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dark-matter-expert

Expert-level dark matter physics covering observational evidence, candidate particles, detection methods, structure formation, and alternative gravity theories.

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luokai0/ai-agent-skills-by-luo-kai

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Dark Matter Expert

Before Starting

  1. Particle physics or astrophysics perspective?
  2. Detection method? Direct, indirect, or collider?
  3. Specific candidate particle?

Core Expertise Areas

Evidence for Dark Matter

Galaxy rotation curves: flat curves require mass beyond visible disk. Gravitational lensing: mass inferred from light bending exceeds visible mass. Bullet Cluster: separation of X-ray gas from lensing mass in cluster collision. CMB: acoustic peaks encode dark matter to baryon ratio. Structure formation: CDM model successfully predicts large-scale structure.

Candidate Particles

WIMPs: 10 GeV to 10 TeV mass, weak interaction cross section, thermal relic. Axions: ultralight, motivated by strong CP problem, cavity experiments. Sterile neutrinos: right-handed neutrinos mixing with active neutrinos. Primordial black holes: formed in early universe, constrained but not ruled out. FIMPs: feebly interacting massive particles, freeze-in production mechanism.

Detection Methods

Direct detection: nuclear recoil in underground detectors, LUX, XENONnT, PandaX. Indirect detection: annihilation or decay products, gamma rays, neutrinos, positrons. Collider production: missing energy signatures at LHC, monojet events. Astronomical: perturbations to stellar streams, substructure in galaxy halos.

Alternative Theories

MOND: modified Newtonian dynamics, acceleration-dependent force law. MOND success: fits galaxy rotation curves with one free parameter. MOND failure: galaxy clusters require additional dark matter even with MOND. TeVeS: relativistic MOND extension, difficulties with CMB and gravitational waves.

Best Practices

  • Consider full range of mass scales for dark matter candidates
  • Account for astrophysical uncertainties in direct detection limits
  • Distinguish robust evidence from model-dependent claims
  • Use model-independent approaches where possible

Common Pitfalls

PitfallFix
WIMP-centric viewMany viable candidates exist at different mass scales
Ignoring local density uncertaintyDirect detection rates depend on local DM density
Dismissing MOND entirelyExplains individual galaxies well, fails at cluster scale
Confusing exclusion limits with detectionNull result sets upper limit only

Related Skills

  • cosmology-expert
  • astrophysics-expert
  • physics/particle-physics-expert

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