Project Details

Awards & Nominations

Logic11 has received the following awards and nominations. Way to go!

Global Nominee

The Challenge | Build a Planet

Your challenge is to create a game that will allow players to customize the characteristics of a star and design planets that could reasonably exist in that star system. Ensure that this game provides an educational experience for players!

X Space Game

we create a game that will allow players to customize the characteristics of a star and design planets that could reasonably exist in that star system. But the player must explore first about the space and master the character of the star and planets.

Logic11

X Space Website

X SPACE GAME

THE GAME

The game allows players to make its own solar system by customizing the characteristics of a star and design planets. The challenges for them is to create the planets that could exist in that star system by orbiting the star they have customized and also to make the planets for harbor life. This game will improve player's knowledge about the space that are waiting to be discovered

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OBJECTIVE

  • Players can experience the feeling making other solar system
  • Players can learn more about the universe by themselves
  • Other way to study about space without using books
  • Gain new information anytime, anywhere

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BENEFITS

  • Educational game
  • Attracts students to learn more about the space
  • Help players to study more efficient
  • Release players' tension
  • Suitable for all ages

INFORMATION

Grab some knowledge here before you start :-

our solar system

THE STARS

YELLOW DWARF STARS

  • Lifetime: 4 - 17 billion years
  • Evolution: early, middle
  • Temperature: 5,000 - 7,300 °C
  • Spectral Types: G, F
  • Luminosity: 0.6 - 5.0
  • Radius: 0.96 - 1.4
  • Mass: 0.8 - 1.4
  • Prevalence: 10%

The Sun, Alpha Centauri A, and Kepler-22 are yellow dwarfs. These stellar cauldrons are in the prime of their lives because they are burning hydrogen fuel in their cores. This normal functioning places them on the `main sequence', where the majority of stars are found. The designation `yellow dwarf' may be imprecise, as these stars typically have a whiter color. However, they do appear yellow when observed through the Earth's atmosphere.

ORANGE DWARF STARS

  • Lifetime: 17 - 73 billion years
  • Evolution: early, middle
  • Temperature: 3,500 - 5,000 °C
  • Spectral Types: K
  • Luminosity: 0.08 - 0.6
  • Radius: 0.7 - 0.96
  • Mass: 0.45 - 0.8
  • Prevalence: 11%

Alpha Centauri B and Epsilon Eridani are orange dwarf stars. These are smaller, cooler, and live longer than yellow dwarfs like our Sun. Like their larger counterparts, they are main sequence stars fusing hydrogen in their cores.

RED DWARF STARS

  • Lifetime: 73 - 5500 billion years
  • Evolution: early, middle
  • Temperature: 1,800 - 3,500 °C
  • Spectral Types: M
  • Luminosity: 0.0001 - 0.08
  • Radius: 0.12 - 0.7
  • Mass: 0.08 - 0.45
  • Prevalence: 73%

Proxima Centauri, Barnard's Star and Gliese 581 are all red dwarfs. They are the smallest kind of main sequence star. Red dwarfs are barely hot enough to maintain the nuclear fusion reactions required to use their hydrogen fuel. However, they are the most common type of star, owing to their remarkably long lifetime that exceeds the current age of the universe (13.8 billion years). This is due to a slow rate of fusion, and an efficient circulation of hydrogen fuel via convective heat transport.

BROWN DWARFS

  • Lifetime: unknown (long)
  • Evolution: not evolving
  • Temperature: 0 - 1,800 °C
  • Spectral Types: L, T, Y (after M)
  • Luminosity: ~0.00001
  • Radius: 0.06 - 0.12
  • Mass: 0.01 - 0.08
  • Prevalence: unknown (many)

Brown dwarfs are substellar objects that never accumulated enough material to become stars. They are too small to generate the heat required for hydrogen fusion. Brown Dwarfs constitute the midpoint between the smallest red dwarf stars and massive planets like Jupiter. They are the same size as Jupiter, but to qualify as a brown dwarf, they must be at least 13 times heavier. Their cold exteriors emit radiation beyond the red region of the spectrum, and to the human observer they appear magenta rather than brown. As brown dwarfs gradually cool, they become difficult to identify, and it is unclear how many exist.

BLUE GIANT STARS

  • Lifetime: 3 - 4,000 million years
  • Evolution: early, middle
  • Temperature: 7,300 - 200,000 °C
  • Spectral Types: O, B, A
  • Luminosity: 5.0 - 9,000,000
  • Radius: 1.4 - 250
  • Mass: 1.4 - 265
  • Prevalence: 0.7%

Blue giants are defined here as large stars with at least a slight blueish coloration, although definitions do vary. A broad definition has been chosen because only about 0.7% of stars fall into this category.

Not all blue giants are main sequence stars. Indeed, the largest and hottest (O-type) burn through the hydrogen in their cores very quickly, causing their outer layers to expand and their luminosity to increase. Their high temperature means they remain blue for much of this expansion (e.g. Rigel), but eventually they may cool to become a red giant, supergiant or hypergiant.

Blue supergiants above about 30 solar masses can begin throw off huge swathes of their outer layers, exposing a super hot and luminous core. These are called Wolf-Rayet stars. These massive stars are more likely to explode in a supernova before they can cool to reach a later evolutionary stage, such as a red supergiant. After a supernova, the stellar remnant becomes a neutron star or a black hole.

RED GIANT STARS

  • Lifetime: 0.1 - 2 billion years
  • Evolution: late
  • Temperature: 3,000 - 5,000 °C
  • Spectral Types: M, K
  • Luminosity: 100 - 1000
  • Radius: 20 - 100
  • Mass: 0.3 - 10
  • Prevalence: 0.4%

Aldebaran and Arcturus are red giants. These stars are in a late evolutionary phase. Red giants would previously have been main sequence stars (such as the Sun) with between 0.3 and 10 solar masses. Smaller stars do not become red giants because, due to convective heat transport, their cores cannot become dense enough to generate the heat needed for expansion. Larger stars become red supergiants or hypergiants.

In red giants, the accumulation of helium (from hydrogen fusion) causes a contraction of the core that raises the internal temperature. This triggers hydrogen fusion in the outer layers of the star, causing it to grow in size and luminosity. Due to a larger surface area, the surface temperature is actually lower (redder). They eventually eject their outer layers to form a planetary nebula, while the core becomes a white dwarf.

RED SUPERGIANT STARS

  • Lifetime: 3 - 100 million years
  • Evolution: late
  • Temperature: 3,000 - 5,000 ºC
  • Spectral Types: K, M
  • Luminosity: 1,000 - 800,000
  • Radius: 100 - 1650
  • Mass: 10 - 40
  • Prevalence: 0.0001%

Betelgeuse and Antares are red supergiants. The largest of these types of stars are called red hypergiants. One of these is 1650 times the size of our Sun (NML Cygni), and is the largest known star in the universe. NML Cygni is 5,300 light years away from the Earth.

Like red giants, these stars have swelled up due to the contraction of their cores, however, they typically evolve from blue giants and supergiants with between 10 and 40 solar masses. Higher mass stars shed their layers too quickly, becoming Wolf-Rayet stars, or exploding in supernovae. Red supergiants eventually destroy themselves in a supernova, leaving behind a neutron star or black hole.

WHITE DWARFS

  • Lifetime: 1015- 1025 years
  • Evolution: dead, cooling
  • Temperature: 4,000 - 150,000 ºC
  • Spectral Types: D (degenerate)
  • Luminosity: 0.0001 - 100
  • Radius: 0.008 - 0.2
  • Mass: 0.1 - 1.4
  • Prevalence: 4%

Stars less than 10 solar masses will shed their outer layers to form planetary nebulae. They will typically leave behind an Earth-sized core of less than 1.4 solar masses. This core will be so dense that the electrons within its volume will be prevented from occupying any smaller region of space (becoming degenerate). This physical law (Pauli's exclusion principle) prevents the stellar remnant from collapsing any further.

The remnant is called a white dwarf, and examples include Sirius B and Van Maanen's star. More than 97% of stars are theorized to become white dwarfs. These super hot structures will remain hot for trillions of years before cooling to become black dwarfs.

BLACK DWARFS

  • Lifetime: unknown (long)
  • Evolution: dead
  • Temperature: < -270 °C
  • Spectral Types: none
  • Luminosity: infinitesimal
  • Radius: 0.008 - 0.2
  • Mass: 0.1 - 1.4
  • Prevalence: ~0%

Once a star has become a white dwarf, it will slowly cool to become a black dwarf. As the universe is not old enough for a white dwarf to have cooled sufficiently, no black dwarfs are thought to exist at this time.

NEUTRON STARS

  • Lifetime: unknown (long)
  • Evolution: dead, cooling
  • Temperature: < 2,000,000 ºC
  • Spectral Types: D (degenerate)
  • Luminosity: ~0.000001
  • Radius: 5 - 15 km
  • Mass: 1.4 - 3.2
  • Prevalence: 0.7%

When stars larger than about 10 solar masses exhaust their fuel, their cores dramatically collapse to form neutron stars. If the core has a mass above 1.4 solar masses, electron degeneracy will be unable to halt the collapse. Instead, the electrons will fuse with protons to produce neutral particles called neutrons, which are compressed until they can no longer occupy a smaller space (becoming degenerate).

The collapse throws off the outer layers of the star in a supernova explosion. The stellar remnant, composed almost entirely of neutrons, is so dense that it occupies a radius of about 12 km. Due to conservation of angular momentum, neutron stars are often left in a rapidly rotating state called a pulsar.

Stars larger than 40 solar masses with cores larger than about 2.5 solar masses are likely to become black holes instead of neutron stars. For a black hole to form, the density must become great enough to overcome neutron degeneracy, causing a collapse into a gravitational singularity.

While stellar classification is more precisely described in terms of spectral type, this does very little to fire the imagination of those who will become the next generation of astrophysicists. There are many different types of stars in the universe, and it's no surprise that those with the most exotic sounding names receive the greatest levels of attention.

WHAT IS AN ORBIT?

An orbit is a regular, repeating path that one object in space takes around another one. An object in an orbit is called a satellite. A satellite can be natural, like Earth or the moon. Many planets have moons that orbit them. A satellite can also be man-made, like the International Space Station.

Planets, comets, asteroids and other objects in the solar system orbit the sun. Most of the objects orbiting the sun move along or close to an imaginary flat surface. This imaginary surface is called the ecliptic plane.

WHAT SHAPE IS AN ORBIT?

Orbits come in different shapes. All orbits are elliptical, which means they are an ellipse, similar to an oval. For the planets, the orbits are almost circular. The orbits of comets have a different shape. They are highly eccentric or "squashed." They look more like thin ellipses than circles.

Satellites that orbit Earth, including the moon, do not always stay the same distance from Earth. Sometimes they are closer, and at other times they are farther away. The closest point a satellite comes to Earth is called its perigee. The farthest point is the apogee. For planets, the point in their orbit closest to the sun is perihelion. The farthest point is called aphelion. Earth reaches its aphelion during summer in the Northern Hemisphere. The time it takes a satellite to make one full orbit is called its period. For example, Earth has an orbital period of one year. The inclination is the angle the orbital plane makes when compared with Earth's equator.

HOW DO OBJECTS STAY IN ORBIT?

An object in motion will stay in motion unless something pushes or pulls on it. This statement is called Newton's first law of motion. Without gravity, an Earth-orbiting satellite would go off into space along a straight line. With gravity, it is pulled back toward Earth. A constant tug-of-war takes place between the satellite's tendency to move in a straight line, or momentum, and the tug of gravity pulling the satellite back.

An object's momentum and the force of gravity have to be balanced for an orbit to happen. If the forward momentum of one object is too great, it will speed past and not enter into orbit. If momentum is too small, the object will be pulled down and crash. When these forces are balanced, the object is always falling toward the planet, but because it's moving sideways fast enough, it never hits the planet. Orbital velocity is the speed needed to stay in orbit. At an altitude of 150 miles (242 kilometers) above Earth, orbital velocity is about 17,000 miles per hour. Satellites that have higher orbits have slower orbital velocities.

WHERE DO SATELLITES ORBIT EARTH?

The International Space Station is in low Earth orbit, or LEO. LEO is the first 100 to 200 miles (161 to 322 km) of space. LEO is the easiest orbit to get to and stay in. One complete orbit in LEO takes about 90 minutes.

Satellites that stay above a location on Earth are in geosynchronous Earth orbit, or GEO. These satellites orbit about 23,000 miles (37,015 km) above the equator and complete one revolution around Earth precisely every 24 hours. Satellites headed for GEO first go to an elliptical orbit with an apogee about 37,015 km. Firing the rocket engines at apogee then makes the orbit round. Geosynchronous orbits are also called geostationary.

Any satellite with an orbital path going over or near the poles maintains a polar orbit. Polar orbits are usually low Earth orbits. Eventually, Earth's entire surface passes under a satellite in polar orbit. When a satellite orbits Earth, the path it takes makes an angle with the equator. This angle is called the inclination. A satellite that orbits parallel to the equator has a zero-degree orbital inclination. A satellite in a polar orbit has a 90-degree inclination.

Words to Know

ellipse: A flattened circle or oval.

orbital plane: An imaginary, gigantic flat plate containing an Earth satellite's orbit. The orbital plane passes through the center of Earth.

momentum: The mass of an object multiplied by its velocity.

parallel: Extending in the same direction, everywhere equidistant, and not meeting.

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