High-Level Project Summary
The purpose of our game that created is to help people to learn about stellar variability in a fun way. Below are our game rules and the introductions to play:1. This game is suitable for all.2. This game is for 2 to 4 people to play. 3. Player starts from the nebula and upgrades to supernova by collecting HYDROGEN.4. Every step forward needs 3 HYDROGEN cards, 2 steps forward need 6 HYDROGEN cards, and so on.5. The chess piece that reaches the center point the faster wins. (Becomes a Supernova)
Link to Final Project
Link to Project "Demo"
Detailed Project Description
The purpose of our game that created is to help people to learn about stellar variability in a fun way. Below are our game rules and the introductions to play:
1. This game is suitable for beginners, children, adults, and so on.
2. This game is for 2 to 4 people to play. If there are 4 players, players can form a team, that is a group of 2 players.
3. Player gets the chess piece and dice and starts from the nebula and upgrades to supernova by collecting HYDROGEN.
4. To vote for "HYDROGEN", you need to take 3 HYDROGEN cards.
5. To vote for "OPPORTUNITY", you need to draw an OPPORTUNITY card, just depends on luck.
6. To vote for "PUNISHMENT", you need to draw a PUNISHMENT card and accept the corresponding punishment.
7. When the chess piece goes to the position with the symbol “?”, you need to draw a QUESTION Card then answer the question, and get the corresponding reward or punishment.
8. Players get HYDROGEN by rolling dice and quiz questions.
9. The cards’ content:
OPPORTUNITY CARD
Move forward (1 step)
Move forwards (3 steps)
Get 1 hydrogen
Get 3 hydrogens
Get one more chance to dice
Get 50% of the hydrogen that you have
Get the opportunity card one more time
Get a punishment card
PUNISHMENT CARD
You are safe
Divide the hydrogen and give it to the next player
Banned from throwing the dice for 1 round
Give your chance to the next player in the next round
Move backward (1 step)
Give 1 hydrogen to the next player
Give half of your hydrogen to the next player
Return to the starting point
QUESTION CARD
Example of stellar remnants?
What is the nearest star to our Earth?
What does the star need to burn in adulthood?
What does the hydrogen change into after burning?
What is stellar evolution?
Who predicted the existence of a black hole?
What is the end of the black draft?
What is the star?
10. Every step forward needs 3 HYDROGEN cards, 2 steps forward need 6 HYDROGEN cards and so on.
11. When level up, players need to return 3 HYDROGEN cards for every 1 step forward.
12. The chess piece that reaches the center point the faster wins. (Becomes a Supernova)
Space Agency Data
1. From https://en.wikipedia.org/wiki/Stellar_evolution
Stellar evolution is the process by which a star changes over the course of time. Depending on the mass of the star, its lifetime can range from a few million years for the most massive to trillions of years for the least massive, which is considerably longer than the age of the universe. The table shows the lifetimes of stars as a function of their masses. All stars are formed from collapsing clouds of gas and dust, often called nebulae or molecular clouds. Over the course of millions of years, these protostars settle down into a state of equilibrium, becoming what is known as a main-sequence star.
2. From https://en.wikipedia.org/wiki/Supernova_nucleosynthesis
Supernova nucleosynthesis is the nucleosynthesis of chemical elements in supernova explosions.
In sufficiently massive stars, the nucleosynthesis by fusion of lighter elements into heavier ones occurs during sequential hydrostatic burning processes called helium burning, carbon burning, oxygen burning, and silicon burning, in which the byproducts of one nuclear fuel become, after compressional heating, the fuel for the subsequent burning stage. In this context, the word "burning" refers to nuclear fusion and not a chemical reaction.
During hydrostatic burning these fuels synthesize overwhelmingly the alpha nuclides (A = 2Z), nuclei composed of integer numbers of helium-4 nuclei.[clarification needed] A rapid final explosive burning is caused by the sudden temperature spike owing to passage of the radially moving shock wave that was launched by the gravitational collapse of the core. W. D. Arnett and his Rice University colleagues demonstrated that the final shock burning would synthesize the non-alpha-nucleus isotopes more effectively than hydrostatic burning was able to do, suggesting that the expected shock-wave nucleosynthesis is an essential component of supernova nucleosynthesis. Together, shock-wave nucleosynthesis and hydrostatic-burning processes create most of the isotopes of the elements carbon (Z = 6), oxygen (Z = 8), and elements with Z = 10 to 28 (from neon to nickel). As a result of the ejection of the newly synthesized isotopes of the chemical elements by supernova explosions, their abundances steadily increased within interstellar gas. That increase became evident to astronomers from the initial abundances in newly born stars exceeding those in earlier-born stars.
Elements heavier than nickel are comparatively rare owing to the decline with atomic weight of their nuclear binding energies per nucleon, but they too are created in part within supernovae. Of greatest interest historically has been their synthesis by rapid capture of neutrons during the r-process, reflecting the common belief that supernova cores are likely to provide the necessary conditions. However, newer research has proposed a promising alternative (see the r-process below). The r-process isotopes are approximately 100,000 times less abundant than the primary chemical elements fused in supernova shells above. Furthermore, other nucleosynthesis processes in supernovae are thought to be responsible also for some nucleosynthesis of other heavy elements, notably, the proton capture process known as the rp-process, the slow capture of neutrons (s-process) in the helium-burning shells and in the carbon-burning shells of massive stars, and a photodisintegration process known as the γ-process (gamma-process). The latter synthesizes the lightest, most neutron-poor, isotopes of the elements heavier than iron from preexisting heavier isotopes.
Hackathon Journey
We feel very excited, because we love board games, so we try to learn about stellar evolution through games. The cooperation of teachers and parents and the cooperation of students are the factors that make us step by step towards success. In the future, we will continue to try various challenges, and we will strive to obtain various knowledge of astronomy and apply it to the details of life. Our group is committed to constantly updating and improving bugs, finding information, listening to each other's opinions, and having fun working together. We are most grateful to NASA SPACE APPS for the opportunity to participate in the competition, and also thank the teachers and parents for their encouragement.
References
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