adolfodarriba@ observatoriolascasqueras.es

Detection of the time delays in AGNs through radioactive decay In this study, I focused mainly on the radioactive decay of cadmium 109, which occurs at 463 days. My objective is to detect if a time delay occurs in the different AGNs. The following light curves of the AAVSO correspond to 1,000 days of observation. Below, I expose the list of all radioactive elements within this period. Although I show the three types of explosions, as I have defined it in my previous article (it is the first link of this Web), Type III Explosions are the most energetic. Therefore, they are the ones that best adjust to secondary explosions with the disintegration of radioactive elements, measured in their half-life. As their behavior are the least random, it is easier to find a pattern of behavior among them all. As seen in the following light curves of the AAVSO, in most of them there is a time delay in the AGNs studied. The maximum brightness in the optician is the point that I consider as the Main Explosion, marked as 0 days. It is also observed that the maximum brightness in Gamma rays usually occurs about 3 days before. The time delay in all subclasses of AGNs (Blazars, Quasars, Seyfert 2 galaxies, etc.) is the same. The only thing that is appreciable in its curves of light, is its lower light amplitude. Secondary explosions are directly related to the radioactive decay of the different elements. What is more difficult for me is to detect the exact moment of the main explosion and secondary explosions. As I gather more light curves, I will attach it and reduce the errors. That is, I want to further define the light curve and its time delay. That is why, if the maximum brightness in the optical occurs a few days after the radioactive decay of Cadmium 109, which occurs at 463 days, then a time delay in the AGN is deduced. Actually, this is my main objective of this study. If so, all maximums (red lines) and minimums (blue lines) will be displaced to the right in their proportion (blue and yellow discontinuous lines). In the graph below, a light curve of an Explosion of Type III is theoretically represented, with a maximum brightness very marked in the 85 days, as bright as the main explosion. If the AGN were really a Type I Explosion, secondary explosions would not be detected in most cases. If it were an Explosion of Type II, the maximums in the secondary explosions would be more representative, but it would not have a maximum in the 85 days.

Basic concepts - The Blazares are still predictable. Light curves 1,000 days. - There are three types of main explosions. Type I, Type II and Type III. - At the time of a principal explosion, a cascade of stable elements is produced as radioactive. - The radioactive decays of the different elements cause secondary explosions. - Depending on the sharpness of the secondary explosions, the width of the jet can be known. - As the radioactive elements behave like well-defined atomic clocks measured in their half-life, when there is a delay in the secondary explosions, it is a clear indication of their time delay. That is, each Blazar has its own time delay. Types of main explosions - Those of Type I, usually move near their minimum brightness, without large variations occurring when they reach their secondary explosions, although sometimes there is some significant increase. Its most important feature is that no explosions are detected between 60 and 100 days. Its trajectory is usually flat or even descending slightly. - Those of type II, have a greater movement within the light curve, detecting an increase in brightness at 75 and 90 days later. - Those of type III, are the most energetic explosions. A secondary explosion is detected at 85 days, almost as bright as the main one. They are the most predictable. Its movement within the light curve is similar to those of Type II. Concept in Gamma flashes - In Gamma rays, the main explosion usually happens about 3 to 10 days before the optic. - In secondary explosions usually occurs with the same time delay as the optical or about 6 days later. - Occasionally, a Gamma flash is observed three or four weeks apart from the previous, which would correspond to a maximum of light in the optic. - This symmetry is produced because the two lobes are connected and we would be seeing the Gamma flash coming from the opposite lobe. That is, we would see a symmetry in the Gamma flash, not being the same in their detection, although physically they would be the same. - The time taken from the first Gamma flash to the second is the distance that the two lobes are separated. It is not strictly correct because space-time is dragged and this greatly influences this appreciation. - It is possible that the symmetry is produced by the precession of the two emitting lobes, when rotating. Hence, the symmetry of each blazar never occurs in a certain exact time. Mathematic expression Each Blazar has its own time delay, so I apply a constant (D). In my theoretical model above, the constant could be: D = 0.011 That is, when the maximum brightness occurs at 463 days (T), its time delay corresponds (Td): Td = T x D // Td = 463 x 0.011 // Td = 5 Days (The maximum would occur 5 days later) and when it reaches 735 days (T), it corresponds to: Td = T x D // Td = 735 x 0.011 // Td = 8 Days (The maximum would occur 8 days later) As can be seen, the time delay (Td) is proportional to the elapsed time (T). Temporary Delay. Cadmium 109 Outburst Type I Blazar BL LAC (22 02 43.29139 +42 16 39.9803) z=0.069 Outburst Type I Seyfert 1 Galaxy 3C 390.3 (18 42 08.9899 +79 46 17.128) z=0.056159 Outburst Type I Quasar 3C 279 (12 56 11.16657 -05 47 21.5247) z=0.53620 Light curve. NASA's Fermi Gamma-ray Space Telescope Outburst Type II Blazar S5 2007+77 (20 05 31.004 +77 52 43.27) z=0.342 The Astronomer’s Telegram. Nº 8635 Burst Gamma ray. 4 Feb 2016 Light curve. NASA's Fermi Gamma-ray Space Telescope Outburst Type II Quasar PKS 0736+01 (07 39 18.03390 +01 37 04.6179) z=0.191 Light curve. NASA's Fermi Gamma-ray Space Telescope Outburst Type III Seyfert 1 Galaxy 1RXS J190910.3+665222 (19 09 10.8964 +66 52 21.373) z=0.191 Outburst Type II Blazar PKS 0716+71 (07 21 53.44846 +71 20 36.3634) z=0.300 Light curve. NASA's Fermi Gamma-ray Space Telescope Outburst Type III Blazar OT 081 (17 51 32.81855 +09 39 00.7288) z=0.322 Light curve. NASA's Fermi Gamma-ray Space Telescope Outburst Type II Quasar S5 1044+71 (10 48 27.6 +71 43 36) z=1.1500 Light curve. NASA's Fermi Gamma-ray Space Telescope Outburst Type III Blazar S5 1803+78 (18 00 45.684 +78 28 04.02) z=0.680 The Astronomer’s Telegram. Nº 7933 Burst Gamma ray. 20 Aug 2015 Light curve. NASA's Fermi Gamma-ray Space Telescope Outburst Type III Blazar S4 0954+65 (09 58 47.24510 +65 33 54.8181) z=0.367 Light curve. NASA's Fermi Gamma-ray Space Telescope Outburst Type III Seyfert 1 Galaxy S4 1030+61 (10 33 51.42726 +60 51 07.3301) z=1.40095 Light curve. NASA's Fermi Gamma-ray Space Telescope Outburst Type III Blazar OJ 287 (08 54 48.87493 +20 06 30.6410) z=0.306 The Astronomer’s Telegram. Nº 9489 Burst Gamma ray. 13 Sep 2016 Light curve. NASA's Fermi Gamma-ray Space Telescope Outburst Type III Blazar S2 0109+224 (01 12 05.82470 +22 44 38.7868) z=0.265 Outburst Type I Blazar PKS 0048-09 (00 50 41.31738756 -09 29 05.2102688) z=0.635 Outburst Type II Blazar QSO B0506+056 (05 09 25.9645434784 +05 41 35.333636817) z=0.3365 Outburst Type ? Quasar 4C 29.45 (11 59 31.83390975 +29 14 43.8268741) z=0.72475 Outburst Type ? Quasar 1ES 0806+52.4 (08 09 49.18673 +52 18 58.2507) z=0.13710 Outburst Type III Blazar PKS 0735+178 (07 38 07.39376 +17 42 18.9983) z=0.424 Outburst Type I Blazar QSO B1553+113 (15 55 43.0440 +11 11 24.366) z=0.360 Outburst Type ? Blazar NSV 19409 (12 30 14.0894 +25 18 07.136) z=0.135 Outburst Type ? Quasar PKS 1510-089 (15 12 50.53292 -09 05 59.8296) z=0.360 Outburst Type III Quasar B2 1420+32 (14 22 30.37890 +32 23 10.4446) z=0.68144 Light curve. NASA's Fermi Gamma-ray Space Telescope Outburst Type III Blazar S5 1803+78 (18 00 45.684 +78 28 04.02) z=0.680 Outburst Type III Blazar BL LAC (22 02 43.29139 +42 16 39.9803) z = 0.069 Outburst Type ?? Blazar S4 0954+65 (09 58 47.24510 +65 33 54.8181) z=0.367 Outburst Type ? Quasar 4C 29.45 (11 59 31.83390975 +29 14 43.8268741) z=0.72475 Outburst Type III Blazar S4 1749+70 (17 48 32.84043 +70 05 50.7684) z=0.770 Light curve. NASA's Fermi Gamma-ray Space Telescope Outburst Type III Blazar PKS 0735+178 (07 38 07.39376 +17 42 18.9983) z=0.424 Outburst Type I Blazar B2 1147+24 (11 50 19.2122083392 +24 17 53.834712576) z=0.2090 Conclusions - The Blazars have a temporary delay. This indicates that the observed light is very close to the event horizon of the black hole. - They have a recognizable pattern. They are predictable. - Secondary explosions correspond to radioactive decays and are in direct proportion to the intensity emitted. By comparing the intensity of these secondary explosions, we can know their amount of heavy elements. - All AGNs have their maximum and minimum periods, equal. This confirms that all AGNs are the same objects, viewed from different perspectives. - Although the maximum brightness at different wavelengths is related, there is a time delay of a few days with respect to other types of wavelengths detected, so that light emission does not occur exactly in the same place. Even in the main explosion, the maximum brightness in Gamma rays usually happens about 3 days earlier than in the optic. - The higher the frequency detected, for example, in Gamma rays with respect to optics, the faster its brightness can change. This indicates that the gamma-ray emitting region is much smaller than in the optical region. - By comparing the degree of time delay with other astrophysical magnitudes, we could discover related concepts. - Depending on the Blazar, the main explosion as secondary explosions may be more acute or flattened, in the curves of light. We could know why the cone of the emitting Jet is narrower than others. Types of radioactive disintegration Type III Outbursts secondary (Around 8 days) Iodine 131 to Xenon 131 --> Half life 8,02 days Selenium 72 to Astatine 72 --> Half life 8,40 days Thulium 167 to Erbium 167 --> Half life 9,25 days Erbium 169 to Thulium 169 --> Half life 9,40 days Actinium 225 to Fran­cium 221 --> Half life 10,00 days Iridium 193 to Iridium 193 --> Half life 10,5 days Barium 140 to Lanthanum 140 --> Half life 12,8 days (Around 18 days) Provoked as in the SN IIb Protactinium 230 to Thorium 230 --> Half life 17,40 days Arsenic 74 to Germanium 74 --> Half life 17,78 days Californium 253 to Einsteinium 253 --> Half life 17,81 days Californium 253 to Curium 249 --> Half life 17,81 days (Around 20 days) Einsteinium 253 to Berkelium 249 --> Half life 20,47 days (Around 30 days) Chromium 51 to Vanadium 51 --> Half life 27,70 days Protactinium 233 to Uranium 233 --> Half life 29,97 days Osmium 193 to Iridium 193 --> Half life 30,11 days Mendelevium 260 to Fermium 260 --> Half life 31,80 days Ytterbium 169 to Thulium 169 --> Half life 32,026 days Cerium 141 to Praseodymium 141 --> Half life 32,501 days Argon 37 to Chlorine 37 --> Half life 35,04 days (Around 50 days) Strontium 89 --> Half life 51,50 days Mendelevium 258 to Fermium 258 --> Half life 51,50 days Beryllium 7 to Lithium 7 --> Half life 53,12 days (Around 64 days) Zirconium 95 --> Half life 64,02 days (Around 85 days) Nickel 56 to Iron 56 --> 83,35 days (Nickel 56 to Cobalt 56 --> Vida media 6,08 days) + (Cobalt 56 to Iron 56 --> Half life 77,27 days) = 83,35 days Arsenic 73 to Germanium 73 --> Half life 80,30 days Zirconium 88 to Yttrium 88 --> Half life 83,40 days Scandium 46 to Titanium 46 --> Half life 83,79 days (Around 87 days) Sulfur 35 to Chlorine 35 --> Half life 87,32 days (Around 93 days) Thulium 168 to Erbium 168 --> Half life 93,10 days Osmium 185 to Rhenium 185 --> Half life 93,60 days (Around 120 days) Selenium 75 to Astatine 75 --> Half life 119,779 days Tungsten 181 to Tantalum 181 --> Half life 121,2 days (Around 128 days) Thulium 170 to Ytterbium 170 --> Half life 128,6 days (Around 138 days) Polonium 210 to Lead 206 --> Half life 138,376 days (Around 207 days) Rhodium 102 to Ruthenium 102 --> Half life 207,0 days (Around 272 days) Cobalt 57 to Iron 57 --> Half life 271,79 days (Around 285 days) Cerium 144 to Praseodymium 144 --> Half life 284,893 days (Around 374 days) Ruthenium 106 to Rhodium 106 --> Half life 373,59 days (Around 463 days) Cadmium 109 to Silver 109 --> Half life 462,6 days (Around 754 days) Caesium 134 to Xenon 134 --> Half life 754,17 days Caesium 134 to Barium 134 --> Half life 754,17 days (Around 950 days) Sodium 22 to Neon 22 --> Half life 950,38 days (Around 966 days) Californium 252 to Curium 248 --> Half life 966,09 days (Around 1205 days) Rhodium 101 to Ruthenium 101 --> Half life 1205,32 days (Around 1925 days) Cobalt 60 to Nickel 60 --> Half life 1925,38 days (Around 2191 days) Osmium 194 to Iridium 194 --> Half life 2191,50 days Minimum in the light curves 1º Minimum --> 60 days (First minimum important) 2º Minimum --> 103 days (End of Plateau phase) 3º Minimum --> 260 days (Minimum deep) 4º Minimum --> 317 days (Minimum deep) 5º Minimum --> 385 days (Corresponds to the absolute minimum) 6º Minimum --> 533 days (Minimum deep) 7º Minimum --> 1425 days (Corresponds to the absolute minimum) Gratefulness I thank the AAVSO for permission to publish their light curves and the M1 Group for their important contribution. Also to all observers who have made these observations, without them, this work would not have been possible. To all of them, thank you very much. Especially my partner Diego Rodríguez from the M1 Group, and Gianpiero Locatelli, Ramón Naves, David Cejudo, Jose Luis Martin and Jordi Berenguer from the Supernova Group, and Dave Hinzel and Heinz-Bernd Eggenstein from the AAVSO. Also the NASA Fermi Group to authorize publish their light curves in gamma rays for a greater understanding of these objects.