Loading in 5 sec....

Model Spectra of Neutron Star Surface Thermal Emission ---Diffusion Approximation PowerPoint Presentation

Model Spectra of Neutron Star Surface Thermal Emission ---Diffusion Approximation

- 100 Views
- Uploaded on

Download Presentation
## PowerPoint Slideshow about 'Model Spectra of Neutron Star Surface Thermal Emission ---Diffusion Approximation' - kylee-vang

**An Image/Link below is provided (as is) to download presentation**

Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.

- - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - -

Presentation Transcript

### Model Spectra of Neutron Star Surface Thermal Emission---Diffusion Approximation

Department of Physics

National Tsing Hua University

G.T. Chen

2005/11/3

Outline

- Assumptions
- Radiation Transfer Equation
------Diffusion Approximation

- Improved Feautrier Method
- Temperature Correction
- Results
- Future work

Assumptions

- Plane-parallel atmosphere( local model).
- Radiative equilibrium( energy transported solely by radiation ) .
- Hydrostatics. All physical quantities are independent of time
- The composition of the atmosphere is fully ionized ideal hydrogen gas.
- No magnetic field

The Structure of neutron star atmosphere

P(τ) ρ(τ) T(τ)

Improved Feautrier Method

Flux = const

Radiation transfer equation

Diffusion Approximation

Flux ≠const

Unsold Lucy process

Temperature correction

Spectrum

The Structure of neutron star atmosphere

P(τ) ρ(τ) T(τ)

Improved Feautrier Method

Flux = const

Spectrum

Radiation transfer equation

Diffusion Approximation

Flux ≠const

Unsold Lucy process

Temperature correction

The structure of neutron star atmosphere

- Gray atmosphere(Trail temperature profile)
- Equation of state
- Oppenheimer-Volkoff

The Rosseland mean depth

The structure of neutron star atmosphere

The Rosseland mean opacity

where

If given an effective temperature( Te ) and effective gravity ( g* ) , we can get

(The structure of NS atmosphere)

Parameters In this Case

- First ,we consider the effective temperature is 106 K and effective gravity is 1014 cm/s2

The Structure of neutron star atmosphere

P(τ) ρ(τ) T(τ)

Improved Feautrier Method

Radiation transfer equation

Flux = const

Spectrum

Diffusion Approximation

Flux ≠const

Unsold Lucy process

Temperature correction

Diffusion Approximation

τ>>1 ,

(1) Integrate all solid angle and divide by 4π

(2) Times μ ,then integrate all solid angle and divide by 4π

Diffusion Approximation

We assume the form of the specific intensity is always the same in all optical depth

Radiation Transfer Equation

(1) Integrate all solid angle and divide by 4π

(1)

(2) Times μ ,then integrate all solid angle and divide

by 4π

(2)

Note:

Jν= ∫I ν dΩ/4π

Hν= ∫I νμdΩ/4π

Kν= ∫I νμ2dΩ/4π

RTE---Boundary Conditions

I(τ1,-μ,)=0

τ1,τ2,τ3, . . . . . . . . . . . . . . . . . . . . . . . . . . .,τD

Improved Feautrier Method

To solve the RTE of u , we use the outer boundary condition ,and define some discrete parameters, then we get the recurrence relation of u

where

Improved Feautrier Method

Initial conditions

Improved Feautrier Method

- Put the inner boundary condition into the relation , we can get the u=u (τ)
F = F (τ)

- Choose the delta-logtau=0.01
from tau=10-7 ~ 1000

- Choose the delta-lognu=0.1
from freq.=1015 ~ 1019

Note : first, we put BC1 in the relation

The Structure of neutron star atmosphere

P(τ) ρ(τ) T(τ)

Improved Feautrier Method

Flux = const

Radiation transfer equation

Diffusion Approximation

Flux ≠const

Unsold Lucy process

Temperature correction

Spectrum

Unsold-Lucy Process

define B= ∫Bν dν , J= ∫Jν dν, H= ∫Hν dν, K= ∫Kν dν

define Planck mean κp= ∫κff* Bν dν /B

intensity mean κJ= ∫ κff* Jν dν/J

flux mean κH= ∫(κff*+κsc )Hν dν/H

Unsold-Lucy Process

Eddington approximation: J(τ)~3K(τ)

and J(0)~2H(0)

Use Eddington approximation and combine above two equation

The Structure of neutron star atmosphere

P(τ) ρ(τ) T(τ)

Improved Feautrier Method

Flux = const

Radiation transfer equation

Diffusion Approximation

Flux ≠const

Unsold Lucy process

Temperature correction

Spectrum

5.670*1019 ±1%

Te=106 K

Te=106 K

Te=106 K

Te=106 K

Te=106 K

Te=106 K frequency=1017 Hz

Te=106 K

Spectrum

BC1 vs BC2

Te=106 K

BC1 vs BC2

Te=106 K

BC1 vs BC2

- The results of using BC1 and BC2 are almost the same
- BC1 has more physical meanings, so we take the results of using BC1 to compare with Non-diffusion approximation solutions calculated by Soccer

Diffusion ApproximationvsNon-Diffusion Approximation

This part had been calculated by Soccer

Te=106 K

Te=106 K frequency=1016 Hz

Te=106 K frequency=1017 Hz

Te=106 K frequency=1018 Hz

Te=5*105 K

Te=5*106 K

3.9811*1017 Hz

Te=5*106 K

- The results with higher effective temperature are more closed to Non-DA solutions than with lower effective temperature
- When θ is large , the difference between two methods is large
- The computing time for this method is faster than another
- The results comparing with Non-DA are not good enough

Future Work closed to Non-DA solutions than with lower effective temperature

- Including magnetic field effects in R.T.E, and solve the eq. by diffusion approximation
- Compare with Non-D.A. results
- Another subject:
One and two-photon process calculation

To Be Continued……. closed to Non-DA solutions than with lower effective temperature

Te=10 closed to Non-DA solutions than with lower effective temperature6 K intensity of gray temperature profile

ν=1017 Hz

Te=10 closed to Non-DA solutions than with lower effective temperature6 K Total flux of gray temperature profile

Download Presentation

Connecting to Server..