|The Blazar Times|
|A Research Newsletter Dedicated to the BL Lac and Blazar Phenomena|
|No. 50 - December 2002||Editor: Travis A. Rector (firstname.lastname@example.org)|
Journal Abstracts 1
Abstract Guidelines 3
The Blazar Times will again take a recess during the holiday season. The next issue will be in February 2003.
Happy winter solstice!
Travis A. Rector
The Disc-Jet Relation in Strong-lined Blazars
Valerio D'Elia1,2,3, Paolo Padovani1,4 and Hermine Landt1,5
1 Space Telescope Science Institute, 3700 San
Martin Drive, Baltimore MD 21218, USA
2 Dipartimento di Fisica, II Università di Roma ``Tor Vergata'', Via della Ricerca Scientifica 1, I-00133 Roma, Italy
3 Osservatorio Astronomico di Roma, Via di Frascati 33, I-00040 Monteporzio, Italy (current address)
4 ESA Space Telescope Division
5 Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany
The relation between accretion disc (thermal emission) and jet (non-thermal emission) in blazars is still a mystery as, typically, the beamed jet emission swamps the disc even in the ultraviolet band where disc emission peaks. In this paper we estimate the accretion disc component for 136 flat-spectrum radio quasars selected from the Deep X-ray Radio Blazar Survey. We do this by deriving the accretion disc spectrum from the mass and accretion rate onto the central black hole for each object, estimated using the emission line widths and the power emitted from the broad line region. We find that non-thermal emission dominates the optical/UV band of our sources. The thermal component, in fact, is, on average, ~ 15 per cent of the total and > 90 per cent of the objects in the sample have a thermal component < 0.5 of the total luminosity. We then estimate the integrated disc and kinetic jet powers and find that, on average, the disc luminosity is ~ 1 to 20 times the jet power (depending on the uncertainties in the estimation of the latter quantity). A comparison with previous, independent results favours a scenario in which jet and disk powers are of the same order of magnitude. Extraction of energy from a rotating black hole via the ``Blandford-Znajek'' mechanism fails to explain the estimated jet power in the majority of our sources. Finally, we find that the typical masses for our sources are ~ 5 ×108 M\odot and that, contrary to previous claims, about one quarter of our radio quasars have relatively small ( < 3 ×108 M\odot) black hole mass.
Accepted by Montly Notices of the RAS
For preprints contact: email@example.com
For preprints via ftp or WWW: http://arXiv.org/abs/astro-ph/0211147
Ultra Fast Self-Compton Cooling
1 Department of Earth and Space Science,
Osaka University, Toyonaka 560-0043, Japan
We investigate the synchrotron self-Compton process in a planar shell taking the shock structure into account. We find that the energy density of the seed photons could deviate from the one-zone estimate by order of unity depending on the shock velocity and the electron cooling time. We also find that as the electron cooling becomes faster, the seed photons are increased more, so that the inverse Compton cooling becomes more efficient. This ``ultra'' fast cooling may work in such as gamma-ray bursts, blazars and microquasars.
Accepted by ApJ
For preprints contact: firstname.lastname@example.org
Rapid Variability and Annual Cycles in the Characteristic Time-scale of the Scintillating Source PKS 1257-326
H. E. Bignall1,2, D. L. Jauncey2, J. E. J. Lovell2, A. K. Tzioumis2, L. Kedziora-Chudczer2,3, J.-P. Macquart4, S. J. Tingay2 and D. P. Rayner2
1 Dept. of Physics & Mathematical Physics, University of Adelaide, SA 5005, Australia
2 CSIRO Australia Telescope National Facitily, PO Box 76, Epping NSW 1710, Australia
3 Anglo-Australian Observatory, PO Box 296, Epping NSW 1710, Australia
4 Kapteyn Institute, University of Groningen, the Netherlands
Rapid radio intra-day variability (IDV) has been discovered in the southern quasar PKS 1257-326. Flux density changes of up to 40% in as little as 45 minutes have been observed in this source, making it, along with PKS 0405-385 and J1819+3845, one of the three most rapid IDV sources known. We have monitored the IDV in this source with the Australia Telescope Compact Array (ATCA) at 4.8 and 8.6 GHz over the course of the last year, and find a clear annual cycle in the characteristic time-scale of variability. This annual cycle demonstrates unequivocally that interstellar scintillation (ISS) is the cause of the rapid IDV at radio wavelengths observed in this source. We use the observed annual cycle to constrain the velocity of the scattering material, and the angular size of the scintillating component of PKS 1257-326. We observe a time delay, which also shows an annual cycle, between the similar variability patterns at the two frequencies. We suggest that this is caused by a small ( ~ 10 mas) offset between the centroids of the 4.8 and 8.6 GHz components, and may be due to opacity effects in the source. The statistical properties of the observed scintillation thus enable us to resolve source structure on a scale of ~ 10 microarcseconds, resolution orders of magnitude higher than current VLBI techniques allow. General implications of ISS for the physical properties of sources and the turbulent ISM are discussed.
Accepted by ApJ
For preprints contact: email@example.com
For preprints via ftp or WWW: http://arXiv.org/abs/astro-ph/0211451
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