The standard solar model (SSM) is a mathematical treatment of the Sun as a spherical ball of gas (in varying states of ionisation, with the hydrogen in the deep interior being a completely ionised plasma).
 This model, technically the spherically symmetric quasi-static model of a star, has stellar structure described by several differential equations derived from basic physical principles.
 The model is constrained by boundary conditions, namely the luminosity, radius, age and composition of the Sun, which are well determined.
 The age of the Sun cannot be measured directly; one way to estimate it is from the age of the oldest meteorites, and models of the evolution of the Solar System.
 The composition in the photosphere of the modern-day Sun, by mass, is 74.9% hydrogen and 23.8% helium.
 All heavier elements, called "metals" in astronomy, account for less than 2 percent of the mass.
 The SSM is used to test the validity of stellar evolution theory.
 In fact, the only way to determine the two free parameters of the stellar evolution model, the helium abundance and the mixing length parameter (used to model convection in the Sun), are to adjust the SSM to "fit" the observed Sun.
WR 102ka, also known as the Peony star, is a Wolf-Rayet star that is one of several candidates for the most luminous known star in the Milky Way.
 An even more luminous yet closer star, WR 25, appears to be most likely to the title.
 Another nearer star Eta Carinae, which was the second brightest star in the sky for a few years in the 19th century, appears to be slightly more luminous than WR 102ka, but is known to be a binary star system.
 There is also the more recently discovered Pistol star that, like the Peony star, derives its name from the shape of the nebula in which it is embedded, and which it has probably created through heavy mass loss via fierce stellar winds and perhaps also major "mini-supernova-like" eruptions as happened to Eta Carinae around the 1830s-1840s creating the lobes observed by the Hubble Space Telescope.
WR 102c is a Wolf–Rayet star located in the constellation Sagittarius towards the galactic centre.
 It is only a few parsecs from the Quintuplet Cluster, within the Sickle Nebula.
An O-type star is a hot, blue-white star of spectral type O in the Yerkes classification system employed by astronomers.
 They have temperatures in excess of 30,000 kelvins (K) and so appear to the left on the Hertzsprung–Russell diagram.
 Stars of this type are identified by their dominant Helium II absorption lines, strong lines of other ionised elements, and Hydrogen and neutral He lines weaker than spectral type B.
Wolf–Rayet stars, often abbreviated as WR stars, are a rare heterogeneous set of stars with unusual spectra showing prominent broad emission lines of highly ionised helium and nitrogen or carbon.
 The spectra indicate very high surface enhancement of heavy elements, depletion of hydrogen, and strong stellar winds.
 Their surface temperatures range from 30,000 K to around 200,000 K, hotter than almost all other stars.
WR 102ea is a Wolf–Rayet star in the Sagittarius constellation.
 It is the second most luminous star in the Quintuplet cluster after WR 102hb.
 With a luminosity of 2,500,000 times solar, it is also one of the most luminous stars known.
 Despite the high luminosity it can only be observed at infra-red wavelengths due to the dimming effect of intervening dust on visual light.
NGC 6814 is an intermediate spiral galaxy in constellation Aquila.
 It is located at a distance of about 75 million light years from Earth, which, given its apparent dimensions, means that NGC 6814 is about 85,000 light years across.
 NGC 6814 has an extremely bright nucleus and is a type 1.5 Seyfert galaxy.
 The galaxy is also a highly variable source of X-ray radiation.
 The ultraviolet and optical emission also varies, although more smoothly, with time lag of two days.
 The cause of the lag and the smoothening of lightcurves is considered to be the reprossesing of the X-rays in the accretion disk.
 The cause of the active galactic nucleus is suspected to be a supermassive black hole with a mass about 18 million times that of the Sun.
 Many regions of ionised gas are studded along the dusty spiral arms.
WR 102 is a Wolf-Rayet star in the constellation Sagittarius, an extremely rare star on the WO oxygen sequence.
WR 7 (HD 56925) is a Wolf-Rayet star in the constellation of Canis Major.
 It lies at the centre of a complex bubble of gas which is shocked and partially ionised by the star's radiation and winds.
The Cockermouth & Workington Railway was an English railway company (established by Act of Parliament in 1845) which built and operated a railway between the Cumbrian towns of Workington and Cockermouth .
 The railway opened for service in 1847, and ran from the Whitehaven Junction Railway station at Workington to a station at Cockermouth near the bridge over the Derwent.
 A single-tracked line of eight and a half miles length, its revenue came largely from the transport of coal from the pits of the lower Derwent valley to the port at Workington for shipment by sea.
 The Marron extension of the Whitehaven, Cleator and Egremont Railway and the Derwent Branch of the Maryport and Carlisle Railway were both constructed to link with the C&WR and together give an alternative route for the northward movement of haematite ore from the Cumberland ore-field.
 The completion of the Cockermouth, Keswick and Penrith Railway made the C&WR part of a continuous through route between South Durham and the Cumberland orefield.
 These developments both improved the potential profitability of the C&WR and made control of it important to bigger companies wishing to maximise the iron-ore traffic over their lines: the C&WR was absorbed by the London and North Western Railway in 1866.
 Goods traffic on the line ceased in 1964; passenger traffic in 1966.
 From just east of Bridgefoot to just short of the Papcastle roundabout, the modern A66 trunk road follows the alignment of the C&WR.

Question: What highly ionised elements are found in the spectrum of WR 102c?
Answer: helium and nitrogen