mass & radius of compact objects f astest pulsar and its stellar eos
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Mass & Radius of Compact Objects F astest pulsar and its stellar EOS. CHENGMIN ZHANG National Astronomical Observatories Chinese Academy of Sciences, Beijing. Significance of Measuring Star mass and radius – Neutron or Quark. - PowerPoint PPT PresentationTRANSCRIPT
Mass & Radius of Compact Objects Fastest pulsar and its stellar EOS
CHENGMIN ZHANG National Astronomical Observatories
Chinese Academy of Sciences, Beijing
Significance of Measuring Star mass and radius – Neutron or Quark
we can measure physical parameters of star, mass and radius, probe the nuclear physics and understand EOS
we can study the strong gravitational field, where Einstein GR might be tested
Neutron Stars ?
(Stairs 2004)
(MT77)
(Lattimer & Prakash 2004 , 2006)
40+ NSs, M=1.4 M⊙ , R= 10 -30 km ?
Radio pulsars, X-ray NS, binary systems
NS mass determined in Binary system
MSP, PSR J0751+1807, M = 2.1(2) M ⊙ ?; Nice et al. 20042A1822-371, M>0.97+-0.24 M⊙; Jonker et al 2003 ; ( 1.74 M ⊙ , 2008 )DNS: M=1.25M , M=1.34 ⊙ M , double pulsars (2004)⊙
PSR J0737-3039A/B Post-Keplerian Effects
R: Mass ratio
: periastron advance
: gravitational redshift
r & s: Shapiro delay
Pb: orbit decay
(Kramer et al. 2005)
.
.
• Six measured parameters – only two independent
• Fully consistent with general relativity (0.1%)
A: 1.34 M⊙ ; B: 1.25 M⊙
Measured M-R relations
Apparent Radius: R∞=R/(1-Rs/R)1/2
Gravitational redshift: z=(1-Rs/R)-1/2 -1 Mass density: M/R3 g=~M/R2
1E1207.4-5209, Aql X-1 and EXO 0748-676Rs=2GM: Schwarzschild radius
No direct measure of radius !
Photon Spectra: Key to Measuring Radius
For perfect Black Body:Observed Total Flux: F =4 R∞
2 SB T∞4/d2
R R
1- 2GM/Rc 2
T 1- 2GM/Rc 2 T
( 1- 2GM/Rc 2 (1 z)-1)Spectra are seldom black body: Neutron Stars have atmospheres !Composition and Magnetic field shape the spectra.
Other issues: Is the surface temperature and radiation isotropic ?
RX J1856.5-3754 (Fred Walter’s Star !)
The Mass-Radius
Gravitational Red-shift: observation of spectral lines (Cottam, et al 2002).
QPOs indicate ISCO
Exotic Stars
Typical twin kHz QPOs ( 24/35)Z: Sco x-1, van der Klis et al 2006
Separation ~300 Hz
~Spin ?
Typically: Twin KHz QPO
Upper ν2 ~ 1000 (Hz)
Lower ν1 ~ 700 (Hz)
Twin 21/27 sources ; ~290
Constrain star M_R by kHz QPOs
Inner boundary to emit kHz QPO: ISCO, R > MAX M, R
M<2.2 M⊙ (1kHz/freq) R<19.5 km (1kHz/freq) M/R3 relation known by model for twin kHz QPOs
SAXJ 1808.4: M/R3 by Burderi & King 1998
kHz QPOs from LMXBs: R-ISCO
kHz QPO maximum frequency constrains NS equations of state
Excluded
Sco X-1
Striking case of RX J1856.5-3754
Truempet et al. 2004; Burwitz et al. 2003
Apparent radius RApparent radius R∞∞=16.5 km (d/117pc), =16.5 km (d/117pc), Truempet 2005Truempet 2005 True radius 14 km (1.4 MTrue radius 14 km (1.4 M⊙⊙), stiff EOS, rule out quark star), stiff EOS, rule out quark star
This is an isolated neutron star (INS), valuable because: We can see the surface There are minimal magnetospheric complications If we can see the surface, we can determine the angular diameter The parallax gives the radius R spectral lines give the surface composition, T, and g R and g give M M/R constrains the EOS of matter at nuclear densities
Gravitational light bending effect: R/M <~10 km/M⊙ ; Ransom et al 2004
Einstein’s General Relativity: Perihelion precession
Precession Model for KHz QPO, Stella and Vietri, 1999
ν2 = νkepler
ν1 = νprecession = ν2 [1 – (1 – 3Rs/r)1/2]
∆ν = ν2 - ν1 is not constant
ISCO Saturation
Relativistic precession model by Stella & Vietri 1999
M inferred from twin kHz QPOs
Max frequency – ISCO
M/R3 inferred from twin kHz QPOs
Max frequency – Star Surface R
Kepler frequency νk = (GM/4π2r3)0.5
νk = 1850 (Hz) A X3/2
ν1 = ν 2X (1- (1-X)1/2)1/2
A2=m/R63; X=R/r, m=M/M⊙ , R6 = R/106 cm
Zhang 2004, AA; Li & Zhang 2005
Maximum kHz QPO occurs at R or ISCO=3Rs
A> νk /1850 (Hz) and m < 2200 (Hz)/ νk
Miller et al 1998
Constraining M – R by R∞ and z
1E 1207.4-5209: R∞=4.6 km, Bignami et al 2004 z=0.12-0.23; Sanwal et al 2002 ? R 6 =R∞6 /(1+z) M=f(z)R∞6 /(1+z) F(z)=(20/3)z(1+z/2)/(1+z)2
Constraining M – R by R∞ and A~M/R3
Aql X-1 : 9 km<R∞<18 km, Rutledge et al 2001
one kHz QPO: 1040 Hz; van der Klis 2006
R6 =R∞6 /(1+0.15(A/0.7)2 R2∞6 )0.5
m=AR36
Constraining M – R by A=M/R^3 and z
EXo 0728-676: z=0.35; Cottam et al 2002
One kHz QPO 695 Hz; Homan & van der Klis 2000
R6 =1.43f0.5(z)(0.7/A) m=1.43f1.5(z)(0.7/A) f(z)=(20/3)z(1+z/2)/(1+z)2
1E1207.4-5209,
Apparent radius, gravitational redshift
QUARK STAR ?
Aql X-1 ,
Apparent radius=14 km, single kHz QPO
EXO 0748-676 ,
gravitational redshift, kHz QPO
Mass-Radius relations
Apparent Radius: R∞=R/(1-Rs/R)1/2 Haensel 2001
Gravitational redshift: z=(1-Rs/R)-1/2 -1 Cottam et al 2003, z=0.35
Mass density: M/R3 (by kHz QPOs) Zhang 2004
1E1207.4-5209, Aql X-1 and EXO 0748-676
Rs=2GM: Schwarzschild radius
Measuring NS Mass & Radius
by kHz QPO, gravitational redshift and apparent radius
Measuring STAR Mass-Radius
by kHz QPO, gravitational redshift and apparent radius
CN1/CN2: normal neutron matter, CS1/CS2: quark star
CPC: Bose-Einstein condensate of pions
Zhang, Yin, Li, Xu, Zhang B, 2007
AqlX-1 , EXO 0748-676 Samples
How about the Sub-millisecond Pulsar XTE J1739285, spin=1122 Hz
Spin=1122 Hz Radio PSR, 716 Hz
Quark Star, FAST target
Cheng et al 1998,
Li 1999;
Xu, Qiao, Wang 2002
Horvath 2002
Harko, 2005
Zhang, ..Li, 2007
More……
ISCO condition, m ≤ 2200 (Hz)/spin Keplerian at R, crust split
Zhang et al. 2006
Max kHz QPO 1330 Hz
Cir X-1
dif
fere
nce
Rat
io
Spin Frequency - LMXBs
23 Spin sources, Av ~ 400 Hz
Radio MSP : Max Spin=716 Hz
Spin frequency:
Max: 1122 Hz, Kaaret et al 2007
Min: 45 Hz Villarreal & Strohmayer 2004
kHz QPO & spin relation
List of the Low-Mass X-Ray Binaries Simultaneously Detected Twin Kilohertz QPO and Spin Frequencies
QPO (Hz) spin Dnu/spin 4U 160852 . . . . . . . . 802–1099 619 1.3 4U 163653 . . . . . . . . 971–1192 581 1.7 4U 170243 . . . . . . . . . 1055 330 3.2 4U 172834 . . . . . . . . . 582–1183 363 1.6 KS 1731260 . . . . . . . . 1169 524 2.2 4U 191505 . . . . . . . . . 514–1055 270 1.9 XTE J1807294 . . . . . . 353–587 191 1.8 SAX J1808.43658 . . . .694 401 1.7 QPO data, Belloni et al. (2005), van der Klis (2006)
Fastest Pulsar XTE J1739-285 spin = 1122 Hz M – R Kaaret et al. 2007
Quark Star ?
Quark Star = sub-MSP ?
Summary
THANKS
Conclusions: M-R relations
1. Mass, measured
2. Radius, not measured directly
3. Spectra, MR relation
4. Redshift, M/R
5. kHz QPO, M/R^3, constraints
6. Others… Ozel 2006
Not clear: fuzzy in M-R
EOS: Quark or Neutron ?
Saturation of kHz QPO frequency ?ISCO – Star Mass
4U1820-30, NASA
Swank 2004; Miller 2004
BH/ISCO: 3 Schwarzschild radius
Innermost stable circular orbit
NS/Surface: star radius, hard surface