Evolution of the X-Ray Jets from 4U 1755--33

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dc.creatorKaaret, P.
dc.creatorCorbel, S.
dc.creatorTomsick, J. A.
dc.creatorLazendic, J.
dc.creatorTzioumis, A. K.
dc.creatorButt, Y.
dc.creatorWijnands, R.
dc.date2005-12-09
dc.date.accessioned2026-07-07T10:27:44Z
dc.date.available2026-07-07T10:27:44Z
dc.descriptionWe report on new X-ray observations of the large-scale jets recently discovered in X-rays from the black hole candidate 4U 1755-33. Our observations in 2004 show that the jets found in 2001 are still present in X-rays. However, sensitive radio observations in 2004 failed to detect the jets. We suggest that synchrotron radiation is a viable emission mechanism for the jets and that thermal bremsstrahlung and inverse-Compton emission are unlikely on energetic grounds. In the synchrotron interpretation, the production of X-rays requires acceleration of electrons up to ~ 60 TeV, the jet power is ~ 4x10^35 erg s^-1, and the radio non-detection requires a spectral index alpha > -0.65 (S_ν\propto ν^α) which is similar to the indexes found in lobes surrounding some other compact objects. We find an upper limit on the flux of 4U 1755-33 in quiescence of 5x10^-16 erg cm^-2 s^-1 in the 0.3-8 keV band.
dc.descriptionaccepted by ApJ, 11 pages, 2 color figures
dc.identifierhttps://arxiv.org/abs/astro-ph/0512240
dc.identifierhttp://arxiv.org/abs/astro-ph/0512240
dc.identifierAstrophys.J.641:410-417,2006
dc.identifierdoi:10.1086/500399
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/177241
dc.subjectAstrophysics
dc.titleEvolution of the X-Ray Jets from 4U 1755--33
dc.typetext

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