Gamma-ray emission from massive star forming regions

Recent radio observations support a picture for star formation where there is accretion of matter onto a central protostar with the ejection of molecular outflows that can affect the surrounding medium. The impact of a supersonic outflow on the ambient gas can produce a strong shock that could accel...

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Detalles Bibliográficos
Autores principales: Araudo, Anabella Teresa, Romero, Gustavo Esteban, Bosch-Ramon, Valentí, Paredes, J. M.
Formato: Articulo Preprint
Lenguaje:Inglés
Publicado: 2008
Materias:
Astronomía
Gamma-ray emission
Massive stars: formation
Radiation mechanisms: non-thermal
Acceso en línea:http://sedici.unlp.edu.ar/handle/10915/127373
Aporte de:
SEDICI (UNLP) de Universidad Nacional de La Plata
id I19-R120-10915-127373
record_format dspace
institution Universidad Nacional de La Plata
institution_str I-19
repository_str R-120
collection SEDICI (UNLP)
language Inglés
topic Astronomía
Gamma-ray emission
Massive stars: formation
Radiation mechanisms: non-thermal
spellingShingle Astronomía
Gamma-ray emission
Massive stars: formation
Radiation mechanisms: non-thermal
Araudo, Anabella Teresa
Romero, Gustavo Esteban
Bosch-Ramon, Valentí
Paredes, J. M.
Gamma-ray emission from massive star forming regions
topic_facet Astronomía
Gamma-ray emission
Massive stars: formation
Radiation mechanisms: non-thermal
description Recent radio observations support a picture for star formation where there is accretion of matter onto a central protostar with the ejection of molecular outflows that can affect the surrounding medium. The impact of a supersonic outflow on the ambient gas can produce a strong shock that could accelerate particles up to relativistic energies. A strong evidence of this has been the detection of non-thermal radio emission coming from the jet termination region of some young massive stars. In the present contribution, we study the possible high-energy emission due to the interaction of relativistic particles, electrons and protons, with the magnetic, photon and matter fields inside a giant molecular cloud. Electrons lose energy via relativistic Bremsstrahlung, synchrotron radiation and inverse Compton interactions, and protons cool mainly through inelastic collisions with atoms in the cloud. We conclude that some massive young stellar objects might be detectable at gamma-rays by next generation instruments, both satellite-borne and ground based.
format Articulo
Preprint
author Araudo, Anabella Teresa
Romero, Gustavo Esteban
Bosch-Ramon, Valentí
Paredes, J. M.
author_facet Araudo, Anabella Teresa
Romero, Gustavo Esteban
Bosch-Ramon, Valentí
Paredes, J. M.
author_sort Araudo, Anabella Teresa
title Gamma-ray emission from massive star forming regions
title_short Gamma-ray emission from massive star forming regions
title_full Gamma-ray emission from massive star forming regions
title_fullStr Gamma-ray emission from massive star forming regions
title_full_unstemmed Gamma-ray emission from massive star forming regions
title_sort gamma-ray emission from massive star forming regions
publishDate 2008
url http://sedici.unlp.edu.ar/handle/10915/127373
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AT romerogustavoesteban gammarayemissionfrommassivestarformingregions
AT boschramonvalenti gammarayemissionfrommassivestarformingregions
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bdutipo_str Repositorios
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