The Fusion Gungnir (Also known as IC 1613 DR1) was an oxygen-sequence Wolf-Rayet star located in Aolunsk Galaxy, that during the War of the Ancients, was used strategically by the Quintet Puontari Federation to eliminate most CUEN forces in its area. It was discovered before 2100, but the exact date has been lost. At the time of its discovery, it was already nearing the end of helium burning.
Due to being a WO (oxygen-sequence Wolf-Rayet) star, the Fusion Gungnir had to be an extremely hot star, the hottest non-degenerate star in the entire galaxy at the time of its existence, in fact. When it was discovered, it had a temperature of 150000 Kelvins. Over the remainder of its lifetime, that value increased to a staggering 296000 Kelvins.
WO stars are typically very small for their mass, and so was this star. It was only 3% larger than Sol at the time of its discovery, and it had shrunk to a mere 19% the size of Sol when it finally died.
Solar Wind and Nebula
All Wolf-Rayet stars have extremely powerful solar winds, especially WOs (due to their high temperatures), and this star was no exception. Its solar wind was so powerful that in 2122 CE, it was discovered to have a wind-blown bubble nebula, made of the matter that it had expelled as a red supergiant that had been ionized and glowed a brilliant blue. The solar wind is also responsible for heavy mass loss, making the Fusion Gungnir lose nearly 88% of its initial mass by the time of its death.
However, the Gungnir's wind is in fact slower than other WO stars, at just ~3000 km/s, compared to, for example, 5000 km/s for the WO2 star WR 102. This is partially due to its lower temperature, but it is more to do with the Fusion Gungnir's low metallicity environment.
As Wolf-Rayet stars (especially WOs) are the stripped cores of massive stars, they do not have much hydrogen left in them at all. Owing to this, they have a very high metallicity, often above 2.5. At the time of its discovery, only about 0.008% of the star was still hydrogen, leading to a very high metallicity of ~3,2. If the star were one solar mass, its metallicity would be around 1.91. However, the Fusion Gungnir exists in a low metallicity environment (Aolunsk) and so its initial metallicity would be much lower.
Around 4.5 million years ago, the Fusion Gungnir started life as a rapidly spinning massive star about 50 times more massive than the sun, and around 330000 times brighter. It rapidly fused hydrogen and slowly expanded and accumulated heavy elements in its core. The convection that took place in the various stellar layers brought these heavy elements throughout the star, enriching it and giving it the f designation at the end of its spectral type.
Around a million years ago, it started to expand, becoming a blue supergiant and experiencing heavy mass loss. The star started to pulsate and became a small LBV, radiating around 540000 suns worth of energy. With every pulsation, a bit more mass was released, and around 400,000 years ago, the LBV was so small it was too small to pulsate and then it became a Wolf-Rayet star.
Now a carbon-sequence WR, the Fusion Gungnir continued to steadily decrease in mass and size, and increase in temperature. By 50000 BC, the star was already a WC6.5 star, with only 2.5 times Sol's size and 80000 K in temperature. Finally, in 10000 BC, the star entered the WO stage, and continued to shrink until its eventual death in 88714 CE.