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

Outline

Introduction & MotivationsSample and Data processResults & DiscussionsConclusion

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 (L

x) and the spin-down power (Edot)

Radiation Components of Rotation Powered Pulsars

Non-thermal PWNpulsed radiation from

pulsarNon-pulsed radiation

from pulsar

Thermal non-pulsed radiation

from the pulsar~0.1keVpulsed radiation from

the pulsar~1keVCheng & Zhang 1999

Radiation Components of Rotation Powered Pulsars

Non-thermal PWNpulsed radiation from

pulsarNon-pulsed radiation

from pulsar

Thermal non-pulsed radiation

from the pulsar~0.1keVpulsed radiation from

the pulsar~1keVCheng & Zhang 1999

Becker and Trumper (1997) used ROSAT data (0.1-2.4 keV) and found Lx ~ 10-3Edot for 27 rotation-power pulsars (thermal and non-thermal)

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

Possenti et al. (2002) used ROSAT, ASCA, RXTE, BappoSAX, Chandra, XMM (41 pulsars) to obtain

Lx ~ (Edot)1.34(2-10keV)

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

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

Results & Discussions

The correlation between Lxpsr and Edot of pulsars

Becker&Truemper(1997)

ROSAT

Saito(1998)

ASCA

Possenti et al. (2002)

Lx ~ (Edot)1.34

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

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

Theory ： Lx~(Edot)1.15 (Cheng & Zhang 1999)

The correlation between Lx of PWN and Edot

Possenti et al. (2002)

Saito(1998)

ASCA

Cheng et al. (2004)

(Lx)npul ~ (Edot)1.4Lx ~ (Edot)1.34

What these Correlations mean?

psr~Lx

psr~B psr~c

Conclusions (I)

Lxpsr~Edot relation in 2-10 keV is different fro

m those from 0.1-2.4 keV (Becker & Truemper 19

97)Different emission componentsDifferent energy band

Lxpsr~Edot relation is different with Possenti(2002)

higher resolution observations have been used Lx

psr~Edot relation of pulsars are consistent with the model predicted (Cheng & Zhang 1999)

Conclusions (II)

LxPWN~Edot of PWNe are consistent with thos

e given by other authors The correlations

psr~Bpsr~Lx

psr

psr~c

What these correlations mean? Welcome suggestions!

Thanks