3-11 July 2007
Merida, Mexico
Mexico/General timezone
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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
Type: Oral Session: SH 1.6, SH 1.7, SH 2.2, SH 2.3
Track: SH.2.3
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
Type: Oral Session: SH 1.6, SH 1.7, SH 2.2, SH 2.3
Track: SH.2.2
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
Type: Oral Session: SH 1.6, SH 1.7, SH 2.2, SH 2.3
Track: SH.1.7
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
Type: Oral Session: SH 1.6, SH 1.7, SH 2.2, SH 2.3
Track: SH.1.7
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
Type: Oral Session: SH 1.6, SH 1.7, SH 2.2, SH 2.3
Track: SH.1.6
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
Type: Oral Session: SH 1.6, SH 1.7, SH 2.2, SH 2.3
Track: SH.1.6
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
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