Characteristic Polynomial
Also known as: Secular equation · Eigenvalue equation
To find a matrix's eigenvalues — the special scaling factors along which it merely stretches vectors — you ask when A−λI collapses a direction to zero, i.e. when its determinant vanishes. That determinant, as a function of λ, is the characteristic polynomial. Its roots are the eigenvalues. Physicists call it the 'secular equation' because it first arose computing slow (secular) perturbations of planetary orbits. Its coefficients encode invariants: the trace and determinant of A.
Eigenvalues are where det(A−λI) crosses zero; the curve slides as the sweep parameter moves.
Equivalent forms
One polynomial packages every eigenvalue, and its coefficients are exactly the rotation-invariant quantities (trace, determinant) of the matrix.
Where it holds
Dimensional analysis
The 'secular equation' appeared in 18th-century celestial mechanics (Lagrange, Laplace) analyzing long-term orbital stability. Cauchy (1829) proved real symmetric matrices have real eigenvalues. The Cayley–Hamilton theorem (1858) later showed every matrix satisfies its own characteristic polynomial.
- Normal modes and resonant frequencies of coupled oscillators
- Quantum energy levels from a Hamiltonian matrix
- Stability analysis of dynamical systems (eigenvalue signs)
- Coefficients alternate with the elementary symmetric functions of eigenvalues, not arbitrary numbers
- Algebraic multiplicity (root order) can exceed geometric multiplicity (eigenvectors)
- Computing it via cofactor expansion is numerically unstable — use QR iteration in practice
What if…
All roots are real and eigenvectors are orthogonal — the spectral theorem, why observables in QM are Hermitian.
The eigenvalue is repeated; there may be fewer independent eigenvectors, signalling a defective (non-diagonalizable) matrix.
2×2 eigenvalues
- , 3 (trace ,