Phenomenological description of young massive star clusters

Abstract : The most massive stars appear grouped in giant molecular clouds. Their strong wind activity generates large structures known as super bubbles and induces collective effects which could accelerate particles up to the high energy and produce gamma-rays. The best objects to observe these effects are young massive star clusters in which no supernova explosion has occurred yet. Such star associations are typically still embedded in their parent molecular cloud, which can be traced by the emission due to ionization by the stellar light (HII region). Considering this region as a spherical leaky-box surrounding a central cosmic ray source, a phenomenological model has been developed to estimate cosmic-rays and gamma-rays production for several clusters. The expected gamma-ray flux have been finally compared to the present and future gamma-ray telescopes sensitivities.
Type de document :
Poster
34th International Cosmic Ray Conference (ICRC2015), Jul 2015, The Hague, Netherlands
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http://hal.in2p3.fr/in2p3-01186549
Contributeur : Claudine Bombar <>
Soumis le : mardi 25 août 2015 - 11:20:34
Dernière modification le : jeudi 11 janvier 2018 - 06:13:32

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  • HAL Id : in2p3-01186549, version 1

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G. Lamanna. Phenomenological description of young massive star clusters. 34th International Cosmic Ray Conference (ICRC2015), Jul 2015, The Hague, Netherlands. 〈in2p3-01186549〉

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