'Solar maximum' diaporamas de présentation

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Motivation Coronal signatures Scaling Introducing memory Heavy-tails Summary

Motivation Coronal signatures Scaling Introducing memory Heavy-tails Summary. Motivation Coronal signatures Scaling Introducing memory Heavy-tails Summary. the solar wind. Motivation Coronal signatures Scaling Introducing memory Heavy-tails Summary.

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Department of Astronomy, Nanjing University, Nanjing 210093, China

Possible collaboration between Solar-B and the facilities of Nanjing University. C. Fang, M. D. Ding, P. F. Chen. Department of Astronomy, Nanjing University, Nanjing 210093, China. Outline. Observation History in Nanjing University Introduction to the New Telescope

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The Influence of Solar Variability on the Atmosphere and Ocean Dynamics

The Influence of Solar Variability on the Atmosphere and Ocean Dynamics. Speaker ? Pei-Yu Chueh Adviser ? Yu- Heng Tseng Date ? 2010/10/12. Review. Observation- Solar variability.

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Reading

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Balloon Measurements of Charge Sign Dependent Solar Modulation

Balloon Measurements of Charge Sign Dependent Solar Modulation. Paul Evenson John Clem University of Delaware. 1912: Discovery of Cosmic Rays. As his balloon ascended to 5300m, Viktor Hess observed the rate of discharge of his electroscope increase with altitude.

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The Polar Fields Seen in 17 GHz Microwave Flux

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Solar Wind Helium Abundance and the Minimum Speed of the Solar Wind

Solar Wind Helium Abundance and the Minimum Speed of the Solar Wind. Justin C. Kasper 1 and Michael L. Stevens 2 1 Harvard Smithsonian Center for Astrophysics 2 Boston University. 07 June 2007. Question. We have an abundance of information about thermal H, He++ in the ecliptic at 1 AU.

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Long Term Measurements of Solar Wind Fe Charge States

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. slow. fast. Von Steiger et al., (2000). Solar Wind Fe Charge State Expectations. Four types (Schwenn, 2006)

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PHOEBUS* on LISA: A Proposal for Solar Physics on LISA

PHOEBUS* on LISA: A Proposal for Solar Physics on LISA. INFN-SPAZIO/2 Riunione sulle prospettive della Fisica Astroparticellare nello spazio LNF, 16 Febbraio 2005. Catia Grimani 1 & Helios Vocca 2 (1) Urbino University and INFN Florence (2) University and INFN Perugia.

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Propagation Trends 2013-2014

Propagation Trends 2013-2014. Solar Maximum ! A Double Peaked Sunspot Cycle ?. Every 6 Meter DXer Remembers This! The Second Sunspot Peak of Solar Cycle 23. 400 Years of Sunspot Observations 60 years of high sunspot cycles have probably come to an end. 40 years. 70 years.

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Propagation Trends 2013-2014

Propagation Trends 2013-2014. Solar Maximum ! A Double Peaked Sunspot Cycle ?. Every 6 Meter DXer Remembers This! The Second Sunspot Peak of Solar Cycle 23. 400 Years of Sunspot Observations 60 years of high sunspot cycles have probably come to an end. 40 years. 70 years.

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SOLAR FLARES AND ERUPTIONS

SOLAR FLARES AND ERUPTIONS. Lyndsay Fletcher University of Glasgow. Sunspots - hotbeds of solar activity. Solar minimum, solar maximum. An active region seen by Hinode. Winding up the magnetic field. Gas at the solar equator has a higher speed than that at the poles.

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Mark Wiedenbeck, JPL/Caltech with contributions from STEREO/LET, SEPT and SIT

A Search for 3 He-rich Solar Energetic Particle Events at Solar Minimum using the STEREO/LET Instruments. Mark Wiedenbeck, JPL/Caltech with contributions from STEREO/LET, SEPT and SIT and from ACE/SIS, ULEIS and EPAM. Rate of Occurrence of 3 He-rich SEP Events over the Solar Cycle

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Science Nugget from NAG5-10850 : Superposed Epoch Analysis of Ring Current Geoeffectiveness

Science Nugget from NAG5-10850 : Superposed Epoch Analysis of Ring Current Geoeffectiveness. PI: Michael Liemohn Institution: University of Michigan Key Personnel: Jichun Zhang, U-M grad student Michelle Thomsen, LANL. Intense Storms vs. Moderate Storms @ Solar Maximum. Comparison.

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The slow rise of Cycle 24 as seen in Fe XIV

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