English   español  
Por favor, use este identificador para citar o enlazar a este item: http://hdl.handle.net/10261/20440
Compartir / Impacto:
Estadísticas
Add this article to your Mendeley library MendeleyBASE
Citado 61 veces en Web of Knowledge®  |  Ver citas en Google académico
Visualizar otros formatos: MARC | Dublin Core | RDF | ORE | MODS | METS | DIDL
Título

Spectral evolution of superluminal components in parsec-scale jets

AutorMimica, Petar; Aloy, Miguel Ángel; Agudo, Iván ; Martí, José M.; Gómez Fernández, J. L. ; Miralles, Juan Antonio
Palabras claveGalaxies: jets
Hydrodynamics
Radiation mechanisms: non-thermal
Relativity
Fecha de publicaciónabr-2009
EditorAmerican Astronomical Society
CitaciónAstrophysical Journal 696(2): 1142-1163 (2009)
ResumenWe present numerical simulations of the spectral evolution and emission of radio components in relativistic jets. We have developed an algorithm (SPEV) for the transport of a population of non-thermal electrons including radiative losses. For large values of the ratio of gas pressure to magnetic field energy density, \ab \sim 6\times 10^4, quiescent jet models show substantial spectral evolution, with observational consequences only above radio frequencies. Larger values of the magnetic field (\ab \sim 6\times 10^2), such that synchrotron losses are moderately important at radio frequencies, present a larger ratio of shocked-to-unshocked regions brightness than the models without radiative losses, despite the fact that they correspond to the same underlying hydrodynamic structure. We also show that jets with a positive photon spectral index result if the lower limit \gamma_min of the non-thermal particle energy distribution is large enough. A temporary increase of the Lorentz factor at the jet inlet produces a traveling perturbation that appears in the synthetic maps as a superluminal component. We show that trailing components can be originated not only in pressure matched jets, but also in over-pressured ones, where the existence of recollimation shocks does not allow for a direct identification of such features as Kelvin-Helmholtz modes, and its observational imprint depends on the observing frequency. If the magnetic field is large (\ab \sim 6\times 10^2), the spectral index in the rarefaction trailing the traveling perturbation does not change much with respect to the same model without any hydrodynamic perturbation. If the synchrotron losses are considered the spectral index displays a smaller value than in the corresponding region of the quiescent jet model.
Descripción27 pages, 18 figures, 1 table, 1 appendix.-- Pre-print archive.
Versión del editorhttp://dx.doi.org/10.1088/0004-637X/696/2/1142
URIhttp://hdl.handle.net/10261/20440
DOI10.1088/0004-637X/696/2/1142
ISSN0004-637X
Aparece en las colecciones: (IAA) Artículos
Ficheros en este ítem:
Fichero Descripción Tamaño Formato  
0811.1143v2.pdf2,63 MBAdobe PDFVista previa
Visualizar/Abrir
Mostrar el registro completo
 



NOTA: Los ítems de Digital.CSIC están protegidos por copyright, con todos los derechos reservados, a menos que se indique lo contrario.