超新星遗迹 的XTP 观测模拟 南京大学 陈阳、周平、张潇

1. Non-thermal X-ray shells A great advantage of XTP for SNR studies: able to tell the polarized synchrotron X-rays from thermal X-rays. Chandra discovered ~10 SNRs with nonthermal (sync.) X-ray boundaries In some SNRs, non-thermal X-rays may be blended with thermal ones, and are needed to be differentiated E.g.，in SNR N132D, thermal component + hard tail. Is the hard tail synchrotron emission?

N132D in LMC(50kpc) for example Powerlaw component: S3: F(2-10keV)=4E-13 erg/cm^2/s S4: F(2-10keV)=3E-13 erg/cm^2/s Entire: F(2-10keV)>~1E-11 erg/cm^2/s If at d of Galactic SNRs (~10kpc) X-ray flux of order: 1E-10至1E-9erg/cm^2/s

Simulated XTP spectra of N132D N132D S4 region  100ks

LFA spectrum

direction of effective injection: ‘quasi-parallel scenario’ vs. ‘quasi-perpendicular scenario’ (Fulbright & Reynolds 1990) bilateral SNR, e.g. SN1006，“polar cap”or “equator”? SN 1006 G1.9+0.3

“Role of B”目标、对策 <10 keV, 一维偏振成像, 偏振度一维分布 Pix=2’ PSF=2’ 30 arcmin in diameter

Simulated XTP spectra of SN1006 Model: phabs*srcut  NH=6.8e20, alpha=0.57, break=5.69e16 Hz, norm=16.2 (Bamba et al. 2008) exposure=100ks

4. Pulsar wind nebulae (PWNe) PWNe harbored in SNRs has prominent polarized sync. X-rays (radio P-degree upto 50% Reynolds 2012). XTP observation: beneficial to filtering PWNe in SNRs, such as the PSR and PWN in SNR G11.2-0.3. obtains degree of polarization (but hard for spatial structure due to small size of PWNe) P = (s+1)/(s+7/3)

Simulated XTP spectra of Crab Crab   10ks, Model: phabs*powerlaw NH=0.32e22, Photon index=2.1, Norm=9.65

Identify PWN in SNRs/UGSs HESS J1837 (Anada, T. 2009, PASJ, 61, 183; Suzaku & ASCA) P=70.5 ms

Our prediction for src1 : for P = 50%

Secondary electrons’ synchrotron of SNR in molecular clouds? * A qualitative consideration: In the radiative stage of SNR, particle acc. essentially stops; Major electrons can’t emit X-rays, But: p-p coll.  decay secondary electrons X-ray synchrotron (XTP detection?) Would be an evidence for proton acc. & hadronic interaction * 难点首先在于空间分辨！

Simulated secondary sync. of W28