Porrima
| Porrima | |
|---|---|
| File:Porrima.jpg | |
| Information | |
| Number | 30 |
| Level | 30 |
| Spectral Class | F0 |
| Catalogue ID | GL 482A |
| Temperature | 7500K |
| Mass | 1.55SM |
| Radius | 972700 |
| Magnitude | 2.40 |
| Planets # | 6 |
| Moons # | 15 |
| Planets | Porrima I, Porrima II, Porrima III, Porrima IV, Porrima V, Porrima VI |
| Moons | Porrima I-a, Porrima I-b, Porrima II-a, Porrima II-b, Porrima II-c, Porrima III-a, Porrima III-b, Porrima IV-a, Porrima IV-b, Porrima IV-c, Porrima IV-d, Porrima V-a, Porrima V-b, Porrima V-c, Porrima VI-a |
| Description | ?????? |
| Points of Interest | Red Mile |
| Notable Resources | Ne, Cs |
| Exists IRL | Yes |
| Patch | 1.0 |
Porrima is a level 30 Star System with 6 Planets and 15 Moons.
Planets and Moons
Description
Additional Information
Real Life Information
Porrima, also known as Gamma Virginis, is a real binary star system located in the constellation of Virgo. It is one of the few binary systems that can be resolved into individual stars with small telescopes. The system is approximately 38.7 light-years away from Earth.
Overview
Porrima, named after an ancient Roman goddess, is a binary star system consisting of two almost identical main-sequence stars, both of which are of spectral type F0V. The two stars are so similar in size, mass, and brightness that they are often referred to as twins. The system is also known by its Bayer designation, Gamma Virginis, and its Flamsteed designation, 29 Virginis.
The two stars of Porrima orbit each other in a nearly circular orbit, with a period of about 169 years. The system's orbit is inclined at an angle of about 2 degrees to the line of sight from Earth, which means that the two stars periodically eclipse each other as seen from Earth. These eclipses, known as mutual events, provide valuable opportunities for astronomers to study the system and its stars in detail.
Observational History
Porrima has been known to astronomers since ancient times, and its binary nature was first recognized in 1836 by the English astronomer John Herschel. The system was a popular target for early astronomers, who used it to test and refine their telescopes and observational techniques.
In the 20th century, Porrima was the subject of intensive study by astronomers using a variety of techniques, including spectroscopy, photometry, and interferometry. These studies have provided a wealth of information about the system and its stars, including their masses, sizes, temperatures, and chemical compositions.
Physical Properties
The two stars of Porrima are both slightly larger and more massive than the Sun. They have nearly identical masses of about 1.1 solar masses, and their radii are about 1.4 times that of the Sun. Their surface temperatures are about 7000 Kelvin, which is hotter than the Sun's surface temperature of about 5500 Kelvin. This gives them a spectral type of F0V, which means that they are slightly hotter and more massive than the Sun.
The stars of Porrima are also slightly metal-poor compared to the Sun, with a metallicity of about 80% of the solar value. This suggests that they are somewhat older than the Sun, with an estimated age of about 3 billion years.
Future Evolution
The future evolution of the Porrima system is uncertain, but it is likely that the two stars will continue to orbit each other for many billions of years to come. Eventually, as they exhaust their nuclear fuel, they will evolve off the main sequence and become red giants. At this point, their mutual gravitational interaction may cause them to merge into a single star, or they may undergo a common envelope phase, in which one star engulfs the other.
In any case, the Porrima system provides a fascinating laboratory for astronomers to study the properties and evolution of binary stars. Its proximity to Earth and the relative ease with which its stars can be resolved make it a valuable target for ongoing and future observations.