1 / 7

Gamma-Rays from Galactic Compact Objects

Gamma-Rays from Galactic Compact Objects. Philip Kaaret, A. Abdo, J. Arons, M. Baring, S. Funk, A. Harding, S. Heinz, E. Hays, B. Gaensler, D. Kieda, M. Pohl, K. Ragan, P. Slane, D. Torres. Outline: TeV sky Plerions = pulsar wind nebulae Jets from compact objects. TeV sky (in 2006).

lisbet
Télécharger la présentation

Gamma-Rays from Galactic Compact Objects

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Gamma-Rays from Galactic Compact Objects Philip Kaaret,A. Abdo, J. Arons, M. Baring, S. Funk, A. Harding, S. Heinz, E. Hays, B. Gaensler, D. Kieda, M. Pohl, K. Ragan, P. Slane, D. Torres • Outline: • TeV sky • Plerions = pulsar wind nebulae • Jets from compact objects

  2. TeV sky (in 2006) 29 discovered since 2003 27 are Galactic 39 sources (E > 100 GeV) 39 sources (E > 100 GeV) (Hermann 2006)

  3. Pulsar Wind Nebula Relativistic wind from pulsar terminates in shock accelerating particles to ~ 1000 TeV. • Local laboratory for studying relativistic shocks • Results important for our understanding of relativistic shocks and for applications to other systems such as AGN and GRB

  4. TeV Observations of PWNe • What does shock acceleration work? (maximum energy, efficiency, dependence on particle content) • Hadron acceleration? (older PWNe?) • How do relativistic particles diffuse? • Discover new PWNe (Aharonian et al. 2006) (Atoyan & Aharonian et al. 1996)

  5. Compact objects in binaries

  6. TeV Observations of BH Jets • For 10% acceleration efficiency, jet kinetic power = X-ray luminosity. • Gamma-rays should enable us to determine if jet is e+e- or hadronic. • Future observatory could detect TeV emission from quiescent BHs. (Aharonian et al. 2005) Leptonic model of LS 5039 (Dermer & Bottcher 2006)

  7. Conclusions • New TeV observatories will lead to significant advances in our understanding of relativistic particle acceleration by neutron stars and black holes with important applications to many areas of astrophysics. • Gamma-ray data is essential to understand the physics of pulsar wind nebulae and jet acceleration in binary systems. • A Galactic plane survey to 10-14 erg cm-2 s-1 would discover hundreds of new Galactic sources including PWNe, young pulsars, millisecond pulsars, quiescent black hole and neutron star binaries, new classes of objects…

More Related