{"section":"phenomena","label":"Objects & Phenomena","count":14,"generatedAt":"2026-03-20","items":[{"slug":"stars","path":"/phenomena/stars/","title":"Stars as Physical Systems: Mass & Equilibrium","description":"How stars operate as self-gravitating plasma spheres balanced by thermal pressure and sustained by core nuclear fusion across 0.08 to 150+ solar masses.","questionOrTopic":"How does a star function as a self-regulating physical system?","epistemicStatus":"strong-observational-evidence","formula":"L = 4π R² σ_SB T_eff⁴; L / L_☉ ≈ (M / M_☉)^α (α ≈ 3.5 for 0.5 < M/M_☉ < 20)","keyMetricsCount":4,"sources":["src:gaia-dr3","src:hipparcos-new","src:simbad-cds"]},{"slug":"brown-dwarfs","path":"/phenomena/brown-dwarfs/","title":"Brown Dwarfs: Substellar L, T & Y Objects","description":"Why brown dwarfs (13 to 80 Jupiter masses) halt contraction via electron degeneracy before sustaining hydrogen fusion, cooling through L, T, and Y types.","questionOrTopic":"Why do brown dwarfs fail to become main-sequence stars and how do they evolve?","epistemicStatus":"strong-observational-evidence","formula":"P_deg ∝ ρ^{5/3} ⇒ R ∝ M^{−1/3} (competing with Coulomb attraction to keep R ≈ 1 R_Jup)","keyMetricsCount":4,"sources":["src:jwst-archive","src:gaia-dr3","src:simbad-cds"]},{"slug":"white-dwarfs","path":"/phenomena/white-dwarfs/","title":"White Dwarfs & the Chandrasekhar Limit","description":"How electron-degenerate white dwarfs pack a solar mass into an Earth-sized carbon-oxygen core, why higher mass shrinks their radius, and the 1.44 M☉ limit.","questionOrTopic":"How does quantum electron degeneracy support a white dwarf and why is there a maximum mass limit?","epistemicStatus":"strong-observational-evidence","formula":"R_WD ∝ μ_e^{−5/3} M_WD^{−1/3}; M_Ch = (ω_3^0 √(3π) / 2) (ℏ c / G)^{3/2} (1 / (μ_e m_H))² ≈ 1.44 M_☉","keyMetricsCount":4,"sources":["src:gaia-dr3","src:hipparcos-new","src:simbad-cds"]},{"slug":"neutron-stars","path":"/phenomena/neutron-stars/","title":"Neutron Stars: Nuclear Matter & TOV Limit","description":"How core collapse compresses 1.2–2.2 solar masses into a 12 km sphere of superfluid neutrons and nuclear pasta, bounded by the Tolman-Oppenheimer-Volkoff limit.","questionOrTopic":"What is the internal structure of a neutron star and what holds it up against collapse?","epistemicStatus":"strong-observational-evidence","formula":"dP / dr = −[G m(r) ρ(r) / r²] [1 + P / (ρ c²)] [1 + 4π r³ P / (m c²)] [1 − 2 G m(r) / (r c²)]^{−1}","keyMetricsCount":4,"sources":["src:gwtc-3","src:simbad-cds","src:ngc-ic-steinicke"]},{"slug":"pulsars","path":"/phenomena/pulsars/","title":"Pulsars: Magnetospheres & Precision Timing","description":"How rapidly spinning magnetized neutron stars emit coherent lighthouse beams, spin down via magnetic dipole radiation, and act as cosmic clocks.","questionOrTopic":"How do pulsars generate periodic pulses and how do astronomers use their spin-down rates?","epistemicStatus":"strong-observational-evidence","formula":"τ_c = P / (2 Ṗ); B_surf ≈ 3.2 × 10^{19} √(P · Ṗ) Gauss (for I = 10^{45} g cm², R = 10 km)","keyMetricsCount":4,"sources":["src:simbad-cds","src:ngc-ic-steinicke","src:gwtc-3"]},{"slug":"magnetars","path":"/phenomena/magnetars/","title":"Magnetars: Extreme Fields & Fast Radio Bursts","description":"How magnetars generate 10^14–10^15 Gauss magnetic fields above the quantum electrodynamic critical threshold, powering giant X-ray flares and FRBs.","questionOrTopic":"What makes a magnetar different from an ordinary radio pulsar?","epistemicStatus":"standard-model-consensus","formula":"B_QED = (m_e² c³) / (e ℏ) = 4.414 × 10^{13} G; E_mag ≈ (B² / 8π) (4π R³ / 3) ≈ 2 × 10^{47} (B / 10^{15} G)² erg","keyMetricsCount":4,"sources":["src:simbad-cds","src:gwtc-3"]},{"slug":"black-holes","path":"/phenomena/black-holes/","title":"Black Holes: Horizons, Kerr Spin & Shadows","description":"How general relativity defines Schwarzschild and Kerr black holes, photon spheres, ISCO accretion efficiency, and horizon-scale shadows.","questionOrTopic":"How do black holes curve spacetime and how do astronomers observe them across mass scales?","epistemicStatus":"strong-observational-evidence","formula":"R_s = 2 G M / c²; R_+ = (G M / c²) [1 + √(1 − a_*²)]; θ_shadow ≈ (2 √27 G M) / (c² D)","keyMetricsCount":4,"sources":["src:eht-m87-sgra","src:gwtc-3","src:simbad-cds"]},{"slug":"planetary-systems","path":"/phenomena/planetary-systems/","title":"Planetary Systems & Exoplanet Architectures","description":"How planetary systems are organized around stars: terrestrial planets, super-Earths, sub-Neptunes, hot Jupiters, resonant chains, and habitable zones.","questionOrTopic":"What types of exoplanets and orbital architectures exist across the Milky Way?","epistemicStatus":"strong-observational-evidence","formula":"T_eq = T_★ √(R_★ / (2 a)) (1 − A_B)^{1/4}; ρ_p = (3 M_p) / (4π R_p³) = ρ_⊕ (M_p / M_⊕) / (R_p / R_⊕)³","keyMetricsCount":4,"sources":["src:nasa-exoplanet-archive","src:jwst-archive","src:jpl-horizons"]},{"slug":"nebulae","path":"/phenomena/nebulae/","title":"Nebulae: H II Regions, Planetary & Dark Clouds","description":"Why astronomical nebulae belong to distinct physical classes: star-forming H II regions, reflection clouds, planetary nebulae, and supernova remnants.","questionOrTopic":"How do the different types of astronomical nebulae form and emit light?","epistemicStatus":"strong-observational-evidence","formula":"R_S = [ (3 Q(H^0)) / (4π α_B(T) n_e n_p) ]^{1/3}","keyMetricsCount":4,"sources":["src:ngc-ic-steinicke","src:jwst-archive","src:simbad-cds"]},{"slug":"star-clusters","path":"/phenomena/star-clusters/","title":"Star Clusters: Open vs. Globular Laboratories","description":"Why open and globular star clusters serve as natural laboratories for stellar evolution, two-body relaxation dynamics, and galactic archaeology.","questionOrTopic":"How do open clusters and globular clusters differ and why are they vital for testing stellar physics?","epistemicStatus":"strong-observational-evidence","formula":"t_relax ≈ (0.14 N) / (ln(0.4 N)) × √(r_h³ / (G M_cluster)); r_tidal = R_gal (M_cluster / (3 M_gal))^{1/3}","keyMetricsCount":4,"sources":["src:harris-globulars","src:gaia-dr3","src:ngc-ic-steinicke"]},{"slug":"galaxies","path":"/phenomena/galaxies/","title":"Galaxies: Disks, Bulges, Halos & Scaling Laws","description":"How galaxies operate as gravitationally bound ecosystems of stars, multiphase gas, central supermassive black holes, and extended dark matter halos.","questionOrTopic":"How are galaxies structured and why do they obey tight empirical scaling relations?","epistemicStatus":"strong-observational-evidence","formula":"v_circ(r) = √(G M(2 s), and how relativistic Γ > 100 jets solve the compactness problem.","questionOrTopic":"What powers cosmological gamma-ray bursts and why do they require ultra-relativistic jets?","epistemicStatus":"strong-observational-evidence","formula":"R_emission ≈ 2 Γ² c Δt_var / (1 + z); E_true = E_iso (1 − cos θ_jet) ≈ (θ_jet² / 2) E_iso","keyMetricsCount":4,"sources":["src:gwtc-3","src:simbad-cds"]}]}