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Gamma-rays from massive stars in Cygnus and Orion

Published online by Cambridge University Press:  26 May 2016

Roland Diehl ,
Karsten Kretschmer ,
Stefan Plüschke ,
Miguel Cerviño  and
Dieter H. Hartmann
Roland Diehl
Affiliation:
Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstraße, D-85741 Garching-bei-Múnchen, BRD
Karsten Kretschmer
Affiliation:
Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstraße, D-85741 Garching-bei-Múnchen, BRD
Stefan Plüschke
Affiliation:
Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstraße, D-85741 Garching-bei-Múnchen, BRD
Miguel Cerviño
Affiliation:
ESA Laboratorio de Astrofísica Espacial y Física Fundamental (INTA), Apdo. 50727, E-28080 Madrid, España Instituto de Astrofísica de Andalucía (CSIC), Camino Bajo de Huétor 24, E-18080 Granada, España
Dieter H. Hartmann
Affiliation:
Department of Physics and Astronomy, Clemson University, Clemson, SC 29634-0978, USA

Abstract

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Radioactive 26Al, ejected by massive stars through winds and supernova explosions, leads to γ-ray line emission that can serve as a probe of the interstellar environment in and near young star clusters. The ~ 1 Myr decay time of 26Al is long enough to allow transport over significant distances, which can cause substantial angular offsets between γ-ray emission and cluster stars. Details of such offsets are determined by the morphology of the ISM. We discuss observations in Cygnus and Orion, and models based on population synthesis methods.

Type
Part 4. Feedback from Massive Stars
Information
Symposium - International Astronomical Union , Volume 212: A Massive Star Odyssey: From Main Sequence to Supernova , 2003 , pp. 706 - 709
Copyright
Copyright © Astronomical Society of the Pacific 2003 

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