xmm-newton contribution
DESCRIPTION
XMM-Newton contribution. 1E1207-52. EPIC 230 ksec. 1 st direct measurent of the magnetic field of an isolated neutron star (where cyclotron absorption is taking place ). 2.1 keV. 2.8 keV. 1.4 keV. 0.7 keV. Conclusions. For electrons: 8 10 10 G - PowerPoint PPT PresentationTRANSCRIPT
XMM-Newton contribution
EPIC 230 ksec
1E1207-52
0.7 keV
1.4 keV 2.1 keV 2.8 keV
1 st direct measurent of the magnetic field of an isolated neutron star (where cyclotron
absorption is taking place)
Conclusions
For electrons: <B> 8 1010 Gfor protons : <B> 1.6 1014 G
PROBLEMpdot:(1.4 0.3) 10-14 s/s
implies B= 2-3 1012
but also an age of 5 105 yversus the SN age ( circa 104 ys)
EPIC 100 ksec
Geminga
MOS
Energetics Edot 3 1034 erg/secD = 160 pc=170 mas/yvtr =120 km/sec
Geminga luminosity 3 1031 erg/sec (0.1-5 keV)Tails luminosity 6.8 1028 erg/sec
The tails account for 2 10-6 Edot
224 NSISMSO
VcR
E
VNS=D/cos(i)
224 NSISMSO
VcR
E
VNS=D/cos(i)
from bow-shock
0.06 < ISM < 0.15 at/cm-3
which implies 7 < M < 20
we can obtain
What produces the X-rays
Power law spectrum -> synchrotron radiation
-> need for electrons and magnetic field
From bow-shock theory
shock = 4 ISM
Since B is frozen-in
shock = 4 ISM
shock = 10-5 G
To produce keV photons in 10-5 G B field one needs 1014 eV electrons
1014 eV electrons will have a Larmor radius of 3.4 1016 cm thickness 6.8 1016 cm 27”
1014 eV electrons will lose half of their energy in 800 y . 180 “ / 170 mas/y = 1,000 y
Caraveo et al. 2003Science 301, 1345
Pn data ~ 53,000 photons
Time-averaged spectroscopy
Timing analysis
Common minimumGamma peaks
Phase-resolved spectroscopy
Phase-resolved spectroscopy
Caraveo et al, 2004 Science 305,376
Phase-resolved emission (160 pc)
Conclusions
-hot spot ( ~1.9 M °K), radius 0-60 m Probably polar cap seen at 70°-80° inclination cos x R (R/c)1/2 (~300m)
luminosity 1.5 1029 erg/sec
rotating
-Cool black-body ( ~.48 M °K), Eurasia size
luminosity 2.6 1031 erg/sec
-Power law photon index 1.7 0.1 luminosity 7.7 1029 erg/sec
Is Geminga unique?
EPIC view of PSRs B1055 & B0656
pn 60 ksec
85,000 photons
1055-52
MOS 83 ksec
0656+14
MOS 40 ksec
pn 35 ksec
120,000 photons
Phase-averaged spectra
They all show phase spectral variations
0656 1055
Geminga
1055-58
0656
Geminga
Cool bb: is it the surface of the NS?
problem0656+14
1055-58
0656
Geminga
hot spot(s) sizes?
0656+14
Hot bb:
rotator inclinations?
their dimensions are vastly different
although they should not !!!
Hot bb: heated polar cap(s) ?
theoretical cap radii ~250-320 m
real EPIC radii: 60, 800, 1500 m