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Heegaard Floer homology assigns groups $H{F}^{\circ }(Y,\mathfrak{s})$ to a closed oriented three-manifold with a Spin-c structure. A pointed Heegaard diagram of genus $g$ gives product Lagrangian tori ${\mathbb{T}}_{\alpha },{\mathbb{T}}_{\beta }\subset {\mathrm{Sym}}^g(\Sigma )$; the chain complex is generated by their intersection points and its differential counts Whitney disk classes represented by holomorphic disks. The minus, infinity, plus and hat versions use different powers or quotients of the variable $U$. The Heegaard Floer cobordism maps and the Mixed Heegaard Floer invariant relate these groups to smooth four-dimensional topology.

The least genus of a Heegaard surface among all Heegaard splittings of a closed orientable three-manifold. Having a splitting of genus $g$ only proves $g_H(M)\le g$; stabilization supplies larger-genus splittings of the same manifold.

Two nonseparating compressing disks on opposite sides with the same boundary form an embedded sphere. Cutting each handlebody along its disk leaves it connected, so the sphere is nonseparating in the glued three-manifold. Capping the two resulting sphere boundaries gives a splitting of one lower genus of the remaining summand; the removed summand is $S^1\times S^2$.

For ${\Phi }^a=f(r)x^a/r$ and $A_i^a={ϵ}_{iaj}{x}^j\alpha (r)$ with $[e_a,e_b]={ϵ}_{abc}{e}_c$, set $K=1+r^2\alpha$. The equation $B=-D\Phi$ equates radial coefficients to give $f^{\prime }=-2\alpha -r^2{\alpha }^2$ and transverse coefficients to give $r{\alpha }^{\prime }+2\alpha =-f/r-r\alpha f$. These are exactly the displayed two radial equations. The sign depends on the chosen orientation and on the order of indices in the gauge ansatz.

For a Bogomolny-Prasad-Sommerfield monopole, the dimensionless radial Bogomolny equations are $dK/d\rho =-KH$ and $dH/d\rho =(1-K^2)/{\rho }^2$. The displayed profiles solve both equations: differentiating $\rho /\sinh \rho$ gives $K(1/\rho -\coth \rho )=-KH$, while differentiating $H$ gives $1/{\rho }^2-{\mathrm{csch}}^2\rho =(1-K^2)/{\rho }^2$. At the origin $K=1-{\rho }^2/6+O({\rho }^4)$ and $H=\rho /3+O({\rho }^3)$, giving a regular core. At infinity $K$ decays exponentially and $H=1-1/\rho +O(e^{-2\rho })$, giving the vacuum Higgs magnitude and a long-range Abelian magnetic field.

On a Fourier series put $U_p(\sum a_n{q}^n)=\sum a_{pn}{q}^n$ and $V_{p}f(q)=f(q^p)$. These auxiliary operators need not individually preserve the level-one modular form space. Nevertheless $U_p{V}_p=1$, and the Fourier coefficients of a composite-index Hecke operator give $T_{p^r}={\sum }_{j=0}^r{p}^{j(k-1)}{V}_p^j{U}_p^{r-j}$. Multiplication by $T_p=U_p+p^{k-1}{V}_p$, using $U_p{V}_p=1$, gives the displayed recurrence. In particular the distinction between $U_p{V}_p=1$ and $V_p{U}_p\ne 1$ is essential.

For a normalized level-one cusp form Hecke eigenform of weight $k$, fix a prime number $p$ whose local quadratic has distinct roots. Hecke multiplication relations give $b_e=x{b}_{e-1}-b_{e-2}$ for $b_e=a_{p^e}/p^{e(k-1)/2}$ and real $x=a_p/p^{(k-1)/2}$. If $|x|<2$, write $x=2\cos \theta$; then $b_e=\sin ((e+1)\theta )/\sin \theta$. Periodicity when $\theta /(2\pi )$ is rational, and density of irrational rotations otherwise, give infinitely many $b_e\ge 1/2$. If $|x|>2$, the distinct real reciprocal roots give positive unbounded even-index terms. Reality follows from Hecke operators are self-adjoint for the Petersson inner product.

Over the polynomial parameter ring, the generic Hecke algebra has basis $(T_w{)}_{w\in W}$ and multiplicationThe parameters must agree for conjugate simple generators; equivalently, $(T_i-a_i)(T_i+1)=0$ together with the braid relations presents the algebra.

Triangulate a torus using the seven vertices of the complete graph $K_7$ and oriented triangles $(i,i+1,i+3)$ and $(i,i+3,i+2)$, with indices modulo seven. Every edge occurs twice with opposite orientations; each vertex has a cyclic link. The Euler characteristic is $7-21+14=0$. Its dual graph is the Heawood graph. This dual map has seven disc faces, each adjacent to all the others, so it needs seven face colors although its edges have a Tait coloring.

Suppose $d{r}_t=a(r_t)dt+b(r_t)d{W}_t$ under a risk-neutral measure and $f_t(T)=F(T-t,r_t)$. By Itô formula, the forward-rate volatility is ${\sigma }_t(T)=b(r_t)F_r(T-t,r_t)$. The Heath-Jarrow-Morton model drift restriction is equivalent toTo verify it directly for bonds, put $G(\theta ,r)={\int }_0^{\theta }F(s,r)ds$. Integration gives $F-r=a{G}_r+\frac{1}{2}{b}^2{G}_{rr}-\frac{1}{2}{b}^2{G}_r^2$. The zero-coupon bond price $P(t,T)=e^{-G(T-t,r_t)}$ therefore satisfiesIts bank-account-discounted price is a positive local martingale. A common equivalent local martingale measure excludes admissible arbitrage for any finite collection of these traded maturities.

With deterministic Hilbert-space-valued volatility, a deterministic initial curve and the Heath-Jarrow-Morton model drift restriction, the instantaneous forward rate is a Gaussian random field indexed by observation time and maturity. Put $\Sigma (t,T)={\int }_t^T\sigma (t,u)du$. Absence of arbitrage requires $\alpha (t,T)=⟨\sigma (t,T),\Sigma (t,T)⟩$. Indeed, Itô formula gives bond drift $r_t-{\int }_t^T\alpha (t,u)du+\Vert \Sigma (t,T){\Vert }^2/2$; equating it to the short rate and differentiating in maturity yields this restriction. The field covariance isFinite-dimensional volatility spaces give finite-factor models; an infinite-dimensional space permits much richer maturity correlations. Gaussian rates can be negative. Deterministic volatility gives explicit zero-coupon bond and bond-option formulas.

For the Heath-Jarrow-Morton model with $\sigma (t,T)=T-t$, the risk-neutral drift is $\alpha (t,T)=(T-t{)}^3/2$. Its short rate is $r_t=f(0,t)+t^4/8+{\int }_0^t{W}_{s}ds$. The centered integrated Brownian component is not Markov: its past reveals its derivative $W_t$, which affects the conditional mean of future increments, whereas its current integral does not determine $W_t$. Indeed the conditional variance of $W_t$ given the current integral is $t/4$. A one-dimensional driving noise therefore does not force a one-dimensional Markov state.

For a maturity-differentiable Heath-Jarrow-Morton model forward field with the integrability needed for stochastic differentiation, the short rate $r_t=f(t,t)$ has the displayed dynamics. Indeed changing observation time uses the forward-rate stochastic differential equation, while changing maturity adds ${\partial }_{T}f(t,t)dt$. Under a risk-neutral measure, $\alpha (t,T)=\sigma (t,T){\int }_t^T\sigma (t,u)du$, so $\alpha (t,t)=0$. The remaining drift depends on the diagonal slope of the whole forward curve, which need not be determined by $r_t$; a Markov process for the short rate is an additional modelling restriction. Without sufficient maturity regularity, the diagonal need not admit this classical Itô process formula.

For a compact smooth Riemannian surface with smooth boundary and a pure Dirichlet boundary condition or pure Neumann boundary condition, the constant coefficient in the heat trace isThe equality is the Gauss-Bonnet theorem. Thus such isospectral manifolds have the same Euler characteristic. A simply connected compact connected bordered surface is a disk with $\chi =1$, whereas a nonorientable surface with $c\ge 1$ crosscaps and $b\ge 1$ boundary components has $\chi =2-c-b\le 0$. These cannot be isospectral in this setting. Corners and mixed boundary conditions contribute additional heat coefficients, so the smooth pure-boundary-condition hypothesis is essential.

On a closed manifold, the positive Laplace-Beltrami operator has a smooth heat kernel and its heat semigroup is a trace-class operator for positive time. Expanding in a smooth orthonormal eigenbasis gives $K_t(x,y)={\sum }_j{e}^{-t{\lambda }_j}{\varphi }_j(x)\overline{{\varphi }_j(y)}$. Elliptic regularity bounds each derivative of ${\varphi }_j$ polynomially in ${\lambda }_j$, while the exponential dominates those powers, so the expansion converges with all derivatives. Integrating the diagonal and using the unit norm of each eigenfunction proves the formula. For a bundle operator, insert the fibre matrix trace inside the integral.

A lambda term is solvable if its closure by lambda abstractions over its free variables can be applied to finitely many closed lambda terms to obtain $I=\lambda x.x$ in beta equivalence. This is equivalent to having a head normal form. A head variable in a head normal form can be replaced by a projection returning $I$; conversely standardization theorem for beta reduction traces any successful head computation back to a head variable of the original term.

An unsolvable lambda term has no head normal form, equivalently it is not a solvable lambda term. Capture-avoiding substitution and lambda application preserve unsolvability: until a head variable appears, head contractions proceed within the original term and cannot inspect the supplied terms.

The Böhm tree of an unsolvable lambda term is $\perp$. If $M{\to }_{\beta }^{\ast }\lambda x_1\cdots x_n.y{M}_1\cdots M_r$ is a head normal form, its Böhm tree has root label $\lambda x_1\cdots x_n.y$ and ordered children $BT(M_1),\dots ,BT(M_r)$. The tree may be infinite. Church-Rosser theorem and alpha equivalence make this independent of the selected head reduct.

For a monatomic fully convective ideal gas star, uniform specific entropy gives $P=K{T}^{5/2}$ with $K\propto {\mu }^{-5/2}{M}^{-1/2}{R}^{-3/2}$. Combining this with the stellar surface boundary condition $\kappa P=2g/3$ and $\kappa ={\kappa }_0{\rho }^a{T}^b$ givesAll composition comparisons here hold ${\kappa }_0$ fixed. For $a=1,b=4$, $T_e^8\propto {\mu }^4{M}^{2}R$, and the Stefan–Boltzmann law gives $L\propto {\mu }^{2}M{R}^{5/2}$. The stellar virial theorem and Kelvin-Helmholtz contraction then give $R^{-7/2}-R_0^{-7/2}\propto {\mu }^2{M}^{-1}(t-t_0)$, with a positive coefficient. Once the initial-radius term is negligible, $R\propto {\mu }^{-4/7}{M}^{2/7}(t-t_0{)}^{-2/7}$.

Match an efficient, monatomic gas, fully convective star to the grey-atmosphere convection onset with thirteenth-power opacity. Its convective relation is $P=K_T{T}^{5/2}$. At the matching temperature $T_b\propto T_e$, the stellar atmosphere gives $K_T^2\propto M{L}^{-1}{T}_e^{-13}\propto M{R}^{13/2}{L}^{-17/4}$ using the Stefan–Boltzmann law. The ideal-gas relation converts this to $P=K_{\rho }{\rho }^{5/3}$ with $K_{\rho }=(\mathcal{R}/\mu {)}^{5/3}{K}_T^{-2/3}$. The polytropic mass-radius relation at index $3/2$ gives $K_{\rho }\propto G{M}^{1/3}R$, hence $K_T^2\propto M^{-1}{R}^{-3}$. Equating the two expressions proves $L^{17/4}\propto M^2{R}^{19/2}$, or $L\propto M^{8/17}{R}^{38/17}$. The entropy coefficient is constant throughout the convective envelope, but can change between models.