'Waxman' presentation slideshows

High energy n & Gravitational wave detectors: New windows on the universe

384 views • 38 slides

High energy neutrino astronomy: Challenges & Prospects

High energy neutrino astronomy: Challenges & Prospects. Eli Waxman Weizmann Institute, ISRAEL. High energy n ’ s: A new window. MeV n detectors: Solar & SN1987A n ’ s Stellar physics (Sun ’ s core, SNe core collapse) n physics >0.1 TeV n detectors:

416 views • 31 slides

What do we know about the identity of CR sources?

What do we know about the identity of CR sources?. Boaz Katz, Kfir Blum Eli Waxman Weizmann Institute, ISRAEL. The cosmic-ray spectrum & Composition. log [dJ/dE]. E -2.7. Galactic. Protons. E -3. Source: Supernovae(?). X-Galactic (?). Heavy Nuclei. Source?. Light Nuclei?. Lighter.

409 views • 28 slides

What do we know about the identity of CR sources?

What do we know about the identity of CR sources?. Boaz Katz, Kfir Blum Eli Waxman Weizmann Institute, ISRAEL. The cosmic-ray spectrum & Composition. log [dJ/dE]. E -2.7. Galactic. Protons. E -3. Source: Supernovae(?). X-Galactic (?). Heavy Nuclei. Source?. Light Nuclei?. Lighter.

283 views • 28 slides

UHECRs & GRBs

UHECRs & GRBs. Eli Waxman Weizmann Institute, ISRAEL. The acceleration challenge. v. R. /G. B. v. 2R. G 2. G 2. l =R/ G. (d t RF =R/ G c). [Hillas, ARA&A (1984); Waxman 04]. The suspects. Active Galactic Nuclei (steady): G ~ few requires L>10 47 erg/s Few, brightest AGN

269 views • 18 slides