ausblenden:
Schlagwörter:
-
MPINP:
Hochenergie-Astrophysik Theorie - Abteilung Hofmann
Zusammenfassung:
We analyzed the 2.6 mm CO and 21 cm H I lines toward the Magellanic superbubble 30. Doradus. C, in order to reveal the associated molecular and atomic gas. We uncovered five molecular clouds in a velocity range from 251 to 276 km s(-1) toward the western shell. The non-thermal X-rays are clearly enhanced around the molecular clouds on a parsec scale, suggesting possible evidence for magnetic field amplification via shock-cloud interaction. The thermal X-rays are brighter in the eastern shell, where there are no dense molecular or atomic clouds, opposite to. the western shell. The TeV gamma- ray distribution may spatially match the total interstellar proton column density as well as the non-thermal X-rays. If the hadronic gamma-ray is dominant, the total energy of the cosmic-ray protons is at least similar to 1.2 x 10(50) erg with the estimated mean interstellar proton density similar to 60 cm(-3). In addition, the gamma-ray flux associated with the molecular cloud (e.g., MC3) could be detected and resolved by the Cherenkov Telescope Array (CTA). This should permit CTA to probe the diffusion of cosmic-rays into the associated dense ISM.
