paczyński m odulation : d iagnostics of the neutron star eos?
DESCRIPTION
Paczyński M odulation : D iagnostics of the Neutron Star EOS?. Gabriel Török , Martin Urbanec, Karel Adámek, Pavel Bakala , Eva Šrámková, Zdeněk Stuchlík. Institute of Physics, Silesian University in Opava. - PowerPoint PPT PresentationTRANSCRIPT
Paczyński Modulation: Diagnostics of the Neutron Star EOS?
Institute of Physics, Silesian University in OpavaGabriel Török, Martin Urbanec, Karel Adámek, Pavel Bakala, Eva Šrámková, Zdeněk Stuchlík
CZ.1.07/2.3.00/20.0071 Synergy , GAČR 209/12/P740, 202/09/0772, SGS-01-2010, www.physics.cz
1. Outline
1. Introduction: QPOs2. NS Compactness C (another introduction)3. Epicyclic Resonance Model – Falsification using condition for
Paczynski Modulation, C < 1 4. General Implications of Paczynski Modulation Mechanism
(disc oscillation models): report on a work in progress
• density comparable to the Sun• mass in units of solar masses• temperature ~ roughly as the T Sun• more or less optical wavelengths
MOTIVATION
Companion:
Compact object:- black hole or neutron star (>10^10gcm^3)
>90% of radiation in X-ray
LMXB Accretion disc
Observations: The X-ray radiation is absorbed by the Earth atmosphere and must be studied using detectors on orbiting satellites representing rather expensive research tool. On the other hand, it provides a unique chance to probe effects in the strong-gravity-field region (GM/r~c^2) and test extremal implications of General relativity (or other theories).
T ~ 10^6K
Figs: space-art, nasa.gov
2. Introduction: QPOs
LMXBs
Fig: nasa.gov
LMXBs short-term X-ray variability:peaked noise (Quasi-Periodic Oscillations)
• Low frequency QPOs (up to 100Hz)• hecto-hertz QPOs (100-200Hz),...• HF QPOs (~200-1500Hz): Lower and upper QPO feature forming twin peak QPOs
frequency
pow
er
Sco X-1
The HF QPO origin remains questionable, it is most often expected that it is associated to orbital motion in the inner part of the accretion disc.
Individual peaks can be related to a set of oscillators, as well as to time evolution of a single oscillator.
2. Introduction: QPOs
MOTIVATION
Pow
er
Frequency
height h width w at ½ h
Quality factor Q indicates sharpness of the peak, Q ~ h/w
Amplitude r indicates strength of peak variability (its energy) in terms of “rms amplitude” = percentual fraction (root mean square fraction) of the peak energy with the respect to the total countrate(r ~ area under peak)
BH QPOs (Galactic microquasars):frequencies up to 500Hzlow amplitude and Q : typically up to r~5% and Q~5NS QPOs:frequencies up to 1500Hzoften amplitudes up to r~20% and quality factors up to Q~200
2. Introduction: QPOs
KERR
3. NS Compactness
OBLATENESS
The influence of NS oblateness on orbital frequenies has been extensively studied in last decade, e.g.,Morsink, Stella, 1999, ApJ; Gondek-Rosińska, Stergioulas, Bulik, Kluźniak, Gourgoulhon, A&A (2001); Amsterdamski, Bulik, Gondek-Rosińska, Kluźniak, A&A (2002),…
Kluzniak et al., ApJ (1990)
Toro
k et
al.
(201
0),A
pJ
KERR
OBLATENESS
3. NS Compactness
KERR
OBLATENESSC =
RNS/
Rms
3. NS Compactness
KERR
OBLATENESSC =
RNS/
Rms
1
3. NS Compactness
KERR
OBLATENESSC =
RNS/
Rms
1
1
3. NS Compactness
KERR
OBLATENESSC =
RNS/
Rms
1
1
1
3. NS Compactness
KERR
OBLATENESSC =
RNS/
Rms
1
1
1
MAS
S
low mass
high mass
3. NS Compactness
C =
RNS/
Rms
3. NS Compactness
a) Observed frequencies are roughly equal to resonant eigenfrequencies.
b) Alternatively, there are large corrections to the resonant eigenfrequencies.
This for NSs FAILS.
Abramowicz et al., 2005
3. Epicyclic Resonance Model for NS QPOs and NS Mass Within the group of non-linear models suggested by Abramowicz and Kluzniak there is one specific (often quted and discussed) model which relates QPOs to the axisymmetric vertical and radial accretion disc oscillations (Abramowicz & Kluzniak 2001). These oscillations have frequencies equal to the vertical and radial frequency of the perturbed geodesic motion.Two distinct simplifications can be than assumed (see Urbanec et al. 2010, for refs):
Fig: J. Horák
For a non-rotating approximation it gives NS mass about (Bursa 2004, unp.).
The solution related to the high mass (i.e. Kerr) approximation thus cannot be trusted.
j
3. Epicyclic Resonance Model for NS QPOs and NS Mass
For a non-rotating approximation it gives NS mass about (Bursa 2004, unp.).
Mass-spin relations inferred assuming Hartle-Thorne metric and various NS oblateness.One can expect that the red/yellow region is allowed by NS equations of state (EOS).
q/j2
j
Urb
anec
et a
l., (2
010)
, A&
A
3. Epicyclic Resonance Model for NS QPOs and NS Mass
KERR
OBLATENESS
For a non-rotating approximation it gives NS mass about (Bursa 2004, unp.).
Mass-spin relations calculated assuming several modern EOS (of both “Nuclear” and “Strange” type) and realistic scatter from 600/900 Hz eigenfrequencies.
j
3. Epicyclic Resonance Model for NS QPOs and NS Mass
Urb
anec
et a
l., (2
010)
, A&
A
After
Abr
. et a
l., (2
007)
, Hor
ák (2
005)
4. Paczynski Modulation and NS Compactness Possible relation between the X-ray QPO phenomenon and general relativity
Bohdan Paczyński, 1987
”….suggest that the unsteady flow would make the boundary-layer luminosity variable, possibly giving rise to the X-ray quasi-periodic oscillation (QPO) phenomenon.”
REQUIRED CONDITION:
C = RNS/Rms < 1
4. Paczynski Modulation and NS Compactness
KERR
OBLATENESSC =
RNS/
Rms
1
1
1
MAS
S
low mass
high mass
(Epicyclic Resonance Model)
The condition for modulation is fulfilled only for rapidly rotating strange stars, which most likely falsifies the postulation of the 3:2 resonant mode eigenfrequencies being equal to geodesic radial and vertical epicyclic frequency….
(Typical spin frequencies of discussed sources are about 200-700Hz; based on X-ray bursts)
4. Paczynski Modulation and Implied Restrictions
Urb
anec
et a
l., (2
010)
, A&
A
5. Paczynski Modulation – General Implications
Almost any disc-oscillation model requires C<1
MAS
S [M
Sun]
SPIN [Hz]
Initial Distribution of NS[C<>1] =>
Distribution of QPO Sources
5. Paczynski Modulation – General Implications
Almost any disc-oscillation model requires C<1
Mass [M
sun]
0 1 1.5 2SPIN [Hz]
MAS
S [M
Sun]
Initial Distribution of NS (one concrete EoS)
5. Paczynski Modulation – General Implications
Almost any disc-oscillation model requires C<1
Mass [M
sun]
0 1 1.5 2SPIN [Hz]
MAS
S [M
Sun]
Initial Distribution of NS (one concrete EoS)
5. Paczynski Modulation – General Implications
0 500 1000 1500 Spin [Hz]
Mass [M
sun]
0 1 1.5 2
MAS
S [M
Sun]
SPIN [Hz]
Resulting Distribution of QPO sources (the same EoS)
5. Paczynski Modulation – General Implications
0 500 1000 1500 Spin [Hz]
Mass [M
sun]
0 1 1.5 2
MAS
S [M
Sun]
SPIN [Hz]
Resulting Distribution of QPO sources(another example)
5. Paczynski Modulation – General Implications M
ass [Msun]
0 1 1.5 2
Num
ber o
f Sou
rces
SPIN [Hz]
6. Conclusions
Mass [M
sun]
0 1 1.5 2
Num
ber o
f Sou
rces
SPIN [Hz]
END
Thank you for your attention…