3-11 July 2007
Merida, Mexico
Mexico/General timezone
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SH 3.4, SH 3.5

Place

Location: Merida, Mexico
Room: Yucatan I (Fiesta Americana)
Date: 10 Jul 08:30 - 10:00

Conveners

    • Dr. Kota, Jozsef (University of Arizona)

Timetable | Contribution List

Displaying 7 contributions out of 7
Type: Oral Session: SH 3.4, SH 3.5
Track: SH.3.4
The propagation of galactic and solar cosmic rays in the solar wind (SW) can be strongly influenced by the SW fluctuations properties. Magnetohydrodynamic (MHD) scale fluctuations in the solar wind are usually highly anisotropic, and have also been found to exhibit different properties in regions of high and low solar wind speed. We analyze here the anisotropy properties of the solar wind f ... More
Presented by Dr. Sergio DASSO on 10/7/2007 at 14:18
Type: Oral Session: SH 3.4, SH 3.5
Track: SH.3.5
Energetic heavy ions with 20 – 200 MeV/n in the radiation belts have been observed by Heavy Ion Telescope (HIT) onboard TSUBASA satellite which stayed in the geostationary transfer orbit with the inclination of 28.5 deg. The observed data during quiet period in the outer region of radiation belt found out that the relative abundance for major elements, C, O, Ne, Mg, Si and Fe, were similar t ... More
Presented by Dr. Makoto HAREYAMA on 10/7/2007 at 14:42
Type: Oral Session: SH 3.4, SH 3.5
Track: SH.3.4
We present preliminary results of measuring the direction of the anisotropy vector of cosmic ray intensity. The measurements were made with the Carpet air shower array of the Baksan Neutrino Observatory. The anisotropy vector direction is determined by analyzing the distribution of time delays of the shower signal detected by distant detectors of the array relative to the array’s centr ... More
Presented by Dr. Alexander LIDVANSKY on 10/7/2007 at 13:42
Type: Oral Session: SH 3.4, SH 3.5
Track: SH.3.4
This paper presents the sidereal anisotropy of ~10 TeV galactic cosmic ray (GCR) intensity observed by the Tibet Air Shower experiment. The observed sky- map of the directional anisotropy clearly shows the large-scale feature consisting of excess and deficit of the relative intensity. We note that the observed angular separation between the excess and the deficit is ~120 deg, which is muc ... More
Presented by Prof. M. TAKITA on 10/7/2007 at 13:30
Type: Oral Session: SH 3.4, SH 3.5
Track: SH.3.4
The relative sidereal variation in the arrival direction of primary cosmic ray nuclei of median energy 10 TeV was measured using downward, through-going muons detected with the Super-Kamiokande-I detector. The projection of the anisotropy map onto the right ascension axis has a first harmonic amplitude of (6.64 +/- 0.98 (stat.) +/- 0.55 (syst.)) x 10^-4 and a phase at maximum at (33.2^o +/- ... More
Presented by Dr. Yuichi OYAMA on 10/7/2007 at 13:54
Type: Oral Session: SH 3.4, SH 3.5
Track: SH.3.5
PAMELA was launched on June $15^{th}$ 2006 in a pressurized container on board the Russian Resurs-DK1 satellite. The satellite is flying in high inclination ($70^o$), low Earth Orbit (350-600 km), allowing measurements in various points and conditions of the geomagnetosphere. It is a multi-purpose apparatus composed of a permanent magnet spectrometer to provide particle charge, rig ... More
Presented by Dr. Marco CASOLINO on 10/7/2007 at 14:30
Type: Oral Session: SH 3.4, SH 3.5
Track: SH.3.4
On the basis of world network data of neutron monitors and muon telescopes at the Yakutsk and Nagoya stations the galactic cosmic ray anisotropy directed transverse to the mean field line (in the direction of 15.00 LT) has been revealed. This component undergoes the 11-year variation. Its value rises as the IMF intensity, solar activity level and neutral sheet deformation increase. Such ... More
Presented by Dr. Sardaana GERASIMOVA on 10/7/2007 at 14:06
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