On dynamical models for radio galaxies |
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| Affiliation: | 1. Astrophysics Research Center, Physics Department, New Mexico Tech, Socorro, NM 87801, USA;2. Physics & Astronomy Department, University of Alabama, Tuscaloosa, AL 35487, USA;3. Institute for Astrophysics, Physics & Astronomy Department, University of New Mexico, Albuquerque NM 87131, USA;1. Government Science College, Hassan 573201, Karnataka, India;2. St Aloysius College (Autonomous), Mangalore 575001, Karnataka, India;3. University Science Instrumentation Centre (USIC), Mangalore University, Mangalagangothri 574199 (D K), Karnataka, India;1. Department of Engineering Physics, Tsinghua University, Beijing, 100084, China;2. Key Laboratory of Particle & Radiation Imaging (Tsinghua University), Ministry of Education, Beijing, 100084, China;3. Nuclear Reactor Laboratory, Massachusetts Institute of Technology, 77 Massachusetts Ave., Cambridge, MA 02139, USA;4. Physical Measurement Laboratory, NIST, Gaithersburg, Maryland 20899-8461, USA;1. Max-Planck-Institut für Kernphysik, D-69029 Heidelberg, Germany;2. Yerevan Physics Institute, 375036 Yerevan, Armenia;1. Astronomical Observatory of the Kyiv University, Observatorna Str. 3, Kyiv 04053, Ukraine;2. Main Astronomical Observatory of the National Academy of Sciences of Ukraine, Golosiiv, Kyiv 03680, Ukraine |
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| Abstract: | The tailed radio galaxies that have been called ‘Type I’ are not a uniform set. To study their dynamics, we have used the Ledlow–Owen data set, which provides a new sample of 250 radio galaxies in nearby Abell clusters. These sources divide into two clear categories based on their radio morphology. Type A sources (‘straight’) contain nearly straight jets which are embedded in outer radio lobe. Type B sources (‘tailed’) have a well-collimated jet flow which undergoes a sudden transition, at an inner hot spot, to a less collimated flow which continues on and forms a radio tail. We have not found any separation of these classes in terms of radio power, radio flux size, galaxy power or external gas density. We propose the difference is due to the development, or not, of a disruptive flow instability, such as Kelvin–Helmholtz, and the saturation of the instability when it develops. |
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