Evolution of isolated neutron stars: young coolers and old accretors Sergei Popov (SAI)
The Absorption Features in X-ray Emission from Isolated Neutron Stars
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Transcript of The Absorption Features in X-ray Emission from Isolated Neutron Stars
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The Absorption Features in X-ray Emission
from Isolated Neutron Stars
2004 / 04 / 15
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Assumptions & Global Model
Gravitation Effect (see Isothermal NS Case)
Canonical Model & Line profile
INS: 1E 1207.4-5209
Results & Discussions
OH MY!! What’s going on??
Outline
Lensing Red-shift
Strong M field Effect
Anisotropy of the surface temperature Beaming
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Assumption
Spherical symmetry typical neutron star.
Photons are emitted from the surface of an opaque sphere.
LTE: Iν= Bν.
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Global modelChanging coordinate
Z axisθθ
θmθm
Magnetic Axis
θbθb
θpθpSurface normal
Magnetic Axis
Rotation Axis
θθ00
ββ
γγ
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Flux(t): (Lightcurve)∫I(t) cosθ’ dΩ’
Spec.:∫Iν(t) cosθ’ dΩ’
∫Iν(t) cosθ ’ dt dΩ’
Note: cosθ’ isqual to 1
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Gravitational Effects
Self-Lensing
Gravitational redshift
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5.05.02122
RM
R/M M/R4
0.25e30 0
1
2
4ddB
ddB
Relative total flux v.s ωt
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R/M M/R
40.25
e30 0
15.0)5.01log(21log
R
M
ν’ ν
dB
1
2
3dB ν ’ ν
Relative specific flux v.s Freq.
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Strong Magnetic field effects• Anisotropy of the surface temperature
• Beaming ( In magnetized electron-ion plasma, the scattering and
free-free absorption opacities depend on the direction of propagation and the normal modes of EM waves) Dong Lai etc. MNRAS 327,1081 2001
core
envelope
atmosphereνcyclotron
=eB/2πme
K
Ion cyclotron resonance occurs whenThe E field of the mode rotates in the same direction as the ion gyration
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4 22 )(sin0264.0)(cos02.1 bbeff TPT
Heyl etc. MNRA 324,292 2001Best-fitting model for (a*cos 2θ +b*sin 2θ) for 1012G
4effTFlux
Relative T v.s. θb
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Isotropic :
Iν ( T1)
Iν ( T2)
Iν ( T3)
Iν ( T4) Iν ( T5) Iν ( T4)
Iν ( T3)
Iν ( T2)
Iν ( T1)T 1 = T eff
Iν ( T1)
Iν ( T1)
Iν ( T1)
Iν ( T1)
Iν ( T1)
θbθb
4 cos cos
: assume
effbb TddIFluxtotal
BI
Harding etc. ApJ 500:862 1998 Pavlov etc. A&A 297,441 1995
Beaming due to B field :
B field
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3D Angles…..|=.=|“
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. .
θmθm
Magnetic Axis
θbθb
θpθp
Need to calculate Θm Θm θB_field θB_field surface surface temperaturetemperatureΘphoton Θphoton Limb-darkening Limb-darkeningθphoton&B_fieldθphoton&B_field Magnetic beaming Magnetic beaming
Surface normal
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Canonical ModelM=1.4M⊙ R=10km T =1 secRs=2GM/C2 ~ 0.267R θMAX~132∘
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1E1207.4-5209
XMM PN observationBignami et al. Nature 423:725 2003
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Results
Simple Dipole Model Limb-darkening Model Magnetic Beaming Model
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Cyclotron Resonance Lines
23
2
222
4
1
3
2 frequency) resonance sn' (the
)(
)(
nnn
nnTn
nn
mC
e
mC
eBn
eIf
Ex. B=1011Gauss @ pole
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Binning
Photon number
Line profile in units of σ
Line (line1+line2) Conti.
0.5KeV 1KeV3x1017 Hz
5KeV
50 bin 50 bin
(Log Scale)
Given:1. Observing time2. Effective area3. Distance to the source
case continuumin number photon ltheoretica:
case linein number photon ltheoretica:
conti
line
line
contiline
N
N
N
NN
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N~106
Stellar absorption by NH~1021cm-2
N~103
Numerical Results Observation
0.2~4KeV
208,000 photons
& Lack of photon ~1KeV and higher energy
Note that although we lack of photon at ~ 1KeV and higher energy (“lack” means in our calculus, the theoretical photon number is lower than “1” photon), we can still calculate the residual in units of σ
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40:25
~102 :1
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As a reasonable try , we multiply 103 in each bin to get a similar total photon number with observation.
The ratio of the first line and the second line is even worse. (about 103:1)
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DiscussionOur results show that a direct approach to reproduce the line features for 1E1207.4-5209is not work well. Photon number problem The photon number problem might be solved
by higher temperature in polar cap or the larger neutron star radius in our model.
Ratio problem The ratio problem is essentially difficult to
solved for our considerations.
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