Please use this identifier to cite or link to this item: http://hdl.handle.net/10261/20440
Share/Export:
logo share SHARE logo core CORE BASE
Visualizar otros formatos: MARC | Dublin Core | RDF | ORE | MODS | METS | DIDL | DATACITE
Title

Spectral evolution of superluminal components in parsec-scale jets

AuthorsMimica, Petar; Aloy, Miguel Ángel; Agudo, Iván CSIC ORCID ; Martí, José M.; Gómez Fernández, J. L. CSIC ORCID ; Miralles, Juan Antonio
KeywordsGalaxies: jets
Hydrodynamics
Radiation mechanisms: non-thermal
Relativity
Issue DateApr-2009
PublisherAmerican Astronomical Society
CitationAstrophysical Journal 696(2): 1142-1163 (2009)
AbstractWe 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.
Description27 pages, 18 figures, 1 table, 1 appendix.-- Pre-print archive.
Publisher version (URL)http://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
Appears in Collections:(IAA) Artículos

Files in This Item:
File Description SizeFormat
0811.1143v2.pdf2,63 MBAdobe PDFThumbnail
View/Open
Show full item record
Review this work

SCOPUSTM   
Citations

90
checked on May 14, 2022

WEB OF SCIENCETM
Citations

88
checked on May 11, 2022

Page view(s)

500
checked on May 16, 2022

Download(s)

326
checked on May 16, 2022

Google ScholarTM

Check

Altmetric

Dimensions


WARNING: Items in Digital.CSIC are protected by copyright, with all rights reserved, unless otherwise indicated.