Wolf-Rayet Star
Wolf-Rayet stars are a class of massive, hot, and luminous stars named after the astronomers Charles Wolf and Georges Rayet, who first identified them in the mid-19th century. These stars are quite rare, making up only a small fraction of all massive stars, and they are often considered the "rock stars" of the stellar world due to their extreme properties.

Here are some key characteristics and features of Wolf-Rayet stars:

1. Mass and Size: Wolf-Rayet stars are typically very massive, with masses at least 20 times that of our Sun and often much more massive, sometimes exceeding 100 times the Sun's mass. Because of their high mass, they are also quite large, with radii that can be several times that of the Sun.
2. Temperature and Spectral Classification: These stars are incredibly hot, with surface temperatures ranging from 30,000 to 200,000 degrees Celsius (54,000 to 360,000 degrees Fahrenheit). Their high temperatures cause them to emit intense ultraviolet radiation, making them easily detectable in the UV part of the electromagnetic spectrum.Wolf-Rayet stars are classified into several spectral types, mainly based on the lines present in their spectra. The two primary spectral types are WN (nitrogen-rich) and WC (carbon-rich). These spectral lines are indicative of the composition of the star's outer layers.
3. Strong Stellar Winds: Wolf-Rayet stars are known for their powerful stellar winds. These winds can blow off mass at a rate thousands to millions of times greater than the solar wind. This mass loss is due to the intense radiation pressure from their high temperatures and luminosities. As a result, Wolf-Rayet stars lose a significant portion of their mass over their relatively short lifetimes.
4. Short Lifetimes: Despite their massive size, Wolf-Rayet stars have relatively short lifespans compared to less massive stars like our Sun. They live only a few hundred thousand to a few million years, which is a mere blink of an eye in cosmic terms. This is because their high mass accelerates the nuclear fusion processes in their cores, causing them to consume their nuclear fuel rapidly.
5. Stellar Evolution: Wolf-Rayet stars are often considered a transitional phase in the life cycle of massive stars. They form from massive O-type stars as they evolve and lose their outer layers through powerful stellar winds. The process of losing mass through these winds exposes the hotter and more evolved interior layers of the star, which leads to the distinctive spectral features of Wolf-Rayet stars.
6. Supernova Progenitors: Many Wolf-Rayet stars are considered candidates to eventually explode as supernovae. When they exhaust their nuclear fuel, they can undergo a core-collapse supernova, leaving behind either a neutron star or a black hole, depending on their mass.

In summary, Wolf-Rayet stars are massive, hot, and luminous stars with short lifetimes characterized by intense stellar winds, strong ultraviolet radiation, and distinctive spectral features. They play a crucial role in the evolution of massive stars and can lead to spectacular events like supernovae when they reach the end of their lives.

WR134 (from Wikipedia):
WR 134 is a variable Wolf-Rayet star located around 6,000 light years away from Earth in the constellation of Cygnus, surrounded by a faint bubble nebula blown by the intense radiation and fast wind from the star. It is five times the radius of the sun, but due to a temperature over 63,000 K it is 400,000 times as luminous as the Sun.

WR 134 was one of three stars in Cygnus observed in 1867 to have unusual spectra consisting of intense emission lines rather than the more normal continuum and absorption lines. These were the first members of the class of stars that came to be called Wolf-Rayet stars (WR stars) after Charles Wolf and Georges Rayet who discovered their unusual appearance. It is a member of the nitrogen sequence of WR stars, while the other two (WR 135 and WR 137) are both members of the carbon sequence and also have OB companions. WR 134 has a spectrum with NIII and NIV emission between two and five times stronger than NV, leading to the assignment of a WN6 spectral type. The spectrum also shows strong HeII emission and weaker lines of HeI and CIV.

A light curve for V1769 Cygni, adapted from Marchenko et al. (1998)
WR 134 is classified as an Algol type eclipsing variable and given the designation V1769 Cygni, but the variation is not strictly periodic, and brightness changes occur on timescales of hours to days. It has been investigated several times to search for companions. Morel reported a 2.25 day primary period but considered the variations to be due to rotational modulation rather than the effects of a companion. Rustamov suggests a 1.887 day orbital period with a K-M dwarf companion, but with additional optical variations.

Both hard and soft X-rays have been detected from WR 134 but the sources are not fully explained. The emissions do not match a single star of the expected temperature, are not sufficient for colliding winds between two hot stars, and any compact source such as a neutron star or cool dwarf would be in an unlikely orbit.

WR 134 is less than a degree away from WR 135 and the two are believed to lie at approximately the same distance from Earth within the Cygnus OB3 association. Both stars lie within a shell of hydrogen thought to have been swept up from the interstellar medium when one or both stars were on the main sequence. The shell is over forty parsecs wide and contains about 1,830 M☉ of hydrogen. It is unclear which of the two stars is primarily responsible for creating the shell.

The RGB stars were taken from an older picture from @Dark_Energy, many thanks.

Interpretation of data:
This interpretation reflects my unique perspective and understanding of the data we acquired from WR134. I find it incredibly satisfying to be able to interpret data independently which gives me a sense of control and ownership over the information, allowing me to make decisions based on my insights. I've put in a lot of effort to enhance my data interpretation skills over time. The satisfaction doesn't just come from the interpretation itself but also from the personal growth and development I've undergone in the process. Data interpretation can be a creative process, and I enjoy the challenge of synthesizing information and generating insights. Finding satisfaction in this creativity is personally rewarding. I am certain that not everyone may like the interpretation of WR134 presented here but during the process of coming to this image I made conscious decisions which ultimately concluded in the way I like it the most.