![]() ![]() ![]() You can only do this in the VAB, not during flight. You have to do this switch in the VAB by right-clicking on the generator and changing the type (there's a button to change it). When I switched my 2.5m generator to use the KTEC Solid type, it worked. I don't know what the heck is going on and nothing online is helping me (the documentation for the mod is REALLY bad =P).ĭoes the antimatter containment need to be directly attached to the reactor? What am I missing?Įdit: Found it. Nothing changes the fact that my Antimatter reactor is outputting 0 KW. ![]() I have turned the microwave receiver on and off, the smaller reactor on and off, all just to see if there's something weird going on. The problem is, it says it's outputting at 0 KW (0%). I'll get into orbit using my microwave power network, and get a fair amount of antimatter (1500 or so), and then try to turn the antimatter reactor on. Finally, I top it all off with an Alcubierre drive and 4 huge radiators. I successfully got into a 900km orbit with a ship that has 2 collectors, a 62.5m generator/fission reactor for backup power, a 2.5m generator/antimatter reactor for primary propulsion (Quantum Vacuum plasma thruster for primary thrust), and I also have a 2.5m antimatter containment unit. We conducted Very Long Baseline Array (VLBA) observations of seven nearby narrow-line Seyfert 1 (NLS1) galaxies at 1.7 GHz ( yr are much younger than radio galaxies but comparable to other NLS1s.So, I got up to getting Antimatter reactors, and I'm trying to use them. Box 23-141, Taipei 10617, Taiwan (China) Fujisawa, Kenta [The Research Institute of Time Studies, Yamaguchi University, 1677-1 Yoshida, Yamaguchi, Yamaguchi 753-8511 (Japan) Nagai, Hiroshi Hagiwara, Yoshiaki [National Astronomical Observatory, 2-21-1 Osawa, Mitaka, Tokyo 181-8588 (Japan) Wajima, Kiyoaki, E-mail: [Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030 (China) VERY LONG BASELINE ARRAY IMAGING OF PARSEC-SCALE RADIO EMISSIONS IN NEARBY RADIO-QUIET NARROW-LINE SEYFERT 1 GALAXIESĮnergy Technology Data Exchange (ETDEWEB)ĭoi, Akihiro [The Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuou-ku, Sagamihara, Kanagawa 252-5210 (Japan) Asada, Keiichi Inoue, Makoto [Academia Sinica Institute of Astronomy and Astrophysics, P.O. We find one-sided parsec-scale jet structures in Mrk 348, Mrk 231, NGC 4151, and NGC 5506 using VLBI, and we measure low jet speeds (typically = 2 Ã- 105 cm-3 assuming a path length of 0.1 pc, typical of that expected at the inner edge of the obscuring torus. To distinguish, one can look for signs of interaction between the jet and the narrow-line region, and to measure the jet speed close to the jet base, before environmental effects become important. Perhaps the engine is the same in both systems and the jet gets disrupted by dense interstellar medium in radio-quiet objects, or else the difference is intrinsic with jet power scaling with black hole spin. Wrobel Active galaxies tend to be powerful or weak radio sources, and we still do not understand the underlying cause. Parsec-scale jets and tori in seyfert galaxies This suggestion is tentatively supported by Hubble Space Telescope optical polarimetry but needs to be examined in a greater number of sources. The transverse RM gradient in 3C78, the increase in the degree of polarization at the jet edge, the large rotation in the polarization angles due to Faraday rotation, and the low depolarization between frequencies suggest that a layer surrounding the jet with a sufficient number of thermal electrons and threaded by a toroidal or helical magnetic field is a good candidate for the Faraday rotating medium. The RM values in 3C78 and 3C264 are similar to those previously observed in nearby radio galaxies. The inner- jet magnetic field, corrected for Faraday rotation, is found to be aligned along the jet in both 3C78 and 3C264, although the field becomes orthogonal further from the core in 3C78. A transverse RM gradient is observed across the jet of 3C78. ![]() In 3C66B, polarization was detected at 8 GHz only. We detect Faraday rotation measures (RMs) of the order of a few hundred rad m -2 in the nuclear jet regions of 3C78 and 3C264. We report here the detection of parsec-scale polarization at one or more frequencies in all three FRI galaxies studied. Parsec-scale polarization has been detected in a large number of beamed radio-loud active galactic nuclei, but in only a handful of the relatively unbeamed radio galaxies. We present the results of a parsec-scale polarization study of three FRI radio galaxies-3C66B, 3C78, and 3C264-obtained with Very Long Baseline Interferometry at 5, 8, and 15 GHz. A reactionless drive is a hypothetical device producing motion without the exhaust of a propellant. International Nuclear Information System (INIS) ROTATION MEASURES ACROSS PARSEC-SCALE JETS OF FANAROFF-RILEY TYPE I RADIO GALAXIES ![]()
0 Comments
Leave a Reply. |
AuthorWrite something about yourself. No need to be fancy, just an overview. ArchivesCategories |