the magnetic field of an isolated neutron star from x-ray cyclotron absorption lines
DESCRIPTION
The Magnetic Field of an Isolated Neutron Star from X-ray Cyclotron Absorption Lines. G.F.Bignami (1,2) P.A.Caraveo (3) A.De Luca (3,4) S.Mereghetti (3). (1) CESR, Toulouse, France (2) Università di Pavia, Pavia, Italy (3) CNR-IASF, Milano, Italy - PowerPoint PPT PresentationTRANSCRIPT
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The Magnetic Field of an Isolated Neutron Star from X-ray Cyclotron Absorption Lines
G.F.Bignami (1,2)
P.A.Caraveo (3)
A.De Luca (3,4)
S.Mereghetti (3)
(1) CESR, Toulouse, France
(2) Università di Pavia, Pavia, Italy
(3) CNR-IASF, Milano, Italy
(4) Università di Milano Bicocca, Milano, Italy
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INS results from Chandra
PSR B0656+14
PSR B1055-52
Vela pulsarRX J0720.4-3125
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INS results from XMM-Newton
Puppis A PSR J0030+0451
PSR B1055-52 RX J0720.4-3125
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Then came 1E1207.4-5209
•Discovered by Einstein
•Close to the center of SNR G296.5+10.0
•“High” galactic latitude: b≈10°
•SNR age: 7 kyears
•SNR distance: 2 kpc
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A radio-quiet INS candidate
•Lack of optical counterpart
•No radio source
•BB-like X-ray spectrum
Radio-quiet INS?
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NS nature confirmed by Chandra
P~424 ms (Zavlin et al.2000)
Estimate of Pdot (0.7-3.1)x10-14 s s-1 (Pavlov et al.2002)
Age Problem: τPSR >> τSNR
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This INS was the first to show features in its spectrum
ChandraSanwal et al, 2002
Same dataHailey & Mori 2002
XMM-Newton Mereghetti et al, 2002
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The latest EPIC view: 260 ksec
The deepest XMM-Newton galactic field
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Phase-averaged spectroscopy
pn data
208,000 photons
MOS (1+2) data
151,300 photons
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0.7 keV1.4 keV
2.1 keV 2.8 keV
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Check for possible miscalibrations
Red: 3C273 Black: 1E1207.4-5209
0.7 1.4
2.1(2.8)
AuSi
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Timing Analysis
Pulsed fraction ~ 7%
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Phase-resolved spectroscopy
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Conclusions
IF electron cyclotron: <B> 8 1010
IF proton <B> 1.6 1014
Problem with B as derived from timing parameters:
Current pdot:(1.4 0.3) 10-14 s/s implies B= 2-3 1012
but also implies an age of 5 105 years in contrast with the SNR age ( about 104 ys)
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0.7 keV
1.4 keV 2.1 keV 2.8 keV