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In order to enable an iCal export link, your account needs to have a key created. This key enables other applications to access data from within Indico even when you are neither using nor logged into the Indico system yourself with the link provided. Once created, you can manage your key at any time by going to 'My Profile' and looking under the tab entitled 'HTTP API'. Further information about HTTP API keys can be found in the Indico documentation.
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In conjunction with a having a key associated with your account, to have the possibility of exporting private event information necessitates the creation of a persistent key. This new key is also associated with your account and whilst it is active the data which can be obtained through using this key can be obtained by anyone in possession of the link provided. Due to this reason, it is extremely important that you keep links generated with this key private and for your use only. If you think someone else may have acquired access to a link using this key in the future, you must immediately remove it from 'My Profile' under the 'HTTP API' tab and generate a new key before regenerating iCalendar links.
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We consider a generalized statistical model for the production process of cosmic
rays. This model takes into account temperature distribution of sources and yields
Tsallis statistics for cosmic ray energy spectrum. Results are compared with the
experimental data.
Presented by Dr. Zbigniew WLODARCZYK
on
5/7/2007
at
15:30
Gamma rays have long been recognized as a uniquely powerful probe of the existence, origin, and nature of cosmic
rays beyond the solar system. The unprecedented sensitivity and resolution of GLAST should for the first time
confirm the presence of cosmic rays in Local Group galaxies today, and in all galaxies throughout the history of
cosmic star formation. We show that GLAST should detect,
... More
Presented by Prof. Brian FIELDS
on
5/7/2007
at
15:42
Based on the cosmic-ray (CR) data currently available, we estimate the gas
density, diffusion coefficient, and their spacial gradient in both the longitudinal
and the latitudinal directions in the Galaxy. Applying our model on the three
dimensional CR propagation for various CR observables such as stable nuclear
components, isotopes, antiprotons, diffuse gamma-rays, we present analytical
... More
Presented by Prof. Toru SHIBATA
on
5/7/2007
at
16:30
We report on a project to constrain the large-scale and turbulent magnetic fields of
the Milky Way galaxy, which eventually will incorporate all of the relevant
observational data. The initial work is based primarily on the WMAP3 polarization
and intensity maps, plus a large number of galactic and extragalact point source
Faraday Rotation Measures. Preliminary results on the Galactic magneti
... More
Presented by Mr. Ronnie JANSSON
on
5/7/2007
at
16:18
We present a Monte-Carlo calculation of the propagation of cosmic ray protons in the
Galaxy for energies above 1 PeV. We discuss the relative strengths of competing
effects such as parallel/perpendicular diffusion and drifts in toy models of the
Galaxy. We compare our estimates with the results of the MC calculation for the toy
models and then we apply the MC calculation to a few realistic mod
... More
Presented by Dr. Daniel DE MARCO
on
5/7/2007
at
15:54
The long-duration balloon flights of TRACER have provided new measurements of the
intensities and energy spectra of the arriving cosmic-ray nuclei with 5 ≤ Z ≤ 26 at
high energies. In order to determine the particle composition and energy spectra at
the cosmic-ray sources, changes occurring during the interstellar propagation of
cosmic rays must be known. We use a simple propagation mode
... More
Presented by Dr. Patrick BOYLE
on
5/7/2007
at
16:06
Diffuse VHE γ radiation from the Galactic center ridge observed by the H.E.S.S.
telescope has been convincingly linked with the propagation of recently accelerated
cosmic rays that interact with molecular hydrogen clouds during their diffusion.
Through a series of time-dependent simulations of that diffusion for different
propagation parameters we have obtained the most probable values of the
... More
Presented by Mr. Stavros DIMITRAKOUDIS
on
5/7/2007
at
16:42
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