Event calendar file
3-11 July 2007
Merida, Mexico
Mexico/General timezone
- icrc2007@icrc2007.unam.mx
Support
SH 1.6, SH 1.7, SH 2.2, SH 2.3
Place
Location: Merida, Mexico
Room: Yucatan I (Fiesta Americana)
Date:
5 Jul 10:30 - 11:55
Conveners
-
- Dr. Leske, Richard (California Institute of Technology)
Timetable | Contribution List
Displaying 6
contributions
out of
6
We combined solar wind observations from five different spacecraft: Helios 1, Helios
2, IMP-8, Voyager 1 and Voyager 2, from November 1977 to February 1978, to study the
structure of the solar wind streams and the propagation of interplanetary shocks,
interaction regions and ejecta. Comparing the in-situ observations is possible to
illuminate some aspects of these events such as their longitud
... More
Presented by Dr. Gonzalez-Esparza AMERICO
on
5/7/2007
at
16:30
Corotating Interaction Regions are regions in the heliosphere that are formed at the
leading edges of high-speed solar wind streams originating in coronal holes. Their
effects on the propagation of energetic particles are known. Here we concentrate on
the modulation of Jovian electrons by CIRs observed with the Kiel Electron Telescope.
After its launch on Oct. 6, 1990 Ulysses followed an in-ec
... More
Presented by Prof. Bernd HEBER, Mr. R. MÜLLER-MELLIN
on
5/7/2007
at
16:18
It is now well known that Coronal mass Ejection and high Speed solar wind
stream are
the most dynamical features in the interplanetary space. These two
interplanetary features are known as the causes of perturbations in
interplanetary magnetic field. We have identified 95 high speed solar wind
streams events during the period of 1996 to 2002, using the space craft data
near 1 AU. Chr
... More
Presented by Dr. Pankaj Kumar SHRIVASTAVA
Gradual solar energetic particle (SEP) events are believed to be accelerated at CME
driven shocks. Shocks driven by a realistic CMEs are neither simply
quasi-perpendicular nor
quasi-parallel: the geometry and the shock strength may constantly change as the CME
evolves. The shock is likely to be quasi-parallel when it forms and becomes more
parallel at later stages (e.g. Lee and Tylka 2005).
... More
Presented by Dr. Jozsef KOTA
on
5/7/2007
at
15:54
During the period 1996-2005 Intense, Major and Minor Geomagnetic Storms
(GMSs) have been investigated. It is observed that the maximum solar wind
velocity and the maximum decrease in the IMF Bz component are not the
binding conditions for the intensity of the GMSs to occur. It is observed that for
Intense, Major and Minor GMSs the product of solar wind velocity (Vsw) with Bz
min (i.e. Vs
... More
Presented by Dr. Santosh KUMAR, Ms. Simranjit KAUR
The relation between solar particle enhancements near the Earth and solar
flares properties is studied using as a working tool an extensive database of
SXR flares and proton fluxes. This database includes about 63000 SXR flares
observed by GOES satellites and >1200 proton enhancements over period of
time covered 1975-2006. Heliolongitudinal distribution of solar sources of the
most inten
... More
Presented by Dr. Evgenia EROSHENKO
on
5/7/2007
at
15:42
