~130 Years of Solar Wind Data: The Floor and More

Slides:



Advertisements
Similar presentations
EMMREM Predicted Dose Rates for CRaTER N. Schwadron, L. Townsend, K. Kozarev, H. Spence, M. Golightly et al.
Advertisements

An analysis of long-term variations of Sq and geomagnetic activity. Relevance in data reduction for crustal and main field studies Crisan Demetrescu, Venera.
2011/08/ ILWS Science Workshop1 Solar cycle prediction using dynamos and its implication for the solar cycle Jie Jiang National Astronomical Observatories,
An overview of the cycle variations in the solar corona Louise Harra UCL Department of Space and Climate Physics Mullard Space Science.
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,
1 Comments on Leif Svalgaard Journal Club Discussion Stanford University Wed. 19 Feb
An Analysis of Heliospheric Magnetic Field Flux Based on Sunspot Number from 1750 to Today and Prediction for the Coming Solar Minimum Introduction The.
Centennial Variations of Near-Earth IMF and Solar Wind Speed 09:50, Friday November 21 auditorium Reine Elisabeth Session: 14 Space Climate Time allowed.
On the high frequency ingredients of the secular variation C. Demetrescu, V. Dobrica, I. Vaduva Institute of Geodynamics, Bucharest, Romania
1 Reconciling Group and International Sunspot Numbers Leif Svalgaard, HEPL, Stanford University Edward W. Cliver, Space Vehicles Directorate, AFRL XII.
Swedish Institute of Space Physics, Kiruna Variable Sun-Earth energy coupling: dependence on solar cycle strength M. Yamauchi
The Independency of Stellar Mass-Loss Rates on Stellar X-ray Luminosity and Activity Space Telescope Science Institute – 2012.
Reviewing the Summer School Solar Labs Nicholas Gross.
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 SPACE WEATHER EFFECTS ON SATELLITE DRAG 6 January 2006 Cheryl Huang, Frank A. Marcos and William Burke Space Vehicles Directorate Air Force Research.
Extreme Space Weather Events th June 2014 The Maunder minimum: An extreme space climate event? Mathew Owens, Mike Lockwood,
1 WSA Model and Forecasts Nick Arge Space Vehicles Directorate Air Force Research Laboratory.
Center for Space Environment Modeling W. Manchester 1, I. Roussev, I.V. Sokolov 1, 1 University of Michigan AGU Berkeley March.
Periodicities of the Solar Wind, Global Electron Power, and Other Indices in 2005 in HSS Barbara A. Emery (NCAR), Ian G. Richardson (GSFC), David S. Evans.
Polar Network Index as a magnetic proxy for the solar cycle studies Priyal, Muthu, Karak, Bidya Binay, Munoz-Jaramillo, Andres, Ravindra, B., Choudhuri,
Prediction on Time-Scales of Years to Decades Discussion Group A.
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.
What coronal parameters determine solar wind speed? M. Kojima, M. Tokumaru, K. Fujiki, H. Itoh and T. Murakami Solar-Terrestrial Environment Laboratory,
Mervyn Freeman British Antarctic Survey
1 Heliospheric Magnetic Field Leif Svalgaard Stanford University, CA
1 C. “Nick” Arge Space Vehicles Directorate/Air Force Research Laboratory SHINE Workshop Aug. 2, 2007 Comparing the Observed and Modeled Global Heliospheric.
Evolution of the 2012 July 12 CME from the Sun to the Earth: Data- Constrained Three-Dimensional MHD Simulations F. Shen 1, C. Shen 2, J. Zhang 3, P. Hess.
The Unprecedented Solar Magnetic Fields and Their Implications December 21, 2009 Yu Yi Dept. of Astronomy & Space Science, Chungnam National University.
The day after solar cycle 23 IHY 2009 September 23, 2009 Yu Yi 1 and Su Yeon Oh 2 1 Dept. of Astronomy & Space Science, Chungnam National University, Korea.
9 May MESSENGER First Flyby Magnetospheric Results J. A. Slavin and the MESSENGER Team BepiColombo SERENA Team Meeting Santa Fe, New Mexico 11 May.
AFRL/CISM Collaborations
Statistical properties of southward IMF and its geomagnetic effectiveness X. Zhang, M. B. Moldwin Department of Atmospheric, Oceanic, and Space Sciences,
N. A. Schwadron U. New Hampshire Solar Wind and Coronal Electron Temperature in the Protracted Solar Minimum, the Cycle 24 Mini Maximum, and Over Centuries.
Forecast of Geomagnetic Storm based on CME and IP condition R.-S. Kim 1, K.-S. Cho 2, Y.-J. Moon 3, Yu Yi 1, K.-H. Kim 3 1 Chungnam National University.
Evolution of Magnetic Fields from the Sun’s Surface to the Heliopause of one Solar Cycle Nathan Schwadron, Boston University.
Solar Cycle Variation of the Heliospheric Magnetic Flux, Solar Wind Flux and Galactic Cosmic Rays Charles W. Smith, Nathan A. Schwadron Ken G. McCracken,
1 Reconstruction of Heliospheric Magnetic Field Strength Years of HMF B Leif Svalgaard Stanford University LWS Session S-16 (1a) Portland,
17th Cluster workshop Uppsala, Sweden , May 12-15, 2009
CME Propagation CSI 769 / ASTR 769 Lect. 11, April 10 Spring 2008.
ORIGIN OF THE SLOW SOLAR WIND K. Fujiki , T. Ohmi, M. Kojima, M. Tokumaru Solar-Terrestrial Environment Laboratory, Nagoya University and K. Hakamada Department.
WSM Whole Sun Month Sarah Gibson If the Sun is so quiet, why is the Earth still ringing?
Mike Lockwood (Southampton University & Space Science and Technology Department, STFC/Rutherford Appleton Laboratory ) Open solar flux and irradiance during.
1 ~130 Years of Solar Wind Data: The Floor and More E.W. Cliver Space Vehicles Directorate Air Force Research Laboratory AGU May 2008.
1 The Solar Wind - Magnetosphere Coupling Function and Nowcasting of Geomagnetic Activity Leif Svalgaard Stanford University AMS-93, Austin, Jan
Validation/Reconstruction of the Sunspot Number Record, E.W. Cliver Air Force Research Laboratory, Space Vehicles Directorate, Hanscom AFB, MA.
Swedish Institute of Space Physics, Kiruna M. Yamauchi 1 Different Sun-Earth energy coupling between different solar cycles Acknowledgement:
What the Long-Term Sunspot Record Tells Us About Space Climate David H. Hathaway NASA/MSFC National Space Science and Technology Center Huntsville, AL,
Diary of a Wimpy Cycle David H. Hathaway 1 and Lisa Upton 2,3 1 NASA/Marshall Space Flight Center/Science Research Office 2 Vanderbilt University 3 University.
SOHO/ESA/NASA Solar cycle - modeling and predicting Petri Käpylä NORDITA AlbaNova University Center Stockholm, Sweden Stockholm, 2nd Feb 2007 SST NASA.
Using the paleo-cosmic ray record to compare the solar activity during the sunspot minimum of with those during the Spoerer, Maunder, and Dalton.
Time-Dependence (structuring) of the Alpha-to-Proton Ratio (A He ) in the Solar Wind at 1 AU: Initial results, Implications, and Speculations Harlan E.
Nicholeen Viall NASA/GSFC
The Olsen Rotating Dipole Revisited
The Decline to Solar Minimum 2014 through about 2020
Lecture 12 The Importance of Accurate Solar Wind Measurements
Search for Cosmic Ray Anisotropy with the Alpha Magnetic Spectrometer on the International Space Station G. LA VACCA University of Milano-Bicocca.
HMI-WSO Solar Polar Fields and Nobeyama 17 GHz Emission
Disturbance Dynamo Effects in the Low Latitude Ionosphere
Introduction to Space Weather Interplanetary Transients
Estimates of the forthcoming solar cycles 24 and 25
Geomagnetic activity indicates large amplitude for sunspot cycle 24
Solar cycle variation of the heliospheric magnetic field
Variable Sun-Earth energy coupling: dependence on solar cycle strength
Effects of Dipole Tilt Angle on Geomagnetic Activities
Yama's works Using geomagnetic data
Rick Leske, A. C. Cummings, R. A. Mewaldt, and E. C. Stone
Yuki Takagi1*, Kazuo Shiokawa1, Yuichi Otsuka1, and Martin Connors2  
Using Old Geomagnetic Data to Say Something about the Sun
The properties of CMEs embedded in extreme solar wind
Introduction to Space Weather
Presentation transcript:

~130 Years of Solar Wind Data: The Floor and More E.W. Cliver Space Vehicles Directorate Air Force Research Laboratory AGU 27-30 May 2008

Outline Long-term solar wind reconstruction: Emerging consensus Floor in the IMF: Then & Now Secular variation of solar wind speed Entering a Gleissberg Minimum?

Long-term Solar Wind Magnetic Field Reconstruction: 2 2 2005 1 3 4 1 5 Br = 0.56Btot Long-term Solar Wind Magnetic Field Reconstruction: Emerging Consensus

(Svalgaard & Cliver, JGR, 110(12), 2005) The IDV index has the useful property of being highly correlated with B and independent of V

Long-term Solar Wind Magnetic Field Reconstruction: 2 4 3 2 2005 1 3 5 4 2 1 5 Long-term Solar Wind Magnetic Field Reconstruction: Emerging Consensus (Exception: McCracken, 2007)

- Annual averages of B show evidence for a floor ~ 4.5 nT - The sharp drop from 1945-1950 in the McCracken time series does not appear in geomagnetic data - The low value in 1901 from RL&F is in error (APR, priv. comm.)

Floor in the Solar Wind Magnetic Field: Direct Observations (27-Day Averages)

Floor in the Solar Wind Magnetic Field: Recent Direct Observations Last 13 rotations similar to 1901, 1902, 1913 Floor in the Solar Wind Magnetic Field: Recent Direct Observations

Floor in the Solar Wind Magnetic Field: Cosmogenic Nuclei / long-term (Muscheler et al., 2005) (Caballero-Lopez et al., 2004) Since SSN ~ 0 during MM, would expect B to be at floor level. Direct from C-L (parameterized). For M, modulation parameter vs. IDV-based B; IDV-based B vs. SSN Floor in the Solar Wind Magnetic Field: Cosmogenic Nuclei / long-term

Interpretation of Floor: Baseline Open Magnetic Flux SSW + HSS + CME º SSW + HSS * SSW B (nT) M ~250 μT M 245 μT M 200 μT M 115 μT (Fisk et al., 1999; Owens & Crooker, 2006) Year Interpretation of Floor: Baseline Open Magnetic Flux

Svalgaard & Cliver, ApJ Lett. 661, L203, 2007 B(nT) = 0.27R½ + 4.6 For SSN = 0 Then: B Total (ecliptic) = 4.6 nT; B RADIAL (all latitudes) = 3.0 nT Now: B Total (ecliptic) ~ 4 nT; B RADIAL (all latitudes) ~ 2 nT

~15% increase in solar wind speed during the last ~120 years Floor (Rouillard et al., 2007; Svalgaard & Cliver, 2007) ~15% increase in solar wind speed during the last ~120 years

Plea for Help to Magnetospheric Physicists Open Question: Effect of ~10% decrease of Earth’s dipole since ~1850 on geomagnetic activity? - Siscoe et al. (2002)  Decrease in activity (ISM model & Hill M/I coupling models) - Glassmeier et al. (2004)  Weak/no effect (scaling relationships between magnetospheric parameters & M)

A Coming Gleissberg Minimum? Cycle 24 may be smallest in ~100 years Test of Long-term Reconstructions, Precursor Prediction Technique, Dynamo Models, … 164.5 158.5 120.8 75? (Svalgaard, Cliver, & Kamide, 2005)

Conclusions Consensus long-term B & V / Validation of IDV Floor in IMF in ecliptic Btot ~4 nT & Br ~ 2 nT (SSN = 0) ~15% increase in solar wind V since 1872?