The hard X-ray spectrum of Pulsar Wind Nebulae Data-models comparison in the Simbol-X era F. Bocchino, INAF Osservatorio Astronomico di Palermo with contributions of R. Bandiera (INAF-OAA), L. Del Zanna (UNIFI), D. Volpi (UNIFI), G. Cusumano (INAF-IASF Pa)
Data-models comparison in the Simbol-X era F. Bocchino, INAF Osservatorio Astronomico di Palermo with contributions of R. Bandiera (INAF-OAA), L. Del Zanna (UNIFI), D. Volpi (UNIFI), G. Cusumano (INAF-IASF Pa). The hard X-ray spectrum of Pulsar Wind Nebulae. Introduction. What is a PWN. - PowerPoint PPT Presentation
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The hard X-ray spectrum of Pulsar Wind Nebulae
Data-models comparison in the Simbol-X era
F. Bocchino, INAF Osservatorio Astronomico di Palermo
with contributions of
R. Bandiera (INAF-OAA), L. Del Zanna (UNIFI), D. Volpi (UNIFI), G. Cusumano (INAF-IASF Pa)
Introduction
What is a PWN...
Introduction
The mechanism which bring particles and fields to the outer edge of the nebulae is still under investigation
“It's like finding the transmission lines between the power plant and the light bulb.” (J. Hester, Arizona Univ.)
Data-model comparison in the Simbol-X era Simulated synchrotron emission
from PWNe (Del Zanna et al. 2006)
run A: =0.025, nearly ideal case for Crabrun B: =0.1 large equatorial unmagnetized region
equator polepole
Data-model comparison in the Simbol-X era: the Crab
Only the nebular emission is considered
VELA: Mangano et al 06 (obs)
CRAB1: de Jager et al. 1996 (obs)
CRAB2: Massaro et al 2000 (obs)
LDZ06: Del Zanna et al 2006 (models)
Data-model comparison in the Simbol-X era: the Crab
Only the nebular emission is considered
VELA: Mangano et al 06 (obs)
CRAB1: de Jager et al. 1996 (obs)
CRAB2: Massaro et al 2000 (obs)
LDZ06: Del Zanna et al 2006 (model)
Black: Simbol-X 100 ks simulated spectrum
Data-model comparison in the Simbol-X era: 3C 58 Prototype of “non-Crab like” PWNe Diffusive synchrotron radiation from
PWNe (Fleishmann & Bietenholtz 2007) seems to overcome the difficulty of low frequency and large change of slope of the break in the radio band
What about in the X-ray band?
Data-model comparison in the Simbol-X era: 3C 58
DSR 3c58: Diffusive synchrotron radiation model of Fleishmann & Bietenholz (2007) tailored to 3c58 broad band spectrum
Data-model comparison in the Simbol-X era: 3C 58
Black solid: XMM 30 ks DSR 3c58: Diffusive synchrotron radiation model of Fleishmann & Bietenholz (2007) tailored to 3c58 broad band spectrum
Data-model comparison in the Simbol-X era: 3C 58
Black solid: XMM 30 ksRed solid: Simbol-X 100 ks
DSR 3c58: Diffusive synchrotron radiation model of Fleishmann & Bietenholz (2007) tailored to 3c58 broad band spectrum
Conclusions The shape of the hard X-ray spectrum of Pulsar Wind
Nebulae is directly related to the distribution of B and e- in the source
Current measurements are just enough to provide some diagnostics for the brightest objects (Crab and Vela)
Simbol-X may provide an order of magnitude improvement in the comparison between model and observations for these bright sources
Other bright PWNe (G21.5-0.9, 3C58) are hardly detected by non-imaging hard X-ray instruments. Simbol-X will provide THE unique opportunity to study the spectrum above 5-10 keV.