1 = 2.2 pc and from the region ?2 = 1 pc. The high-velocity jet with a diameter ?3 = 0.2 pc is ejected from the central part of the disk, while the remnant falls onto the forming central body. The ejection velocity of the high-velocity flow is v ?0.06c. At a distance up to ? pc, the jet accelerates to an apparent velocity v ?8c. Further out, uniform motion is observed within ? pc following which deceleration occurs. The jet structure corresponding to a conical diverging helix with an increasing pitch is determined by gasdynamic instability. The counterjet structure is a mirror reflection of the nearby part of the jet. The brightness temperature of the fragment of the high-velocity flow at the exit from the counterjet nozzle is T b ?(1012?013) K. The disk inclined at an angle of 60° to the plane of the sky shadows the jet ejector region. Ring currents observed in the tangential directions as parallel chains of components are excited in the rotating flows. The magnetic fields of the rotating bipolar outflow and the disk are aligned and oriented along the rotation axis. The translational motions of the jet and counterjet are parallel and antiparallel to the magnetic field, which determines their acceleration or deceleration. The quasar core is surrounded by a thermal plasma. The sizes of the HII region reach ?0 pc. The electron density decreases with increasing distance from the center from N e ?108 to ?05 cm?. The observed emission from the jet fragments at the exit from the nozzle is partially absorbed by the thermal plasma, is refracted with increasing distance—moves with an apparent superluminal velocity, and decelerates as it goes outside the HII region." />
Kinematics of the active region of the quasar 3C 345
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  • 作者：L. I. Matveyenko (1)
    S. S. Sivakon-/a> (1)
  • 关键词：3C 345 ; AGNs ; accretion disk ; jet ; counterjet ; polarization ; absorption ; refraction
  • 刊名：Astronomy Letters
  • 出版年：2013
  • 出版时间：August 2013
  • 年：2013
  • 卷：39
  • 期：8
  • 页码：481-512
  • 全文大小：1954KB
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  • 作者单位：L. I. Matveyenko (1)
    S. S. Sivakon-/a> (1)

    1. Space Research Institute, Russian Academy of Sciences, Profsoyuznaya ul. 84/32, Moscow, 117997, Russia
文摘
The fine structure of the quasar 3C 345 in polarized emission at 7 mm and 2 cm has been investigated. The kinematics is shown to correspond to an anticentrifuge: the thermal plasma of the surrounding space accretes onto the disk, flows to the center, and is ejected in the form of a rotating bipolar outflow that carries away the excess angular momentum as it accumulates. The bipolar outflow consists of a high-velocity central jet surrounded by a low-velocity component. The low-velocity flows are the rotating hollow tubes ejected from the peripheral part of the disk with a diameter ～?sub class="a-plus-plus">1 = 2.2 pc and from the region ?2 = 1 pc. The high-velocity jet with a diameter ?3 = 0.2 pc is ejected from the central part of the disk, while the remnant falls onto the forming central body. The ejection velocity of the high-velocity flow is v ?0.06c. At a distance up to ? pc, the jet accelerates to an apparent velocity v ?8c. Further out, uniform motion is observed within ? pc following which deceleration occurs. The jet structure corresponding to a conical diverging helix with an increasing pitch is determined by gasdynamic instability. The counterjet structure is a mirror reflection of the nearby part of the jet. The brightness temperature of the fragment of the high-velocity flow at the exit from the counterjet nozzle is T b ?(1012?013) K. The disk inclined at an angle of 60° to the plane of the sky shadows the jet ejector region. Ring currents observed in the tangential directions as parallel chains of components are excited in the rotating flows. The magnetic fields of the rotating bipolar outflow and the disk are aligned and oriented along the rotation axis. The translational motions of the jet and counterjet are parallel and antiparallel to the magnetic field, which determines their acceleration or deceleration. The quasar core is surrounded by a thermal plasma. The sizes of the HII region reach ?0 pc. The electron density decreases with increasing distance from the center from N e ?108 to ?05 cm?. The observed emission from the jet fragments at the exit from the nozzle is partially absorbed by the thermal plasma, is refracted with increasing distance—moves with an apparent superluminal velocity, and decelerates as it goes outside the HII region.

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