Quark star RX J1856.53754 and its mass
Kazunori Kohri
（郡
和範）
RESCEU, Univ. of Tokyo
K. Kohri, K. Iida and Katsuhiko Sato,
Prog. Thor. Phys. 105 (2002) in press
1
Contents
・
Introduction
・
Observations of RX J1856.5-3754
・
Two-temperature model?
・
Quark matter in bag model
・
Quark star
・
Systematic study of mass of the star
in bag model
・
Other constraint on mass of the star
・
Other theoretical model of quark matter
・
Conclusion
2
Introduction
Recent deep Chandra LETG+HRC-S
observations of RX J1856.5-3754
reports,
Drake et al., ApJ. 572 (2002) 996-1001
Black body of
X-ray luminosity,
Radiation radius
3
Distance toward RX
J1856.5-3754
Drake et al., ApJ. 572 (2002) 996-1001
4
Spectra of RX J1856.6-3754
Drake et al., ApJ. 572 (2002) 996-1001
5
The 3σequivalent width
upper limit to line features
Drake et al., ApJ. 572 (2002) 996-1001
6
XMM-Newton observation
V. Burwitz et al, astro-ph/0211536
7
RX J1856.5-3754 is quark
star?
i) No pulsation
ii) No spectral features
iii) Small radiation radius
8
Mass-radius relation of
compact star
(Quark star)
(White dwarf)
M
(Neutron star)
R
Courtesy of K. Iida
9
Two temperature model
with heavy-element atmosphere
F.Walter and J.Lattimer, ApJ (2002)
T.M. Braje and R.W. Romani, ApJ (2002)
X-ray
Hot
Cold
UV/Optical
Hot
X-ray
10
Broad band spectral fit
in two-temperature
blackbody
T. Braje and R.W. Romani, ApJ (2002)
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Quark matter
(zero-temperature uds quark matter)
Thermodynamic potential
QCD coupling constant
where
Energy density
Strange quark mass
Bag constant
12
Quark matter-2
Number density
Pressure
Baryon number
Conditions
In equilibrium through weak interactions
Charge neutrality
13
Bag model parameters
fitted to hadron mass
spectra
Kohri, Iida and Sato, arXiv:astro-ph/0210259
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Energy per baryon
(αｃ＝
0）
15
Energy per baryon
(αｃ＝0.6）
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Equation of state
17
Quark star
Equation of hydrostatic equilibrium
(Tolman-Oppenheimer-Volkoff (TOV) equation)
Equation of mass conservation
Then, the radius is determined by
The mass is
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Mass of quark star
19
Radius of quark star
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Mass-radius relation
21
Mass-radius relation
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Observed X-ray
luminosity
Bondi accretion rate
where,
Then,
23
Contours of upper
limit of mass
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Effects of the pressuredependent bag constant
Generally, we can parameterize the EOS as
A ~ 3 -- 4, for Lattice data , Peshier,Kampfer,Soff (2001).
A ~ 2, for Relativistic Mean Field, Dey et al. (1998) etc.
Then, we transform it into
where
Namely, inside the star the bag
constant effectively becomes large!
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Contour of the effective
bag constant
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Contours of the upper
limint of the mass
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Conclusion
・ We have systematically
computed mass-radius relation
of quark star within the bag
model.
・ Assuming that RX J1856.5-3754 is a pure quark star, we
have derived an upper limit on
its mass.
・ We find the upper limit can
amount to 1 M around
4
B ~ (200MeV).
28