Li 1 B. J. Lynch 1, J. G. Luhmann 1, A. Thernisien 2, A. Vourlidas 2, E. Kilpua 3, L. Jian 4, A. B. Gavin.
16-20 Oct 2005SSPVSE Conference1 Galactic Cosmic Ray Composition, Spectra, and Time Variations Mark E. Wiedenbeck Jet Propulsion Laboratory, California.
SEP Event Onsets: Far Backside Solar Sources and the East-West Hemispheric Asymmetry S. W. Kahler AFRL Space Vehicles Directorate, Kirtland AFB, New Mexico,
Solar Wind Stream Interface Evolution K.D.C. Simunac, L.M. Kistler, A.B. Galvin, M.A. Lee, M.A. Popecki, C. Farrugia, E. Moebius, L.M. Blush, P. Bochsler,
Correlation of magnetic field intensities and solar wind speeds of events observed by ACE. Mathew J. Owens and Peter J. Cargill. Space and Atmospheric.
Introduction to Space Weather Jie Zhang CSI 662 / PHYS 660 Fall, 2009 Copyright © The Heliosphere: Solar Wind Oct. 08, 2009.
Summary Using 21 equatorial CHs during the solar cycle 23 we studied the correlation of SW velocity with the area of EIT CH and the area of NoRH RBP. SW.
Solar Wind Helium Abundance and the Minimum Speed of the Solar Wind
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.
Poster X4.137 Solar Wind Trends in the Current Solar Cycle (STEREO Observations) A.B. Galvin* 1, K.D.C. Simunac 2, C. Farrugia 1 1.Space Science Center,
The Sun. Sun Fact Sheet The Sun is a normal G2 star, one of more than 100 billion stars in our galaxy. Diameter: 1,390,000 km (Earth 12,742 km or nearly.
Carrington Rotation 2106 – Close-up of AR Mr 2106 Bt 2106
Solar Wind Transients and SEPs
Lecture 5 The Formation and Evolution of CIRS
A.B. Galvin*1, K.D.C. Simunac1, M.A. Popecki1, and C.J. Farrugia1
Presentation transcript:

Long Term Measurements of Solar Wind Fe Charge States Mark Popecki, A. Galvin, L. M. Kistler,H. Kucharek, E. Moebius, K. Simunac, P. Bochsler, L. M. Blush, B. Klecker

Solar Wind Fe Charge State Expectations Four types (Schwenn, 2006) –Fast solar wind (coronal holes) –Slow solar wind (near helmet streamers –Slow solar wind (active regions) –ICME solar wind slow > fast ICME QFe ~16+ Small variations in mean charge state compared to SEPs slow fast Von Steiger et al., (2000)

STEREO A Fe Charge States vs. Solar Wind Speed Latter Half of 2008 Q Fe STEREO A solar wind speed/100 (km/s) Limited period of time Solar wind speed is inversely related to Q Fe Examine a longer period, in solar maximum…

Solar Wind QFe from ACE/SWICS Two hour averages of solar wind Fe charge states with a 33 day running average (top) International Monthly Sunspot number (bottom) ICME solar wind may have high Fe charge states (Lepri; Reinard (2005, 2008) Fewer occurrences of high charge state solar wind in The mean Fe charge state decreases in

QFe Histograms: ACE SWICS QFe is reduced by 2 units from 1998 to 2008

from ACE/SWICS and Solar Wind Speed from ACE/SWEPAM Mean ACE Fe charge states: 33 day running averages (top) Solar wind speed from ACE/SWEPAM (bottom) The mean solar wind speed sometimes changes without am inverse change in the mean Fe charge state. QFe S/W speed/100

Iron charge states and solar wind speeds : 2007 (DOY 022) (DOY 230), STEREO A The top trace is the iron charge state, averaged over 2 hour periods. o The average charge states typically ranged between 8+ and 11+. o A prominent exception occurred during the 2007/143 May 23 ICMEs. The average charge state was ~13+ to 14+. The bottom trace is the 2 hour averaged solar wind speed from STEREO A. o An upward trend occurred in the beginning of 2008, maximizing at DOY (early February, 2008). o A long decline below the 2007 levels followed, until August of o Variations in the solar wind speed have decreased compared to early /143 May ICME S/W speed / 100 and

Mean Iron Charge State and Solar Wind Speed: 2007 (DOY 022) (DOY 230), STEREO A The smoothed trendline in the iron charge states is shown in blue (left axis) with the smoothed trendline for the solar wind speed. The iron charge state tends to move in the opposite direction to the solar wind speed in a large scale sense. The charge state has not completely recovered to the early 2007 levels, even though the average solar wind speed has gone lower than it was in QFe S/W speed

Solar Wind Speeds: Recent Solar Min and Max STEREO A: 2007/ /230 ACE: Speeds in the period (solar min) are typically lower than the period (solar max)

Solar Wind Speed vs. Iron Charge State STEREO A The iron charge states are plotted against corresponding solar wind speeds for the period. Variations in charge state are generally related to solar wind speed, but with a broad spread of approximately 1- 2 charge units Solar Wind Speed (STEREO A, km/s)

Iron Charge States for 4 S/W Speed Ranges Histograms of mean iron charge states are plotted for selected intervals of solar wind speed. The average charge state declines particularly over the speed range km/s, then changes little at higher speeds. decreases by ~1 unit over the entire speed range 260 < S/W speed < 310 km/s = < S/W speed < 425 km/s = < S/W speed < 550 km/s = < S/W speed < 750 km/s = 8.6

NSO/GONG synoptic coronal hole plots for selected Carrington rotations –Red/green areas are coronal holes: red negative polarity, green positive polarity –Neutral line is in black Isolated coronal holes disappear with time Polar coronal hole extensions shrink Neutral line flattens (less tilted current sheet) Galvin et al., 2009

Iron Charge States vs. S/W Speed One hour sampling intervals are shown. Transient or ICME intervals are highlighted (Kilpua et al, 2009 a, b) –Small transients: magnetic structures related to sector boundaries in solar wind –ICME list (Jian, 2009) –Additional ICMEs identified by Kilpua 2009b Reinard (2005, 2008) related the Fe charge state to the energetics of the originating solar event such as flare magnitude. No ICMEs occurred with near 16+ Galvin et al. (2009)

Summary ACE/SWICS mean Fe charge states have declined in the declining phase of the previous solar maximum by ~2 units ( ). The decline is partly a result of fewer transient periods of high charge states (fewer ICMEs?) Fe charge states are anticorrelated with solar wind speed over short periods, but they may be poorly correlated in long term averages. The mean STA Fe charge state in the period tends to be higher at low speeds than at high speeds by ~ 1 unit. Variation of the Fe charge state with speed is small above 500 km/s. STEREO A mean Fe charge states have varied inversely with solar wind speed in the period. –Recent Fe charge states are lower for the present low speed regime than they were in –Is this slow solar wind without the high charge state component (~Fe 16+)?

One hour averages of solar wind speed and iron charge state from STEREO A Smoothed lines hour averages (~Carrington rotation)

STEREO A Fe Charge States vs. Solar Wind Speed Average Fe charge state generally shows an anticorrelation with solar wind speed (sources: fast or slow s/w, coronal holes or active region). Typical values of charge state are between 9+ and 10+. Only one period of high charge states exists: May 22-24, 2007 (ICME).