3-11 July 2007
Merida, Mexico
Mexico/General timezone
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OG 2.3, OG 2.4

Place

Location: Merida, Mexico
Room: Uxmal + Tulum (Holiday Inn)
Date: 6 Jul 12:05 - 13:30

Timetable | Contribution List

Displaying 7 contributions out of 7
Type: Oral Session: OG 2.3, OG 2.4
Track: OG.2.3
A spectacular outburst of VHE (>100 GeV) gamma-ray emission was observed from PKS 2155-304 in 2006 with the H.E.S.S. experiment. The VHE flux reached levels of ~20 times the Crab Nebula flux, more that 2 orders of magnitude above typical values observed from the object. This extremely high flux, when coupled with the sensitivity of H.E.S.S., enables temporal studies of the emission wit ... More
Presented by Dr. Wystan BENBOW on 6/7/2007 at 17:17
Type: Oral Session: OG 2.3, OG 2.4
Track: OG.2.4
Many authors have predicted very high energy (VHE; E > 100 GeV) emission from gamma-ray bursts (GRBs) both during the prompt phase and during the multi-component afterglow. To date however, there has been no definitive detection of such emission. Recently, Swift made the exciting discovery that almost half of GRBs are accompanied by one or more X-ray flares which are found to occur from severa ... More
Presented by Dr. Deirdre HORAN on 6/7/2007 at 17:53
Type: Oral Session: OG 2.3, OG 2.4
Track: OG.2.3
Major blazar flares likely result from injections of relativistic pair plasma into the inner jets. Quantifying the jet’s basic physical parameters has been hampered by the modest sensitivity of past observations, which has allowed only time-averaged pictures of these rapidly changing phenomena. The capabilities of gamma-ray observatories have dramatically improved recently with H.E.S.S. and ... More
Presented by Dr. Jennifer CARSON on 6/7/2007 at 17:29
Type: Oral Session: OG 2.3, OG 2.4
Track: OG.2.3
The MAGIC collaboration has been performing Target of Opportunity (ToO) observations whenever alerted that known or potential very high energy gamma-ray emitting extragalactic sources were in a high flux state in the optical, X-ray band or/and in the TeV energy range. Here we report on triggered observations, results of the analysis, and possible optical-TeV correlation seen in the data. Among ... More
Presented by Mr. Daniel MAZIN on 6/7/2007 at 17:41
Type: Oral Session: OG 2.3, OG 2.4
Track: OG.2.4
The "fireball model" is often invoked to explain the prompt emission from Gamma-Ray Bursts (GRBs) as observed in the MeV energy range. In this standard model, the prompt emission occurs due to collisions between layers within the relativistic jet. We will present the expected synchroton emission from electrons accelerated through the usual Fermi mechanism, assuming that the distribution of ... More
Presented by Sylvain GUIRIEC on 6/7/2007 at 18:05
Type: Oral Session: OG 2.3, OG 2.4
Track: OG.2.4
We examine the prompt and afterglow emission within the context of the Supercritical Pile model for GRBs. For this we have performed self-consistent calculations by solving three time-dependent kinetic equations for protons, electrons and photons in addition to the usual mass and energy conservation equations. We follow the evolution of the RBW as it sweeps up circumstellar matter and assume ... More
Presented by Prof. Apostolos MASTICHIADIS on 6/7/2007 at 18:17
Type: Oral Session: OG 2.3, OG 2.4
Track: OG.2.3
Electromagnetic radiation from blazars can be observed from the radio band up to very high energy gamma rays, with spectral energy distributions (SEDs) apparently characterized by a two-bump structure. So far, most of the measured SEDs could be interpreted using simple leptonic origin scenarios, like Synchrotron Self- Compton models. However, models where the gamma rays are due to accelerated ... More
Presented by Mr. Masaaki HAYASHIDA on 6/7/2007 at 17:05
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