| [ |
| { |
| "id": "pulsar", |
| "name": "Pulsar", |
| "body_type": "neutron_star", |
| "one_line": "A pulsar is a rapidly rotating neutron star whose magnetic poles sweep beams of radiation across space.", |
| "facts": [ |
| "Neutron stars are the collapsed cores left behind by some massive stars after supernova explosions.", |
| "A pulsar's radio, X-ray, or gamma-ray pulses are seen when its beam crosses Earth's line of sight.", |
| "Pulsars can rotate from a few times per second to hundreds of times per second.", |
| "The pulses are extremely regular, which makes some pulsars useful as precise cosmic clocks." |
| ], |
| "visual_cues": { |
| "primary_color": "#8fd7ff", |
| "secondary_color": "#f7fbff", |
| "emissive": 1.6, |
| "beam": true |
| } |
| }, |
| { |
| "id": "red_giant", |
| "name": "Red Giant", |
| "body_type": "star", |
| "one_line": "A red giant is an aging star that has expanded after exhausting hydrogen fuel in its core.", |
| "facts": [ |
| "As the core contracts, hydrogen fusion continues in a shell around it and the outer layers swell.", |
| "Red giants are cooler at their surfaces than Sun-like main-sequence stars, so they appear orange or red.", |
| "The Sun is expected to become a red giant late in its life cycle.", |
| "Strong stellar winds from red giants can seed nearby space with heavier elements." |
| ], |
| "visual_cues": { |
| "primary_color": "#ff9b5f", |
| "secondary_color": "#ffd0a3", |
| "emissive": 0.9, |
| "beam": false |
| } |
| }, |
| { |
| "id": "white_dwarf", |
| "name": "White Dwarf", |
| "body_type": "stellar_remnant", |
| "one_line": "A white dwarf is the dense, hot remnant core of a low- or medium-mass star.", |
| "facts": [ |
| "White dwarfs no longer sustain normal fusion in their cores.", |
| "A typical white dwarf packs roughly a Sun-like mass into an Earth-sized volume.", |
| "They slowly cool over enormous spans of time by radiating stored thermal energy.", |
| "In some binary systems, material falling onto a white dwarf can trigger nova outbursts." |
| ], |
| "visual_cues": { |
| "primary_color": "#d7edff", |
| "secondary_color": "#ffffff", |
| "emissive": 1.2, |
| "beam": false |
| } |
| }, |
| { |
| "id": "accretion_disk", |
| "name": "Black Hole Accretion Disk", |
| "body_type": "black_hole", |
| "one_line": "An accretion disk is a rotating disk of gas heated as it spirals around a compact object such as a black hole.", |
| "facts": [ |
| "Friction and magnetic turbulence in the disk convert orbital energy into heat and radiation.", |
| "The black hole itself emits no light, but nearby infalling matter can glow intensely.", |
| "Relativistic speeds near a black hole can distort the disk's apparent brightness and shape.", |
| "Some accreting black holes launch jets along their rotation axes." |
| ], |
| "visual_cues": { |
| "primary_color": "#ffd166", |
| "secondary_color": "#4cc9f0", |
| "emissive": 1.8, |
| "beam": false |
| } |
| }, |
| { |
| "id": "emission_nebula", |
| "name": "Emission Nebula", |
| "body_type": "nebula", |
| "one_line": "An emission nebula is a cloud of gas that glows after ultraviolet light from hot stars ionizes it.", |
| "facts": [ |
| "Ionized hydrogen often produces a red glow as electrons recombine with protons.", |
| "Many emission nebulae are active star-forming regions.", |
| "Dust mixed with the gas can absorb, scatter, and reshape the light we see.", |
| "Massive young stars can carve cavities and pillars into surrounding gas clouds." |
| ], |
| "visual_cues": { |
| "primary_color": "#ff4f8b", |
| "secondary_color": "#46e0c4", |
| "emissive": 0.7, |
| "beam": false |
| } |
| } |
| ] |
|
|
