| {"id": 0, "knowledge": "Distance in Light-Years", "description": "Converts the distance of a celestial object from parsecs to light-years.", "definition": "Given the distance in parsecs ($D_{pc}$), the distance in light-years ($D_{ly}$) is calculated as: $D_{ly} = D_{pc} \\times 3.26156$", "type": "calculation_knowledge", "children_knowledge": -1} | |
| {"id": 1, "knowledge": "Planet Mass in Earth Units", "description": "Converts a planet's mass from Jupiter mass units to Earth mass units.", "definition": "Given a planet's mass in Jupiter masses ($M_J$), its mass in Earth masses ($M_E$) is: $M_E = M_J \\times 317.83$", "type": "calculation_knowledge", "children_knowledge": -1} | |
| {"id": 2, "knowledge": "Planet Radius in Earth Units", "description": "Converts a planet's radius from Jupiter radius units to Earth radius units.", "definition": "Given a planet's radius in Jupiter radii ($R_J$), its radius in Earth radii ($R_E$) is: $R_E = R_J \\times 11.209$", "type": "calculation_knowledge", "children_knowledge": -1} | |
| {"id": 3, "knowledge": "Stellar Luminosity", "description": "Calculates a star's luminosity relative to the Sun using its temperature and radius.", "definition": "Luminosity ($L_{\\star}$) relative to the Sun is estimated using the Stefan-Boltzmann law: $L_{\\star} = \\left( \\frac{R_{\\star}}{R_{\\odot}} \\right)^2 \\left( \\frac{T_{\\star}}{T_{\\odot}} \\right)^4$, where $R_{\\star}$ is the star's radius, $T_{\\star}$ is its effective temperature, and $T_{\\odot}$ is the Sun's effective temperature (~5778 K).", "type": "calculation_knowledge", "children_knowledge": -1} | |
| {"id": 4, "knowledge": "Planet Surface Gravity", "description": "Estimates the surface gravity of a planet relative to Earth's.", "definition": "The surface gravity ($g_p$) relative to Earth's is found by: $g_p = \\frac{M_E}{R_E^2}$, where $M_E$ is the planet's mass in Earth masses and $R_E$ is its radius in Earth radii. Depends on knowing the Planet Mass in Earth Units and Planet Radius in Earth Units.", "type": "calculation_knowledge", "children_knowledge": [1, 2]} | |
| {"id": 5, "knowledge": "Planetary Equilibrium Temperature", "description": "Estimates a planet's surface temperature based on the energy it receives from its star.", "definition": "The equilibrium temperature ($T_{eq}$) of a planet is calculated as: $T_{eq} = T_{\\star} \\sqrt{\\frac{R_{\\star}}{2a}}$, where $T_{\\star}$ is the star's temperature, $R_{\\star}$ is the star's radius, and $a$ is the planet's semi-major axis.", "type": "calculation_knowledge", "children_knowledge": -1} | |
| {"id": 6, "knowledge": "Habitable Zone Inner Boundary", "description": "Calculates the inner edge of a star's habitable zone, where a planet would be too hot for liquid water.", "definition": "The inner boundary of the habitable zone ($r_i$) in AU is estimated based on the star's luminosity ($L_{\\star}$): $r_i \\approx \\sqrt{L_{\\star} / 1.1}$. This relies on the Stellar Luminosity.", "type": "calculation_knowledge", "children_knowledge": [3]} | |
| {"id": 7, "knowledge": "Habitable Zone Outer Boundary", "description": "Calculates the outer edge of a star's habitable zone, where a planet would be too cold for liquid water.", "definition": "The outer boundary of the habitable zone ($r_o$) in AU is estimated based on the star's luminosity ($L_{\\star}$): $r_o \\approx \\sqrt{L_{\\star} / 0.53}$. This relies on the Stellar Luminosity.", "type": "calculation_knowledge", "children_knowledge": [3]} | |
| {"id": 8, "knowledge": "Relative Uncertainty", "description": "Measures the precision of a measurement as a percentage of the measured value.", "definition": "For a value $v$ with positive error $e_1$ and negative error $e_2$, the relative uncertainty ($U_{rel}$) is: $U_{rel} = \\frac{(e_1 - e_2) / 2}{v} \\times 100\\%$", "type": "calculation_knowledge", "children_knowledge": -1} | |
| {"id": 9, "knowledge": "Transit Depth", "description": "Calculates the fractional drop in a star's brightness when a planet passes in front of it.", "definition": "The transit depth ($Delta F$) is the ratio of the planet's surface area to the star's: $Delta F = \\left( \\frac{R_p}{R_{\\star}} \\right)^2$, where $R_p$ is the planet's radius and $R_{\\star}$ is the star's radius.", "type": "calculation_knowledge", "children_knowledge": -1} | |
| {"id": 10, "knowledge": "Planet Escape Velocity", "description": "Calculates the minimum speed needed for an object to escape a planet's gravitational pull.", "definition": "The escape velocity ($v_e$) is calculated as: $v_e = \\sqrt{\\frac{2GM_p}{R_p}}$, where $M_p$ and $R_p$ are the planet's mass and radius, and G is the gravitational constant. The calculation depends on Planet Mass in Earth Units and Planet Radius in Earth Units, converted to standard units.", "type": "calculation_knowledge", "children_knowledge": [1, 2]} | |
| {"id": 11, "knowledge": "Orbital Velocity", "description": "Calculates the average speed of a planet as it orbits its host star.", "definition": "Assuming a circular orbit, the orbital velocity ($v_{orb}$) is: $v_{orb} = \\sqrt{\\frac{GM_{\\star}}{a}}$, where $M_{\\star}$ is the mass of the star and $a$ is the semi-major axis.", "type": "calculation_knowledge", "children_knowledge": -1} | |
| {"id": 12, "knowledge": "Stellar Density", "description": "Calculates the average density of a star.", "definition": "The average density of a star ($\\rho_{\\star}$) is its mass divided by its volume: $\\rho_{\\star} = \\frac{M_{\\star}}{\\frac{4}{3}\\pi R_{\\star}^3}$, where $M_{\\star}$ and $R_{\\star}$ are the star's mass and radius.", "type": "calculation_knowledge", "children_knowledge": -1} | |
| {"id": 13, "knowledge": "Hertzsprung-Russell (HR) Diagram Position", "description": "Determines a star's position on the HR diagram based on its temperature and luminosity.", "definition": "The position is a coordinate pair ($T_{\\star}$, $L_{\\star}$) where $T_{\\star}$ is the star's effective temperature and $L_{\\star}$ is its calculated Stellar Luminosity.", "type": "calculation_knowledge", "children_knowledge": [3]} | |
| {"id": 14, "knowledge": "Goldilocks Value", "description": "Quantifies how centered a planet is within its star's habitable zone.", "definition": "A Goldilocks Value ($G$) can be defined as: $G = \\frac{a - r_i}{r_o - r_i}$, where $a$ is the planet's semi-major axis, and $r_i$ and $r_o$ are the Habitable Zone Inner Boundary and Outer Boundary. A value of 0.5 is perfectly centered.", "type": "calculation_knowledge", "children_knowledge": [6, 7]} | |
| {"id": 15, "knowledge": "Kepler's Third Law Verification", "description": "Uses a planet's orbital properties to calculate the mass of its host star.", "definition": "The mass of the star ($M_{\\star}$) in solar masses can be derived from Kepler's Third Law: $M_{\\star} = \\frac{a^3}{P^2}$, where $a$ is the semi-major axis in AU and $P$ is the orbital period in years.", "type": "calculation_knowledge", "children_knowledge": -1} | |
| {"id": 16, "knowledge": "Mass-Radius Relationship", "description": "A simple ratio to compare a planet's mass and size.", "definition": "A basic mass-radius ratio ($MRR$) can be expressed as: $MRR = \\frac{M_E}{R_E}$, which depends on the Planet Mass in Earth Units and Planet Radius in Earth Units.", "type": "calculation_knowledge", "children_knowledge": [1, 2]} | |
| {"id": 17, "knowledge": "Orbital Period Ratio", "description": "Calculates the ratio of the orbital periods of two adjacent planets in a system.", "definition": "For two planets, an outer planet with period $P_{out}$ and an inner planet with period $P_{in}$, the ratio is: $R_{period} = \\frac{P_{out}}{P_{in}}$.", "type": "calculation_knowledge", "children_knowledge": -1} | |
| {"id": 18, "knowledge": "Planet-Star Mass Ratio", "description": "Calculates the ratio of a planet's mass to its host star's mass.", "definition": "The mass ratio ($q$) is: $q = \\frac{M_p}{M_{\\star}}$, where $M_p$ is the planet's mass and $M_{\\star}$ is the star's mass. Both must be in the same units.", "type": "calculation_knowledge", "children_knowledge": -1} | |
| {"id": 19, "knowledge": "Gravitational Parameter (μ)", "description": "Calculates the standard gravitational parameter for a star, a constant used in orbital mechanics.", "definition": "The standard gravitational parameter is $\\mu = G M_{\\star}$, where G is the gravitational constant and $M_{\\star}$ is the mass of the star.", "type": "calculation_knowledge", "children_knowledge": -1} | |
| {"id": 20, "knowledge": "Gas Giant Planet", "description": "A large planet composed primarily of gases like hydrogen and helium.", "definition": "A planet with a mass greater than 0.1 Jupiter masses.", "type": "domain_knowledge", "children_knowledge": -1} | |
| {"id": 21, "knowledge": "Rocky Planet", "description": "A planet composed primarily of rock or metals, with a solid surface.", "definition": "A planet with a bulk density greater than 3 g/cm³.", "type": "domain_knowledge", "children_knowledge": -1} | |
| {"id": 22, "knowledge": "Short-Period Planet", "description": "A planet that orbits its host star in a very short amount of time.", "definition": "A planet with an orbital period of less than 10 days.", "type": "domain_knowledge", "children_knowledge": -1} | |
| {"id": 23, "knowledge": "Hot Jupiter", "description": "A class of exoplanets that are physically similar to Jupiter but orbit very close to their stars.", "definition": "A planet that is classified as both a Gas Giant Planet and a Short-Period Planet.", "type": "domain_knowledge", "children_knowledge": [20, 22]} | |
| {"id": 24, "knowledge": "Super-Earth", "description": "A class of planets with masses higher than Earth's but substantially below those of the solar system's ice giants.", "definition": "A planet that is likely a Rocky Planet and has a mass between 1 and 10 Earth masses. This depends on the Planet Mass in Earth Units.", "type": "domain_knowledge", "children_knowledge": [1, 21]} | |
| {"id": 25, "knowledge": "Planet in Habitable Zone", "description": "A planet orbiting within a star's habitable zone, where conditions might be right for liquid water.", "definition": "A planet whose semi-major axis ($a$) falls between the Habitable Zone Inner Boundary ($r_i$) and the Habitable Zone Outer Boundary ($r_o$).", "type": "domain_knowledge", "children_knowledge": [6, 7]} | |
| {"id": 26, "knowledge": "Potentially Habitable Exoplanet", "description": "An exoplanet that has the potential to support life, typically meaning it is rocky and in the habitable zone.", "definition": "A planet that is classified as a Rocky Planet and is also a Planet in Habitable Zone.", "type": "domain_knowledge", "children_knowledge": [21, 25]} | |
| {"id": 27, "knowledge": "High Eccentricity Planet", "description": "A planet with a highly elliptical orbit, leading to significant temperature variations.", "definition": "A planet with an orbital eccentricity greater than 0.25.", "type": "domain_knowledge", "children_knowledge": -1} | |
| {"id": 28, "knowledge": "Multi-planetary System", "description": "A star that hosts more than one confirmed planet.", "definition": "Any star system with a total number of confirmed planetary companions greater than 1.", "type": "domain_knowledge", "children_knowledge": -1} | |
| {"id": 29, "knowledge": "High-Precision Measurement", "description": "Indicates that a specific physical or orbital parameter is known with a high degree of confidence.", "definition": "A parameter for which the calculated Relative Uncertainty is less than 5%.", "type": "domain_knowledge", "children_knowledge": [8]} | |
| {"id": 30, "knowledge": "Well-Characterized Planet", "description": "A planet for which the key parameters of mass, radius, and period are known with high precision.", "definition": "A planet where the measurements for mass, radius, and orbital period are all considered High-Precision Measurements.", "type": "domain_knowledge", "children_knowledge": [29]} | |
| {"id": 31, "knowledge": "Retrograde Orbit", "description": "A planet that orbits its star in the opposite direction to the star's rotation.", "definition": "A planet with an orbital inclination greater than 90 degrees.", "type": "domain_knowledge", "children_knowledge": -1} | |
| {"id": 32, "knowledge": "Inflated Gas Giant", "description": "A gas giant planet with a radius that is unexpectedly large for its mass, suggesting a high internal temperature.", "definition": "A Gas Giant Planet with a bulk density less than 0.5 g/cm³.", "type": "domain_knowledge", "children_knowledge": [20]} | |
| {"id": 33, "knowledge": "Compact System", "description": "A planetary system where multiple planets orbit very close to each other.", "definition": "A Multi-planetary System where the Orbital Period Ratio between all adjacent pairs of planets is less than 3.", "type": "domain_knowledge", "children_knowledge": [17, 28]} | |
| {"id": 34, "knowledge": "Minimum Mass Status", "description": "Indicates that the provided mass for a planet is a lower limit, not the true mass.", "definition": "A flag indicating that the planet's mass was determined using a method (like radial velocity) that measures the minimum mass ($M \\sin i$) because the orbital inclination is unknown.", "type": "domain_knowledge", "children_knowledge": -1} | |
| {"id": 35, "knowledge": "Upper Limit Value", "description": "Indicates that a measured value for a parameter is not an exact measurement but an upper boundary.", "definition": "A quality flag on a parameter signifying that its true value is less than or equal to the stated value.", "type": "domain_knowledge", "children_knowledge": -1} | |
| {"id": 36, "knowledge": "Discovery via Transit Method", "description": "Identifies a planet discovered by observing the dimming of its star as the planet passes in front.", "definition": "A planet whose discovery method is listed as Transit, TR, Transit Method, Photometry, or Photometric.", "type": "domain_knowledge", "children_knowledge": -1} | |
| {"id": 37, "knowledge": "Discovery via Radial Velocity", "description": "Identifies a planet discovered by observing the wobble of its star caused by the planet's gravitational pull.", "definition": "A planet whose discovery method is listed as RadVel, RV, RV Method, Radial Velocity, or Doppler.", "type": "domain_knowledge", "children_knowledge": -1} | |
| {"id": 38, "knowledge": "Blended Measurement", "description": "Indicates a parameter measurement (like brightness or temperature) is potentially contaminated by the light of nearby, unresolved stars.", "definition": "A quality flag indicating that a measurement's value is affected by light from stellar companions, potentially reducing its accuracy.", "type": "domain_knowledge", "children_knowledge": -1} | |
| {"id": 39, "knowledge": "Kepler Mission Discovery", "description": "Identifies a planet discovered by the Kepler Space Telescope.", "definition": "A planet whose observation record is linked to the 'kep' facility.", "type": "domain_knowledge", "children_knowledge": -1} | |
| {"id": 40, "knowledge": "Stellar Distance Value", "description": "Illustrates the value for the distance to a star system.", "definition": "Measured in parsecs (pc), where 1 parsec equals about 3.26 light-years. Values range from nearby stars like Proxima Centauri (~1.3 pc) to stars thousands of parsecs away.", "type": "value_illustration", "children_knowledge": -1} | |
| {"id": 41, "knowledge": "Apparent Magnitude Value", "description": "Illustrates the value for a star's brightness as seen from Earth.", "definition": "This is a logarithmic scale where smaller numbers are brighter. A magnitude of 1.0 is 100 times brighter than a magnitude of 6.0. The brightest stars have negative magnitudes (e.g., Sirius is -1.46).", "type": "value_illustration", "children_knowledge": -1} | |
| {"id": 42, "knowledge": "Stellar Temperature Value", "description": "Illustrates the value for a star's effective surface temperature.", "definition": "Measured in Kelvin (K). Cool red dwarfs can be around 3,000 K, a Sun-like star is about 5,800 K, and very hot blue stars can exceed 30,000 K.", "type": "value_illustration", "children_knowledge": -1} | |
| {"id": 43, "knowledge": "Stellar Mass Value", "description": "Illustrates the value for a star's mass.", "definition": "Measured in solar masses ($M_{\\odot}$), where 1 is the mass of our Sun. Most known host stars range from low-mass red dwarfs (~0.1 $M_{\\odot}$) to stars several times more massive than the Sun.", "type": "value_illustration", "children_knowledge": -1} | |
| {"id": 44, "knowledge": "Stellar Radius Value", "description": "Illustrates the value for a star's radius.", "definition": "Measured in solar radii ($R_{\\odot}$), where 1 is the radius of our Sun. Values range from small neutron stars to giant stars like Betelgeuse, which would extend beyond the orbit of Mars if in our solar system.", "type": "value_illustration", "children_knowledge": -1} | |
| {"id": 45, "knowledge": "Orbital Period Value", "description": "Illustrates the value for the time a planet takes to complete one orbit around its star.", "definition": "Measured in days. 'Hot Jupiters' can have periods of only a few days, while planets in very distant orbits can have periods of many thousands of years.", "type": "value_illustration", "children_knowledge": -1} | |
| {"id": 46, "knowledge": "Orbital Eccentricity Value", "description": "Illustrates the value describing how much an orbit deviates from a perfect circle.", "definition": "A dimensionless value from 0 to <1. An eccentricity of 0 is a perfect circle. A value of 0.1 indicates a slightly elliptical orbit, while a value of 0.7 indicates a very elongated, comet-like orbit.", "type": "value_illustration", "children_knowledge": -1} | |
| {"id": 47, "knowledge": "Planet Mass Value", "description": "Illustrates the value for a planet's mass.", "definition": "Typically measured in Jupiter masses ($M_J$). Earth's mass is about 0.003 $M_J$. Known exoplanets range from less than Earth's mass to over 20 times the mass of Jupiter.", "type": "value_illustration", "children_knowledge": -1} | |
| {"id": 48, "knowledge": "Planet Radius Value", "description": "Illustrates the value for a planet's physical size.", "definition": "Typically measured in Jupiter radii ($R_J$). Earth's radius is about 0.09 $R_J$. Planets range from small rocky worlds smaller than Earth to 'inflated' gas giants larger than Jupiter.", "type": "value_illustration", "children_knowledge": -1} | |
| {"id": 49, "knowledge": "Planet Density Value", "description": "Illustrates the value for a planet's bulk density.", "definition": "Measured in grams per cubic centimeter (g/cm³). Puffy gas giants can have densities less than water (<1 g/cm³), while dense, rocky planets like Earth have densities around 5.5 g/cm³.", "type": "value_illustration", "children_knowledge": -1} | |
| {"id": 50, "knowledge": "Transit Timing Variation (TTV) Method", "description": "A method of exoplanet detection that infers the presence of planets by observing variations in the timing of a known transiting planet's transit across its star.", "definition": "A planet whose observation record is linked to the 'ttv' facility.", "type": "domain_knowledge", "children_knowledge": -1} | |
| {"id": 51, "knowledge": "Discovery Method Standardization", "description": "Standardizes various text entries for exoplanet discovery methods into a set of unified categories.", "definition": "A process that groups different raw discovery method labels from the database into a clear, standardized set. The standard categories and their corresponding raw labels are: 'Radial Velocity' (includes 'RadVel', 'RV', 'RV Method', 'Radial Velocity', 'Doppler'), 'Transit' (includes 'Transit', 'TR', 'Transit Method', 'Photometry', 'Photometric'), 'Imaging' (includes 'Direct Imaging', 'DI', 'Imaging', 'IMG', 'Direct'), 'TTV' (includes 'TTV', 'Transit Timing Variations', 'Transit Timing', 'TTV Method', 'Timing Var'), 'Microlensing' (includes 'Microlensing', 'ML', '\\u03bcLens', 'Lensing', 'Gravitational'). Any method not in these groups is classified as 'Other'.", "type": "domain_knowledge", "children_knowledge": [36, 37, 50]} |