Sun

A small blue sun belonging to a class of relatively common dwarf stars that are often planet-bearing or accompanied by planetary dust clouds. Many stars of this kind rotate quickly and the class is known for strong hydrogen and ionized metal lines in stellar spectroscopy.

This small blue star of the unusual A0 classification has been gravitationally captured by a black hole, and is slowly orbiting closer and closer to its eventual merger with the mass singularity. This event will take place many years in the future but the effects of orbiting in the vicinity of a black hole are already being felt in the form of intense and volatile gravitational tidal forces exerted by the singularity. As the star is within the outer edges of the matter accretion disc of the black hole, the instability is further contributed to by the fluctuations in mass density within the clouds of dust, gas, and other matter. The local system environment here is harsh and unforgiving to say the least.

This small blue star has been disrupted by forces apparently unleashed by experimental stellar transmuter technology directed at its heart. Following an extreme stellar event, the star is now in a highly-energetic state and emitting increased radiation as it is wracked by massive coronal flare activity. A small blue sun belonging to a class of relatively common dwarf stars that are often planet-bearing or accompanied by planetary dust clouds. Many stars of this kind rotate quickly and the class is known for strong hydrogen and ionized metal lines in stellar spectroscopy.

This star was originally a small blue sun of a star class of critical interest to the Triglavian Collective. Manipulation of this star by a Triglavian Dazh Porevitium Transmuter has caused profound changes in this stellar body, and throughout the system surrounding it. More typical members of this star class of relatively common dwarf stars are often planet-bearing or accompanied by planetary dust clouds. Many stars of this kind rotate quickly and the class is known for strong hydrogen and ionized metal lines in stellar spectroscopy.

A bright blue stellar body emitting unusually high neutrino levels, this star experiences frequent coronal mass ejections at unpredictable intervals. The turbulent subgiants of this type found in New Eden are prone to violent instability that scientists now believe is linked to unstable wormhole activity and the "Caroline's Star" stellar anomaly.

This luminous blue star belongs to a class known for powerful stellar winds and rapid rotation. These stars generate most of their energy at the center of their mass in a thermonuclear fusion process involving a carbon-nitrogen-oxygen (CNO) catalytic cycle. Stars of this type generally show strong non-ionized helium lines and some have a chemistry that results in very strong lines, leading to the designation 'helium-strong'.

This luminous blue star belongs to a class known for powerful stellar winds and rapid rotation. These stars generate most of their energy at the center of their mass in a thermonuclear fusion process involving a carbon-nitrogen-oxygen (CNO) catalytic cycle. Stars of this type generally show strong non-ionized helium lines and some have a chemistry that results in very strong lines, leading to the designation 'helium-strong'.

This luminous blue star belongs to a class known for powerful stellar winds and rapid rotation. These stars generate most of their energy at the center of their mass in a thermonuclear fusion process involving a carbon-nitrogen-oxygen (CNO) catalytic cycle. Stars of this type generally show strong non-ionized helium lines and some have a chemistry that results in very strong lines, leading to the designation 'helium-strong'.

This was originally a luminous blue star of a class of deep interest to the Triglavian Collective. Manipulation of this star by a Triglavian Dazh Porevitium Transmuter has caused profound changes in this stellar body, and throughout the system surrounding it. More typical members of this star class are known for powerful stellar winds and rapid rotation. These stars generate most of their energy at the center of their mass in a thermonuclear fusion process involving a carbon-nitrogen-oxygen (CNO) catalytic cycle. Stars of this type generally show strong non-ionized helium lines and some have a chemistry that results in very strong lines, leading to the designation 'helium-strong'.

This was originally a luminous blue star of a class of deep interest to the Triglavian Collective. Manipulation of this star by a Triglavian Dazh Porevitium Transmuter has caused profound changes in this stellar body, and throughout the system surrounding it. More typical members of this star class are known for powerful stellar winds and rapid rotation. These stars generate most of their energy at the center of their mass in a thermonuclear fusion process involving a carbon-nitrogen-oxygen (CNO) catalytic cycle. Stars of this type generally show strong non-ionized helium lines and some have a chemistry that results in very strong lines, leading to the designation 'helium-strong'.

This was originally a luminous blue star of a class of deep interest to the Triglavian Collective. Manipulation of this star by a Triglavian Dazh Porevitium Transmuter has caused profound changes in this stellar body, and throughout the system surrounding it. More typical members of this star class are known for powerful stellar winds and rapid rotation. These stars generate most of their energy at the center of their mass in a thermonuclear fusion process involving a carbon-nitrogen-oxygen (CNO) catalytic cycle. Stars of this type generally show strong non-ionized helium lines and some have a chemistry that results in very strong lines, leading to the designation 'helium-strong'.

This small white star is largely made up of degenerate matter and is slowly cooling, having ceased thermonuclear fusion after exhausting its fuel. The temperature of these stars is generally uniform through the body due to the excellent thermal conduction of degenerate electrons making up the bulk of their mass. High surface gravity leads to separation and purification of elements in these stars such that, while generally composed mostly of carbon and oxygen, the atmosphere is rich in lighter elements.

This small white star is largely made up of degenerate matter and is slowly cooling, having ceased thermonuclear fusion after exhausting its fuel. The temperature of these stars is generally uniform through the body due to the excellent thermal conduction of degenerate electrons making up the bulk of their mass. High surface gravity leads to separation and purification of elements in these stars such that, while generally composed mostly of carbon and oxygen, the atmosphere is rich in lighter elements.

A main-sequence star in a class of stellar bodies that are typically white or yellow-white in hue. Hydrogen fusion drives the energy generation of these stars and they are often hot and bright. Stars of this type can be found with companion stars, are often accompanied by mature planetary systems and tend to emit an ultraviolet radiation flux providing for habitable zones conducive to human occupation.

A main-sequence star in a class of stellar bodies that are typically white or yellow-white in hue. Hydrogen fusion drives the energy generation of these stars and they are often hot and bright. Stars of this type can be found with companion stars, are often accompanied by mature planetary systems and tend to emit an ultraviolet radiation flux providing for habitable zones conducive to human occupation.

Small, red-white stars of this kind are relatively old and may be on the verge of exhausting their hydrogen fusion fuel before becoming red giants. Planetary systems can often be found around these stars and an abundance of heavier metals is not uncommon.

Small, red-white stars of this kind are relatively old and may be on the verge of exhausting their hydrogen fusion fuel before becoming red giants. Planetary systems can often be found around these stars and an abundance of heavier metals is not uncommon.

This was originally a main-sequence yellow star that attracted the interest of the Triglavian Collective. Manipulation of this star by a Triglavian Dazh Porevitium Transmuter has caused profound changes in this stellar body, and throughout the system surrounding it. More typical members of this star class are often yellow or yellow-orange in hue, generating and emitting energy from the vast hydrogen fusion process within the heart of the star. Various numbers of planets of the terrestrial and gas giant types are found around these stars and the habitable zones often contain one or more planets.

This was originally a main-sequence yellow star that attracted the interest of the Triglavian Collective. Manipulation of this star by a Triglavian Dazh Porevitium Transmuter has caused profound changes in this stellar body, and throughout the system surrounding it. More typical members of this star class are often yellow or yellow-orange in hue, generating and emitting energy from the vast hydrogen fusion process within the heart of the star. Various numbers of planets of the terrestrial and gas giant types are found around these stars and the habitable zones often contain one or more planets.

Main-sequence stars of this kind can have a slight red-white tint and are generally bright and in the process of fusing vast quantities of hydrogen every second. Various numbers of planets of the terrestrial and gas giant types are found around these stars and the habitable zones often contain one or more planets.

Main-sequence stars of this kind can have a slight red-white tint and are generally bright and in the process of fusing vast quantities of hydrogen every second. Various numbers of planets of the terrestrial and gas giant types are found around these stars and the habitable zones often contain one or more planets.

A main-sequence stellar body of a class that is often yellow or yellow-orange in hue, generating and emitting energy from the vast hydrogen fusion process within the heart of the star. Various numbers of planets of the terrestrial and gas giant types are found around these stars and the habitable zones often contain one or more planets.

A main-sequence stellar body of a class that is often yellow or yellow-orange in hue, generating and emitting energy from the vast hydrogen fusion process within the heart of the star. Various numbers of planets of the terrestrial and gas giant types are found around these stars and the habitable zones often contain one or more planets.

A main-sequence stellar body of a class that is often yellow or yellow-orange in hue, generating and emitting energy from the vast hydrogen fusion process within the heart of the star. Various numbers of planets of the terrestrial and gas giant types are found around these stars and the habitable zones often contain one or more planets.

Rather small but on the main-sequence, these yellow or yellow-orange stars are very stable, remaining on the main-sequence for tens of billions of years. Abundant compared to other classes that tend to support habitable planetary systems, these stars are common targets for colonization efforts. The stability of these stars, combined with the relatively low ultraviolet radiation flux they emit, is thought to enhance the viability of their planetary systems for the development of life.

Rather small but on the main-sequence, these yellow or yellow-orange stars are very stable, remaining on the main-sequence for tens of billions of years. Abundant compared to other classes that tend to support habitable planetary systems, these stars are common targets for colonization efforts. The stability of these stars, combined with the relatively low ultraviolet radiation flux they emit, is thought to enhance the viability of their planetary systems for the development of life.

A bright orange star that is relatively cool but stable, being of a class that typically runs a fusion process on the main-sequence for as long as 30 billion years. Planetary systems containing an abundance of heavier metals and relatively complex molecular products have been noted as present around such stars. These stable stars, emitting relatively gentle levels of ultraviolet radiation, are common targets for scientific expeditions looking for life or colonization survey teams seeking viable planets within their comfortable habitable zones.

A bright orange star that is relatively cool but stable, being of a class that typically runs a fusion process on the main-sequence for as long as 30 billion years. Planetary systems containing an abundance of heavier metals and relatively complex molecular products have been noted as present around such stars. These stable stars, emitting relatively gentle levels of ultraviolet radiation, are common targets for scientific expeditions looking for life or colonization survey teams seeking viable planets within their comfortable habitable zones.

This large red star has exhausted its core hydrogen fuel and is slowly expanding into a red giant, consuming all remaining hydrogen in the stellar shell. While the process of expansion into a full red giant will take hundreds of millions of years, eventually the star will engulf any planetary system orbiting close to it.

This large red star has exhausted its core hydrogen fuel and is slowly expanding into a red giant, consuming all remaining hydrogen in the stellar shell. While the process of expansion into a full red giant will take hundreds of millions of years, eventually the star will engulf any planetary system orbiting close to it.

Yellow-orange and orange stars of this type are rather stable and believed to take tens of billions of years to burn through their core hydrogen reserves in a process of thermonuclear fusion. This stability and long life, combined with the common presence of planetary systems marks these as viable candidates for colonization and exploration efforts.

Yellow-orange and orange stars of this type are rather stable and believed to take tens of billions of years to burn through their core hydrogen reserves in a process of thermonuclear fusion. This stability and long life, combined with the common presence of planetary systems marks these as viable candidates for colonization and exploration efforts.

Yellow-orange and orange stars of this type are rather stable and believed to take tens of billions of years to burn through their core hydrogen reserves in a process of thermonuclear fusion. This stability and long life, combined with the common presence of planetary systems marks these as viable candidates for colonization and exploration efforts.

Orange and red-orange stars in this class are very abundant, making up by far the largest number of main-sequence stars in the locale of the New Eden cluster. However, many such stars are dim and in the dwarf category with the more radiant members of the class being the better known. Rather cool and experiencing constant remixing of their hydrogen fuel by convection, it is believed that stars of this kind could potentially remain stable, at constant luminosity, for trillions of years. By this scale, all stars of this kind are young in terms of their potential lifetime due to the relatively short age of the universe.

Orange and red-orange stars in this class are very abundant, making up by far the largest number of main-sequence stars in the locale of the New Eden cluster. However, many such stars are dim and in the dwarf category with the more radiant members of the class being the better known. Rather cool and experiencing constant remixing of their hydrogen fuel by convection, it is believed that stars of this kind could potentially remain stable, at constant luminosity, for trillions of years. By this scale, all stars of this kind are young in terms of their potential lifetime due to the relatively short age of the universe.

Orange and red-orange stars in this class are very abundant, making up by far the largest number of main-sequence stars in the locale of the New Eden cluster. However, many such stars are dim and in the dwarf category with the more radiant members of the class being the better known. Rather cool and experiencing constant remixing of their hydrogen fuel by convection, it is believed that stars of this kind could potentially remain stable, at constant luminosity, for trillions of years. By this scale, all stars of this kind are young in terms of their potential lifetime due to the relatively short age of the universe.

A hot, luminous and blue stellar body belonging to a relatively rare class of main-sequence stars. Often large and massive, these stars very quickly burn through their core hydrogen fuel supply and therefore have short lifetimes on the main sequence. These stars emit a tremendous amount of ultraviolet radiation and the largest among them will typically go nova after only a few million years. Smaller stars of this type can cool sufficiently that they will turn into rapidly-rotating stars dominated by carbon-nitrogen-oxygen (CNO) cycle nuclear fusion.

This was originally a luminous blue stellar body of a star class of considerable interest to the Triglavian Collective. Manipulation of this star by a Triglavian Dazh Porevitium Transmuter has caused profound changes in this stellar body, and throughout the system surrounding it. More typical members of this relatively rare class of main-sequence stars are often large and massive. Such stars very quickly burn through their core hydrogen fuel supply and therefore have short lifetimes on the main sequence. These stars emit a tremendous amount of ultraviolet radiation and the largest among them will typically go nova after only a few million years. Smaller stars of this type can cool sufficiently that they will turn into rapidly-rotating stars dominated by carbon-nitrogen-oxygen (CNO) cycle nuclear fusion.