1. Spectral behavior of thermal emission from NSs & its application

2. Introduction Code and results Some remarkable sources Model residuals: for the case 1E 1207.4 -5209 Summary

4. ∫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.

5. 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 )

6. Pechenick et al. ApJ 274:846

19. 1E1207.4-5209 XMM PN observation Bignami et al. Nature 423:725 2003 Phase-integrated spectrum

21. Haberl astro-ph/0302540 1E 1207.4-5209 0.42413076 1.4X10 -14 2BB 2.2

22. RX J0720 astro-ph/0312413

24. RBS 1223 A&A 403,L19

26. RX J1605 ApJ 608:432

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

30. Unfolded model Response Folded model

31. Unfolded model Obs. data ?

34. Discussion Obs. Time P An unique case ??

37. 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

39. Summary ”