Spectral behavior of thermal emission from NSs & its application

Introduction Code and results Some remarkable sources Model residuals: for the case 1E Summary

∫Iνθdθdφ∫Iνθdθdφ Total flux = I 0 S 0 (θb, θn) = σ T eff 4 (ψ) σ T Ω 4 =π I 0 f (θb, θn) Choose Conti. Mode or Line Mode Beaming Table θ’(θ)φ’(φ)θ’(θ)φ’(φ) Intensity( ) Line_component( ) Theta( )  Spherical symmetry, the metric outside the star is taken to be the Schwarzschild metric  Photons are emitted from the surface of an opaque sphere.  I ν = B ν.

I ν ( T 1 ) I ν ( T 2 ) I ν ( T 3 ) I ν ( T 4 ) I ν ( T 5 ) I ν ( T 4 ) I ν ( T 3 ) I ν ( T 2 ) I ν ( T 1 )

Pechenick et al. ApJ 274:846

1E XMM PN observation Bignami et al. Nature 423: Phase-integrated spectrum

Haberl astro-ph/ E X BB 2.2

RX J0720 astro-ph/

RBS 1223 A&A 403,L19

RX J1605 ApJ 608:432

table.cBeaming Table spec.c global.h Conti. Mode / Line Modesigma.c Photon NumberResidual

Unfolded model Response Folded model

Unfolded model Obs. data ?

Discussion Obs. Time P An unique case ??

Pechenick et al. ApJ 274:846 H.K Chang 2001 Chinese Journal of Physics 39:319 Contours of Polar-cap-to-stellar-surface area ratio Contours of Pulse fraction

Summary ”