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Model Spectra of Neutron Star Surface Thermal Emission

Model Spectra of Neutron Star Surface Thermal Emission. Department of Physics National Tsing Hua University Lun-Wen Yeh 2004.5.6. Structure of neutron star. P( τ ) ρ ( τ ) T( τ ). Flux = const. Radiation transfer equation. Spectrum. Flux ≠const. Temperature correction.

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Model Spectra of Neutron Star Surface Thermal Emission

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  1. Model Spectra of Neutron Star Surface Thermal Emission Department of Physics National Tsing Hua University Lun-Wen Yeh 2004.5.6

  2. Structure of neutron star P(τ) ρ(τ) T(τ) Flux = const Radiation transfer equation Spectrum Flux ≠const Temperature correction

  3. Assumptions • Plane-parallel atmosphere( local model) • Radiative equilibrium( energy transported solely by radiation ) • Equation of state is ideal gas( ionized H) • Neglect conduction and convection • Hydrostatics • No magnetic field • The physical properties independent of time

  4. Structure of NS • Gray atmosphere • Equation of state • Oppenheimer-Volkoff

  5. Structure of NS • Rosseland mean

  6. Radiation transfer equation Spontaneous emission Induced emission Absorption Scattering

  7. Radiation transfer equation Diffusion approimation

  8. Feautrier method Mean intensity like Flux like

  9. Feautrier method Surface normal n

  10. Feautrier method

  11. Feautrier method d=2,3,……,D-2,D-1 μ=1,2,……M

  12. Feautrier method d=1 d=2 d=3….. I1 I2 I3 .. .. .. I1 I2 I3 .. .. .. I1 I2 I3 .. .. ..

  13. Test Feautrier method Scattering

  14. Test Feautrier method Scattering and free-free absorption

  15. 46~91 4.9% 91~901 4.1% 901~9001 0.39%

  16. 46~91 0.29% 91~901 0.17% 901~9001 0.0079%

  17. 46~91 0.19% 91~901 0.065% 901~9001 0.0058%

  18. 46~91 4.2% 91~901 3.6% 901~9001 0.30%

  19. Future work • Run my program with many directions , and carry out temperature-correction. • Add magnetic filed in local model

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