How Would Be Artificial Dyson-like Structures Around Pulsars Constructed By Supercivilizations? Part 2: Are They Detectable? (Astronomy)

Previously on, “How Would Be The Artificial Dyson-like Structures Around Pulsars Constructed By Supercivilizations?”, we saw Osmanov extended the idea of Freeman Dyson and have shown that a supercivilization has to use ring-like megastructures around pulsars instead of a spherical shell. He also showed that where the ring exactly located and what will be the size of the ring for slowly and rapidly rotating neutron stars. If you haven’t read it yet, kindly go through it first.

Now, in this part, we are going to see if these dyson rings around pulsars are detectable? If yes, how can we detect it? In order to know the answers of these questions, we have to follow up another work of Osmanov. In this work, he outlined the main results of his previous paper, where the extension of the idea of Freeman Dyson has been considered and it has been shown that for relatively slowly rotating pulsars with P = 0.5s and P˙ = 10¯15 ss¯1 the habitable zone will be on distances of the order of 0.1AU. By examining the ring in the habitable zone, in this work, he showed that the temperature of this megastructure will be of the order 390K, indicating that the Dyson megastructure will be visible in the IR band.

He have also considered the sensitivity of VLTI and by taking into account its higher possible angular resolution, 0.001mas, he showed that the maximum distance ∼ 0.2kpc leads to the IR spectral density of the order of 7.4mJy, which in turn, can be detected by the VLTI. He have argued that by monitoring the nearby zone of the solar system approximately 64 pulsars are expected to be located inside it.

In addition, he showed that in order to observe the infrared sources up to the distances of the order of ∼kpc, the IR flux density is of the order of 3 × 10¯27 ergs s¯1 cm¯2 Hz¯1, which can be detected by the IR telescope WISE. On the other hand, the angular resolution is not enough to see the structure of the ring. Therefore, it is necessary to find another feature of the distant IR ring.

Moreover, by implying the model developed by Zhang & Harding, he have found that the temperature of the neutron star’s surface is 7000K, which in the electromagnetic spectrum corresponds to the UV band. The corresponding spectral energy flux density for the distance ∼ 1kpc, 10¯31 ergs s¯1 cm¯2 Hz¯1 is so small that at this moment no UV instrument has such a high sensitivity.

“We show that pulsars from the distance of the order of ∼ 1kpc are still visible for WISE as point-like sources but in order to confirm that the object is the neutron star, one has to use the UV telescopes, which at this moment cannot provide enough sensitivity.”

— told Osmanov, author of the study

As we have seen above, the search of infrared rings is quite promising for distances up to ∼ 0.2kpc, where one will be able to monitor potentially 64 pulsars by using the IR instruments. Observation of distant pulsars (up to ∼ 1kpc), although will significantly increase the total number of potential objects – to 1600, but at this moment the UV instruments cannot provide such a level of sensitivity.

Reference: Osmanov, Z. (2018). Are the Dyson rings around pulsars detectable? International Journal of Astrobiology, 17(2), 112-115. doi:10.1017/S1473550417000155

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