Artículo
High-energy flares from jet-clump interactions
Fecha de publicación:
05/2010
Editorial:
Astronomical Society of the Pacific
Revista:
ASP Conference Series
ISSN:
0004-6280
Idioma:
Inglés
Tipo de recurso:
Artículo publicado
Clasificación temática:
Resumen
High-mass microquasars are binary systems composed by a massive star and a compact object from which relativistic jets are launched. Regarding the companion star, observational evidence supports the idea that winds of hot stars are formed by clumps. Then, these inhomogeneities may interact with the jets producing a flaring activity. In the present contribution we study the interaction between a jet and a clump of the stellar wind in a high-mass microquasar. This interaction produces a shock in the jet, where particles may be accelerated up to relativistic energies. We calculate the spectral energy distributions of the dominant non-thermal processes: synchrotron radiation, inverse Compton scattering, and proton-proton collisions. Significant levels of X- and γ-ray emission are predicted, with luminosities in the different domains up to ∼1034–1035 erg s-1 on a timescale of about ∼1 h. Finally, jet-clump interactions in high-mass microquasars could be detectable at high energies. These phenomena may be behind the fast TeV variability found in some high-mass X-ray binary systems, such as Cygnus X-1, LS 5039 and LS I+61 303. In addition, our model can help to derive information on the properties of jets and clumpy winds.
Palabras clave:
Flares
,
Microquasars
,
Binary Systems
Archivos asociados
Licencia
Identificadores
Colecciones
Articulos(CCT - LA PLATA)
Articulos de CTRO.CIENTIFICO TECNOL.CONICET - LA PLATA
Articulos de CTRO.CIENTIFICO TECNOL.CONICET - LA PLATA
Articulos(IAR)
Articulos de INST.ARG.DE RADIOASTRONOMIA (I)
Articulos de INST.ARG.DE RADIOASTRONOMIA (I)
Citación
Araudo, Anabella Teresa; Bosch Ramon, Valenti; Romero, Gustavo Esteban; High-energy flares from jet-clump interactions; Astronomical Society of the Pacific; ASP Conference Series; 422; 5-2010; 32-40
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