G'day Miss Buffy
Mate, I do not want to be rude, thats the last thing I want to do.
My task at the moment is to get through this reading and hope by 2 years time I will have a little bit more to add.
Modest has given me many links to read, I'm in the middle of those papers.
I'm trying to find where the darn jets form, thats if we have the tools to show us.
Just reading these links, I feel I'm getting closer to the explanation and yet I feel I'm a million miles away.
As for using this as a personal Note pad. That is a far cry. My comp has about 20,000 papers not that I have read them all yet.
I'm also looking for that person who is in the field that is able to help me with the discussion.
How Compact are the Cores of AGN? Sub-Parsec Scale Imaging with VLBI at Millimeter Wavelengths
Authors: T.P. Krichbaum, S.S. Lee, A.P. Lobanov, A.P. Marscher, M.A. Gurwell
(Submitted on
29 Aug 2007)
Quote:
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Abstract: We study the most central regions of AGN jets with an angular resolution of tens of micro-arcseconds using VLBI at millimeter wavelengths (mm-VLBI). We present and discuss a new 86 GHz VLBI survey of compact radio sources. We show new high dynamic range images of two nearby radio galaxies (3C 120 and M87). In M87 the size of the compact VLBI core (the jet base) is < 15 Schwarzschild radii. Future mm-VLBI observations at 1 mm and shorter wavelengths should lead to images of galactic and extragalactic radio sources with a spatial resolution down to a few Schwarzschild radii of the central super massive black holes. To achieve this, the participation of large and sensitive millimeter and sub-millimeter telescopes in VLBI is essential. Owing to their high sensitivity existing and planned phased interferometers like the IRAM Plateau de Bure interferometer, CARMA, the SMA and ALMA could play an important role.
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Part 5 The jet of M87
Quote:
We may identify the size of the
brightest and most compact VLBI component with the jet diameter at or near its
origin. In this case it is remarkable that the jet base is so small and bright (TB ≥
2 · 1010 K), contrary to expectations from magnetic-slingshot type acceleration
models (e.g. Blandford & Payne 1982). Here, magnetic fields are anchored in the
rotating accretion disk, expand and form a light-cylinder. Its diameter defines
the minimum jet width of > 50Rs (Camenzind 1990; Fendt & Memola 2001).
The observed small size therefore points more towards models in which the jet
is attached more directly to the rotating black hole (Blandford & Znajek 1977),
gaining its energy viaMHD interaction with the inner disk (e.g. Mc Kinney 2006)
or the Penrose process (Gariel et al. 2007, and references therein).
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So I'm searching the papers that can somehow explain further the location and formation of jets. So I keep on reading. Everytime I come across an interesting link I want to share it. I hope there is no harm in that. If this is rude I will make this my last post in linksand just chat.
[astro-ph/0406235] Synchrotron Self-Compton Model for Rapid Nonthermal Flares in Blazars with Frequency-Dependent Time Lags
Synchrotron Self-Compton Model for Rapid Nonthermal Flares in Blazars with Frequency-Dependent Time Lags
Authors: Andrei Sokolov, Alan P. Marscher, Ian M. McHardy
(Submitted on
9 Jun 2004)
Quote:
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Abstract: We model rapid variability of multifrequency emission from blazars occurring across the electromagnetic spectrum (from radio to gamma-rays). Lower energy emission is produced by the synchrotron mechanism, whereas higher energy emission is due to inverse Compton scattering of the synchrotron emission. We take into account energy stratification established by particle acceleration at shock fronts and energy losses due to synchrotron emission. We also consider the effect of light travel delays for the synchrotron emission that supplies the seed photons for inverse Compton scattering. The production of a flare is caused by the collision between a relativistic shock wave and a stationary feature in the jet (e.g., a Mach disk). The collision leads to the formation of forward and reverse shocks, which confine two contiguous emission regions resulting in complex profiles of simulated flares. Simulations of multifrequency flares indicate that relative delays between the inverse Compton flares and their synchrotron counterparts are dominated by energy stratification and geometry of the emitting regions, resulting in both negative and positive time delays depending on the frequency of observation. Light travel effects of the seed photons may lead to a noticeable delay of the inverse Compton emission with respect to synchrotron variability if the line of sight is almost perfectly aligned with the jet. We apply the model to a flare in 3C 273 and derive the properties of shocked plasma responsible for the flare. We show that the pronounced negative time delay between the X-ray and IR light curves (X-rays peak after the maximum in the synchrotron emission) can be accounted for if both forward and reverse shocks are considered.
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