1. Non-Thermal X-ray Emission Properties of Rotation-Powered Pulsars with Chandra & XMM
Xiang-Hua Li
Directed by: Ti-Pei Li & Fang-Jun Lu
Institute of High Energy Physics, CAS

2. Outline Introduction & Motivations Sample and Data process
Results & Discussions
Conclusion

3. Introduction
Rotation powered pulsar radiating at the expense of rotational energy
How the spin-down energy is converted to the high energy radiation?
Many studies have sought to determine the relationship between the X-ray luminosity (Lx) and the spin-down power (Edot)

4. Radiation Components of Rotation Powered Pulsars
Non-thermal
PWN
pulsed radiation from pulsar
Non-pulsed radiation from pulsar
Thermal
non-pulsed radiation from the pulsar~0.1keV
pulsed radiation from the pulsar~1keV
Cheng & Zhang 1999

5. Radiation Components of Rotation Powered Pulsars
Non-thermal
PWN
pulsed radiation from pulsar
Non-pulsed radiation from pulsar
Thermal
non-pulsed radiation from the pulsar~0.1keV
pulsed radiation from the pulsar~1keV
Cheng & Zhang 1999

6. Becker and Trumper (1997) used ROSAT data (0. 1-2
Becker and Trumper (1997) used ROSAT data ( keV) and found Lx ~ 10-3Edot for 27 rotation-power pulsars (thermal and non-thermal)

7. Saito (1998) used 16 rotation-power pulsars observed by ASCA (2-10 keV) and found Lx ~ (Edot)3/2

8. Possenti et al. (2002) used ROSAT, ASCA, RXTE, BappoSAX, Chandra, XMM (41 pulsars) to obtain Lx ~ (Edot)1.34(2-10keV)

9. Motivations
With high spatial resolution X-ray data of Chandra and XMM-Newton data, resolved the pulsar from its surrounding PWNe
Energy range: 2-10keV /exclude thermal components
Check the dependences of Lx and Edot, and other parameters of pulsars and PWNe

10. Sample and data process
All rotation-powered pulsars in the Archived data of Chandra and literatures
Use published spectrum data if available
Process the archived data if unavailable，use XMM data if Chandra sources are too faint
Obtain the X-ray spectrum properties of both pulsar and pulsar wind nebula
In Total: 38 pulsars
23 PWNe

11. Results & Discussions

12. The correlation between Lxpsr and Edot of pulsars
Becker&Truemper(1997)
ROSAT
Possenti et al. (2002)
Saito(1998)
ASCA
Lx ~ (Edot)1.34

13. The correlation between Lxpsr and Edot of pulsars
Becker&Truemper(1997)
ROSAT
Possenti et al. (2002)
Lxpul ~ (Edot)1.15
Cheng (2004)
Lx ~ (Edot)1.34

14. The correlation between Lxpsr and Edot of pulsars
Becker&Truemper(1997)
ROSAT
Theory ：Lx~(Edot)1.15 (Cheng & Zhang 1999)
Possenti et al. (2002)
Lxpul ~ (Edot)1.15
Cheng (2004)
Lx ~ (Edot)1.34

15. The correlation between Lx of PWN and Edot
Saito(1998)
ASCA
Possenti et al. (2002)
Cheng et al. (2004)
(Lx)npul ~ (Edot)1.4
Lx ~ (Edot)1.34

16. psr~B
psr~c
psr~Lx
What these Correlations mean?

17. Conclusions (I)
Lxpsr~Edot relation in 2-10 keV is different from those from keV (Becker & Truemper 1997)
Different emission components
Different energy band
Lxpsr~Edot relation is different with Possenti(2002)
higher resolution observations have been used
Lxpsr~Edot relation of pulsars are consistent with the model predicted (Cheng & Zhang 1999)

18. Conclusions (II) What these correlations mean? Welcome suggestions!
LxPWN~Edot of PWNe are consistent with those given by other authors
The correlations
psr~B
psr~Lxpsr
psr~c
What these correlations mean?
Welcome suggestions!

19. Thanks