{"query": "Helium (He) — element 2", "count": 20, "results": [{"id": "card_ref_el_002", "title": "Helium (He) — element 2", "shelf": "chemistry", "surface": "secular", "snippet": "Atomic number 2. Symbol He. Standard atomic weight 4.002602. The helium atom carries 2 protons in its nucleus; its place in the periodic table is fixed by that count. Verified reference data.", "authority_tier": "reference", "source": "Verified reference — chemistry", "readable": false, "generated": false}, {"id": "card_theory_stellar_nucleosynthesis_the_hr_diagram", "title": "Stellar nucleosynthesis & the HR diagram", "shelf": "theories", "surface": "secular", "snippet": "Stellar nucleosynthesis & the HR diagram — an engine domain that can touch it: astronomy. Calibration: partial — specific relations verify; the theory as a whole is not a sealable computation. Where t", "authority_tier": "reference", "source": "The Theory Assay — calibrated, not judged (docs/THEORY_CATALOG.md)", "readable": false, "generated": false}, {"id": "card_theory_spectroscopy", "title": "Spectroscopy (how we know what a distant thing is made of)", "shelf": "theories", "surface": "secular", "snippet": "Spectroscopy (how we know what a distant thing is made of) — an engine domain that can touch it: optics. Calibration: seals — wavelengths, Doppler shifts and Wien's law all recompute and check. Split ", "authority_tier": "reference", "source": "The Theory Assay — calibrated, not judged (docs/THEORY_CATALOG.md)", "readable": false, "generated": false}, {"id": "card_n_0fd6d5654d74", "title": "Binding energy — the mass that glue costs", "shelf": "science", "surface": "secular", "snippet": "Weigh a nucleus and it comes up LIGHT: the missing mass is the binding energy,\nE = mc². Sealed: the deuteron (one proton + one neutron) is short 2.224 MeV — the first\nrung of the strong force — and he", "authority_tier": "engine_derived", "source": "Concordance assay — 2026-07-09", "readable": false, "generated": false}, {"id": "card_bridge_theory_spectroscopy__periodic_law", "title": "Bridge: Spectroscopy (how we know what a distant thing is made of)  ↔  Periodic law (Mendeleev)", "shelf": "bridges", "surface": "secular", "snippet": "Spectroscopy (how we know what a distant thing is made of) and Periodic law (Mendeleev) are the same form in different domains. two independent fingerprints of the same underlying fact. Mendeleev sort", "authority_tier": "reference", "source": "The Bridges — cross-domain isomorphisms", "readable": false, "generated": false}, {"id": "card_n_bbecbbc24fb6", "title": "The nucleus — the strongest glue and the slowest clocks", "shelf": "science", "surface": "secular", "snippet": "Past gamma rays the spectrum ends and the nucleus itself begins. One chain,\neight steps, sealed — four of them IN-DOMAIN by the nuclear fleet: https://narrowhighway.com/s/8a5e89ab13bc499f39240c64360d9", "authority_tier": "engine_derived", "source": "Concordance assay — 2026-07-09", "readable": false, "generated": false}, {"id": "card_n_cda0b1e1a364", "title": "Fusion — why the stars shine", "shelf": "science", "surface": "secular", "snippet": "Four hydrogens weigh more than one helium; the difference is sunlight. Sealed from\nthe measured masses: 4·m(H) − m(He-4) = 0.0287 u → 26.73 MeV per helium forged: https://narrowhighway.com/s/8a5e89ab1", "authority_tier": "engine_derived", "source": "Concordance assay — 2026-07-09", "readable": false, "generated": false}, {"id": "card_c_82914d8d0b24", "title": "Fusion — why the stars shine ↔ The nucleus — the strongest glue and the slo", "shelf": "connections", "surface": null, "snippet": "4·m(H) − m(He-4) = 0.0287 u → 26.73 MeV per helium forged ... the ENERGY seals from the mass tables; the RATE ... is quantum tunnelling through the Coulomb wall  — a concord the card itself states; mi", "authority_tier": "engine_derived", "source": "Concordance miner — 2026-07-11", "readable": false, "generated": false}, {"id": "card_src_openstax_chemistry_18_12_occurrence_preparation_and_propert_15b0d34d", "title": "18.12 Occurrence, Preparation, and Properties of the Noble Gases — Chemistry", "shelf": "chemistry", "surface": "secular", "snippet": "18.12\n\nOccurrence, Preparation, and Properties of the Noble Gases\n\nLearning ObjectivesBy the end of this section, you will be able to:\n\nDescribe the properties, preparation, and uses of the noble gase", "authority_tier": "reference", "source": "OpenStax: Chemistry (CC-BY 4.0)", "readable": false, "generated": false}, {"id": "card_src_openstax_chemistry_2e_18_12_occurrence_preparation_and_propert_06383b4a", "title": "18.12 Occurrence, Preparation, and Properties of the Noble Gases — Chemistry 2e", "shelf": "chemistry", "surface": "secular", "snippet": "18.12\n\nOccurrence, Preparation, and Properties of the Noble Gases\n\nLearning Objectives\nBy the end of this section, you will be able to:\n\nDescribe the properties, preparation, and uses of the noble gas", "authority_tier": "reference", "source": "OpenStax: Chemistry 2e (CC-BY 4.0)", "readable": false, "generated": false}, {"id": "card_src_openstax_chemistry_atoms_first_18_12_occurrence_preparation_and_propert_15b0d34d", "title": "18.12 Occurrence, Preparation, and Properties of the Noble Gases — Chemistry: Atoms First", "shelf": "chemistry", "surface": "secular", "snippet": "18.12\n\nOccurrence, Preparation, and Properties of the Noble Gases\n\nLearning ObjectivesBy the end of this section, you will be able to:\n\nDescribe the properties, preparation, and uses of the noble gase", "authority_tier": "reference", "source": "OpenStax: Chemistry: Atoms First (CC-BY 4.0)", "readable": false, "generated": false}, {"id": "card_src_openstax_chemistry_atoms_first_2e_18_12_occurrence_preparation_and_propert_06383b4a", "title": "18.12 Occurrence, Preparation, and Properties of the Noble Gases — Chemistry: Atoms First 2e", "shelf": "chemistry", "surface": "secular", "snippet": "18.12\n\nOccurrence, Preparation, and Properties of the Noble Gases\n\nLearning Objectives\nBy the end of this section, you will be able to:\n\nDescribe the properties, preparation, and uses of the noble gas", "authority_tier": "reference", "source": "OpenStax: Chemistry: Atoms First 2e (CC-BY 4.0)", "readable": false, "generated": false}, {"id": "card_src_fed_nasa_techdoc_19700032874", "title": "Provisional thermodynamic functions for helium 4 for temperatures from 2 to 1500 K with pressures to 100 MN/m2 /1000 atmospheres)", "shelf": "science", "surface": "secular", "snippet": "Provisional thermodynamic functions for helium 4 for temperatures from 2 to 1500 K with pressures to 100 MN/m2 /1000 atmospheres). A United States federal publication, public domain (17 USC 105). The ", "authority_tier": "reference", "source": "NASA technical documents (PD, 17 USC 105)", "readable": true, "generated": false}, {"id": "card_src_openstax_astronomy_2e_22_5_the_evolution_of_more_massive_stars_a75aea70", "title": "22.5 The Evolution of More Massive Stars — Astronomy 2e", "shelf": "astronomy", "surface": "secular", "snippet": "22.5\n\nThe Evolution of More Massive Stars\n\nLearning Objectives\n\nBy the end of this section, you will be able to:\n\nExplain how and why massive stars evolve much more rapidly than lower-mass stars like ", "authority_tier": "reference", "source": "OpenStax: Astronomy 2e (CC-BY 4.0)", "readable": false, "generated": false}, {"id": "card_src_openstax_astronomy_22_5_the_evolution_of_more_massive_stars_a75aea70", "title": "22.5 The Evolution of More Massive Stars — Astronomy", "shelf": "astronomy", "surface": "secular", "snippet": "22.5\n\nThe Evolution of More Massive Stars\n\nLearning Objectives\n\nBy the end of this section, you will be able to:\n\nExplain how and why massive stars evolve much more rapidly than lower-mass stars like ", "authority_tier": "reference", "source": "OpenStax: Astronomy (CC-BY 4.0)", "readable": false, "generated": false}, {"id": "card_src_openstax_astronomy_25_5_stellar_populations_in_the_galaxy_42d678ee", "title": "25.5 Stellar Populations in the Galaxy — Astronomy", "shelf": "astronomy", "surface": "secular", "snippet": "25.5\n\nStellar Populations in the Galaxy\n\nLearning Objectives\n\nBy the end of this section, you will be able to:\n\nDistinguish between population I and population II stars according to their locations, m", "authority_tier": "reference", "source": "OpenStax: Astronomy (CC-BY 4.0)", "readable": false, "generated": false}, {"id": "card_src_openstax_astronomy_2e_25_5_stellar_populations_in_the_galaxy_42d678ee", "title": "25.5 Stellar Populations in the Galaxy — Astronomy 2e", "shelf": "astronomy", "surface": "secular", "snippet": "25.5\n\nStellar Populations in the Galaxy\n\nLearning Objectives\n\nBy the end of this section, you will be able to:\n\nDistinguish between population I and population II stars according to their locations, m", "authority_tier": "reference", "source": "OpenStax: Astronomy 2e (CC-BY 4.0)", "readable": false, "generated": false}, {"id": "card_src_openstax_astronomy_2e_7_2_composition_and_structure_of_planets_89bccab6", "title": "7.2 Composition and Structure of Planets — Astronomy 2e", "shelf": "astronomy", "surface": "secular", "snippet": "7.2\n\nComposition and Structure of Planets\n\nLearning Objectives\n\nBy the end of this section, you will be able to:\n\nDescribe the characteristics of the giant planets, terrestrial planets, and small bodi", "authority_tier": "reference", "source": "OpenStax: Astronomy 2e (CC-BY 4.0)", "readable": false, "generated": false}, {"id": "card_src_openstax_astronomy_7_2_composition_and_structure_of_planets_89bccab6", "title": "7.2 Composition and Structure of Planets — Astronomy", "shelf": "astronomy", "surface": "secular", "snippet": "7.2\n\nComposition and Structure of Planets\n\nLearning Objectives\n\nBy the end of this section, you will be able to:\n\nDescribe the characteristics of the giant planets, terrestrial planets, and small bodi", "authority_tier": "reference", "source": "OpenStax: Astronomy (CC-BY 4.0)", "readable": false, "generated": false}, {"id": "card_src_etym_helium", "title": "helium", "shelf": "etymology", "surface": "secular", "snippet": "helium: etymology (Webster 1913) — n.: [NL., fr. Gr. (Chem.) Defn: A gaseous element found in the atmospheres of the sun and earth and in some rare minerals.]. From Webster's Revised Unabridged Dictio", "authority_tier": "reference", "source": "Webster's Revised Unabridged Dictionary (1913), Project Gutenberg eBook #29765 — public domain", "readable": true, "generated": false}], "house": {"door": "FIND", "kind": "cards", "trail": "results", "seal": null, "next_step": {"do": "open the top card", "door": "FIND", "tool": "card_get", "params": {"id": "card_ref_el_002"}}, "ends": "a verdict or a card · the trail · a seal · one next step"}}