'Solar wind velocity' presentation slideshows

Magnetic reconnection in the magnetotail: Geotail observations

992 views • 83 slides

What coronal parameters determine solar wind speed?

What coronal parameters determine solar wind speed?. M. Kojima, M. Tokumaru, K. Fujiki, H. Itoh and T. Murakami Solar-Terrestrial Environment Laboratory, Nagoya University K. Hakamada Department of Natural Science and Mathematics, Chubu University.

498 views • 34 slides

NEAR-EARTH TRAJECTORY OF CME DEDUCED FROM COSMIC RAYS

NEAR-EARTH TRAJECTORY OF CME DEDUCED FROM COSMIC RAYS. K. MUNAKATA , T. Kuwabara, J. W. Bieber, P. Evenson, R. Pyle, S. Yasue, C. Kato, Z. Fujii, M. L. Duldig, J. E. Humble, M. R. Silva, N. B. Trivedi, W. D. Gonzalez, and N. J. Schuch. Prototype network (2001~). Data used.

382 views • 27 slides

T. Ogino and T. Aoyama Solar-Terrestrial Environment Laboratory

387 views • 22 slides

293 views • 19 slides

V. Pilipenko , N. Romanova, M. Engebretson, L. Simms

The Role of ULF wave activity in solar wind-magnetosphere interactions and magnetospheric electron acceleration. V. Pilipenko , N. Romanova, M. Engebretson, L. Simms Institute of the Physics of the Earth, Moscow Augsburg College , Minneapolis. Construction of the ULF wave indices.

333 views • 18 slides

The Gulmarg Neutron Monitor

The Gulmarg Neutron Monitor. Ramesh Koul Astrophysical Sciences Division Bhabha Atomic Research Centre Mumbai 400 085. NM configurations. # IGY 1957/58 eff. ~ 1.9% # NM64 1964 eff. ~ 5.7% # He3 based # Gd doped liquid scintillator. Gulmarg Neutron Monitor (GNM).

339 views • 17 slides

Modeling the Magnetosphere

Samantha Sanders Code 674 Dr. David G. Sibeck NASA Goddard Space Flight Center. Modeling the Magnetosphere. Interplanetary magnetic field (IMF) How do the forces within it affect space weather?. What are we modeling?. What are we modeling?. y. EARTH. z. Velocity of solar wind. x.

284 views • 14 slides

How does the magnetic structure of the Sun lead to stream interaction regions (SIRs)?

Diagnostics of Solar Wind Processes Using the Total Perpendicular Pressure Lan Jian, C. T. Russell, and J. T. Gosling. How does the magnetic structure of the Sun lead to stream interaction regions (SIRs)? What are interplanetary coronal mass ejections (ICMEs)?

283 views • 11 slides

model (1)

228 views • 11 slides

Three results

Model constraints and identifying nonlinear SW/M-I coupling effects Bob Weigel George Mason University. Three results. Conclusion: Detecting nonlinearities and coupling response effects is often complicated by model limitations. Estimation of solar wind/magnetosphere coupling function

195 views • 7 slides

Potential Model

High-Latitude Input Options in tiegcm1.92_r296. Potential Model. Default. Heelis. Weimer05. User Specified. IMF Data. User Specified. GPI Data. Namelist Input: bx,by,bz swden,swvel. Namelist Input: Kp. Namelist Input: power,ctpoten. bx,by,bz swden,swvel. Kp. Power= f(Kp)

131 views • 3 slides

V. Belov 1 , E. A. Eroshenko 1 , H. Mavromichalaki 2 , V.A. Oleneva 1 ,

Aug. 2005 Sept. 2005. 20 th ECRS, 5-8 September 2006, Lisboa Portugal. Cosmic ray modulation in August-September 2005. V. Belov 1 , E. A. Eroshenko 1 , H. Mavromichalaki 2 , V.A. Oleneva 1 , A. Papaioannou 2 , G. Mariatos 2 , V. G. Yanke 1

143 views • 1 slides

Empirical Solar Wind Forecasting from the Chromosphere: Inclusion of a Potential Field Corona R.J. Leamon, 1 S.W. McIntosh 2 1 ADNET Systems, Inc. at NASA GSFC, Greenbelt MD; 2 Southwest Research Institute, Boulder, CO. TT. V SW.

75 views • 1 slides

Empirical Solar Wind Forecasting from the Chromosphere: Inclusion of a Potential Field Corona R.J. Leamon, 1 S.W. McIntosh 2 1 ADNET Systems, Inc. at NASA GSFC, Greenbelt MD; 2 Southwest Research Institute, Boulder, CO. TT. V SW.

80 views • 1 slides