Rotating neutron star models with a toroidal magnetic field - SFB/TR7

Results for realistic equations of state
16
3×10 −6
2×10 −6
• BalbN1H1
• GlendNH3
• Pol2C10
2×10 −7 3×10 −7
c B Pol2F10 •
1×10 −6
• SLy4
Pol2 •
AkmalPR
BBB2 •
• FPS
• BPAL12
0
0 1×10 −7 4×10 −7
Distortion coefficients for realistic
equations of state for
models with M = 1.4 M ⊙ in the
non-rotating and non-magnetized
case. The star radius
increases as a function of the
EOS from BPAL12 bottom left
to GlendNH3 top right. Pol2
labels a relativistic model based
upon a γ = 2 polytropic
EOS with a radius of R =
12km. Pol2F10 denotes the
coefficients of a model at the
Newtonian limit with a radius
of R = 10km, Pol2C10 the
corresponding values given
by Cutler (2002).
c Ω
( ) 2 ( ) 2
¯B f
ɛ = ɛ B + ɛ Ω = −c B + c
10 15 Ω , ¯B = 〈B 2 〉 1/2 . (9)
G Hz
Joachim Frieben Golm, June 18, 2007