magnetic eld e ects on compact stars - astrophysics@gu · 2016-01-19 · magnetic eld e ects on...
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Magnetic field effects oncompact stars
Mon.Not.Roy.Astron.Soc. 456 (2015) 2937-2945
Phys.Rev. D92 (2015) 8, 083006
Bruno FranzonCollaborators: V. Dexheimer, S. Schramm
Frankfurt Institute for Advanced Studies
Astrocoffee, January 2016
Plan of the talk
I Motivation
I Effects of magnetic field on the Equation of State
I Magnetized Neutron Stars: fully-general relativistic approachLangage Objet pour la RElativite NaumeriquE (LORENE)
I Results
I Summary
Motivation: magnetic fields
Earth: B∼ 0.5 G
MR: B∼ 103 G
Atlas: B∼ 1020 G
Neutron stars with astrong magnetic field:Duncan and Thompson (1992),Thompson and Duncan (1996).
Typical NS: Bs ∼ 1012 GMagnetars: Bs > 1014 G
Motivation: magnetic fields
Surface magnetic field and atthe pole:
Bd = 3.2× 1019√
PP G
Virial theorem: Bc ∼ 1018 GOrigin?
Duncan, Thompson, Kouveliotou
How to model highly magnetized stars
Einstein Equation
Rµν − 12Rgµν = 8πGTµν
Geometry
1. Spherical: TOV2. Perturbation3. Fully-GR
Energy Content
1. Matter: particles2. Fields: magneticfield
Magnetized EoS
I. An extended hadronic and quark SU(3) non-linear realization ofthe sigma model that describes magnetized hybrid stars containingnucleons, hyperons and quarks. See, e.g. Hempel M. at all(2013); Dexheimer V., Schramm S. (2008, 2010).II. The anomalous magnetic moment of the hadrons.III. Landau levels ν:
E∗iνs
=
√k2zi +
(√M∗2
i + 2ν|qi |B − siκiB)2
IV. Effect of B on the EoS:
0
0.2
0.4
0.6
0.8
1
1.2
1.4
1.6
1.8
0 2 4 6 8 10 12 14
p (
fm-4
)
ε (fm-4
)
B = 0B = 9.4x18
18 G
Fully-General Relativistic Approach
• Stationary neutron stars with no magnetic-field-dependent EoSwere studied by Bonazzola (1993), Bocquet (1995).• magnetic fields effects in the EoS was presented in Chatterjee(2014), for a quark EoS.• Our case: nucleons, hyperons, mixed phase with quarks,AMM of all hadrons (even the uncharged ones):
I. much more complex EoSII. much higher magnetization
Mathematical setupI The energy-momentum tensor: Chatterjee at all. 2014
Tµν = (e + p)uµuν + pgµν
+m
B(bµbν − (b · b)(uµuν + gµν))
+1
µ0
(−bµbν + (b · b)uµuν +
1
2gµν(b · b)
)where m and B are the lengths of the magnetization andmagnetic field 4-vectors.
I In the rest frame of the fluid:
Tµν = fluid + magnetization + field (z direction)
Tµν =
e+ B2
2µ00 0 0
0 p−mB+ B2
2µ00 0
0 0 p−mB+ B2
2µ00
0 0 0 p − B2
2µ0
Mathematical setup
I Stationary and axisymmetric space-time, the metric is writtenas:
ds2 = −N2dt2 + Ψ2r 2 sin2 θ(dφ− Nφdt)2 + λ2(dr 2 + r 2dθ2)
where Nφ, N, Ψ and λ are functions of (r , θ).
I A poloidal magnetic field satisfies the circularity condition:
Aµ = (At , 0, 0,Aφ)
I The magnetic field components as measured by the observer(O0) with nµ velocity can be written as:
Bα = −12εαβγσF γσnβ =
(0, 1
Ψr2 sin θ∂Aφ
∂θ ,−1
Ψ sin θ∂Aφ
∂r , 0)
At ,Aφ → Maxwell Equations. Static case : no electric field
3+1 decomposition of Tµν
I Total energy density (fluid + field): Chatterjee at all. 2014
E = Γ2(e + p)− p + 12µ0
(B iBi )
I and the momentum density flux can be written as:
Jφ = Γ2(e + p)U + 1µ0
(mB B iBiU
).
I 3-tensor stress components are given by:
S rr = p + 1
2µ0(BθBθ − B rBr ) + 2m
BBθBθ
Γ2
Sθ θ = p + 12µ0
(B rBr − BθBθ) + 2mB
BrBrΓ2
Sφφ = p + Γ2(e + p)U2 + 12µ0
[B iBi + 2m
B (1 + Γ2U2)BiBiΓ2
]with Γ = (1− U2)−
12 the Lorenz factor and U the fluid velocity
defined as:
U =Ψr sin θ
N(Ω− Nφ)
I Remember: p = p (h,B), with h(r , θ) := ln(
e+pmbnbc2
)
Field equations: our 4 unknowns N, Nφ, Ψ, λ
I Einstein equations: Rµν − 12 Rgµν = 8πGTµν
∆3ν = 4πGλ2(E + S i
i
)+
Ψ2r 2 sin2 θ
2N2(∂Nφ)2 − ∂ν∂(ν + β)
∆(Nφr sin θ) = −16πGNλ2
Ψ
Jφr sin θ
− r sin θ∂Nφ∂(3β − ν)
∆2[(NΨ− 1)r sin θ] = 8πGNλ2Ψr sin θ(S rr + Sθθ )
∆2(ν + α) = 4πGλ2(E + Sφφ ) +Ψ2r 2 sin2 θ
2N2(∂Nφ)2 − ∂ν∂(ν + β)
I Definitions:ν = ln N, α = ln λ, β = ln Ψ
∆2 =
(∂2
∂r2 + 1r∂∂r
+ 1r2
∂2
∂2θ
)∆3 =
(∂2
∂r2 + 2r∂∂r
+ 1r2
∂2
∂2θ+ 1
r2 tan θ∂∂θ
)∆3 = ∆3 − 1
r2 sin2 θ
E = E (PF ) + E (EM)
S ii = S
(PF ) ii + S
(EM) ii (i = r , θ and φ)
Structure of the star
I MassM =
∫λ2Ψr 2 ×
[N(E + S) + 2NφΨ(E + p)Ur sin θ
]sin θdrdθdφ
I Circumferential RadiusRcirc = Ψ(req,
π2 )req
Increasing of the mass due to the magnetic field andeffect of EoS(B) and magnetization m
1
1.2
1.4
1.6
1.8
2
2.2
2.4
2.6
0.16 0.18 0.2 0.22 0.24 0.26 0.28 0.3 0.32 0.34
Mg/M
O•
Hc (c2)
TOVµ = 1.0x10
32 Am
2- no EoS(B), no mag
EoS(B), no magEoS(B), mag
µ = 2.0x1032
Am2- no EoS(B), no mag
EoS(B), no magEoS(B), mag
µ = 3.0x1032
Am2- no EoS(B), no mag
EoS(B), no magEoS(B), mag
µ = 3.5x1032
Am2- no EoS(B), no mag
EoS(B), no magEoS(B), mag
B. Franzon, V. Dexheimer, S. Schramm, MNRAS, 456 (2015) 2937-2945
→ Very small reduction of stellar masses due to magnetization(negative sign in Tµν).→ Effect on the maximum mass through the effect on the equation ofstate is negligible.
Deformation due to the magnetic field
→ The maximum mass for the value µ = 3.5× 1032 Am2.→ It corresponds to a central enthalpy of Hc = 0.26 c2
(n = 0.463 fm−3).→ The gravitational mass obtained for the star is 2.46 M for a centralmagnetic field of 1.62×1018 G.
→ The ratio between the magnetic pressure and the matter pressure in
the center for this star is 0.793.
Mass-Radius Diagram for different fixed magneticmoments µ
0.5
1
1.5
2
2.5
3
11 12 13 14 15 16
Mg/ M
O•
Rcirc (km)
TOV
µ = 1.0x1032
Am2
µ = 2.0x1032
Am2
µ = 3.0x1032
Am2
µ = 3.5x1032
Am2
MB = 2.20 M
O·
B. Franzon, V. Dexheimer, S. Schramm, MNRAS, 456 (2015) 2937-2945
→ Effects of the magnetic field into the equation of state and themagnetization are also included.→ The gray line shows an equilibrium sequence for a fixed baryon massof 2.2M.
→The full purple circles represent a possible evolution from a highly
magnetized neutron star to a non-magnetized and spherical star.
Global Quantities for a star with fixed MB = 2.20M
0.25
0.3
0.35
0.4
0.45
0.5
0.55
0.6
0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1
nB
c(f
m-3
)
Bc(1018
G)
1.91 1.92 1.93 1.94 1.95 1.96 1.97 1.98 1.99
2 2.01 2.02
0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1
Mg/M
O•
Bc(1018
G)
0.4
0.5
0.6
0.7
0.8
0.9
1
1.1
0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1
r p/r
eq
Bc(1018
G)
0
0.5
1
1.5
2
2.5
3
3.5
4
0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1
µ (
10
32 A
m2)
Bc(1018
G)
→ Change in behaviour for Bc ∼ 0.9− 1.0× 1018 G. At this point, themagnetic force has pushed the matter off-center and a topologicalchange to a toroidal configuration can take place Cardall (2001).→ The ratio between the polar and the equatorial radii can reach 50%for a magnetic field strength of ∼ 1× 1018 G at the center.
Population change for a star with MB = 2.20M
0.001
0.01
0.1
1
900 1100 1300 1500
Yi
B = 0n
p
star center
µ Λ
du
s
900 1100 1300 1500
µ = 1.0x1032
Am2
0.001
0.01
0.1
1
900 1100 1300 1500
Yi
µB (MeV)
µ = 2.0x1032
Am2
900 1100 1300 1500
µB (MeV)
µ = 3.5x1032
Am2
0.5
1
1.5
2
2.5
3
11 12 13 14 15 16
Mg/
MO•
Rcirc (km)
TOV
µ = 1.0x1032
Am2
µ = 2.0x1032
Am2
µ = 3.0x1032
Am2
µ = 3.5x1032
Am2
MB = 2.20 M
O·
B. Franzon, V. Dexheimer, S. Schramm, MNRAS, 456 (2015) 2937-2945
→ As one increases the magnetic field, the particle population changesinside the star.→ These stars are represented in MR diagram by the full purple circles.
→ Younger stars that possess strong magnetic fields might go through a
phase transition later along their evolution, when their central densities
increase enough for the hyperons and quarks to appear.
Properties of White Dwarfs
→ The sizes are the size of the planet Earth→ Densities 105−9g/cm3
→ Typical composition : C and/or O→ Gravity is balanced by the electron degeneracy pressure
→ The masses are up to 1.4 Msun, the Chandrasekhar limit
Progenitors of Type Ia supernovae: Chandrasekhar White Dwarfs
Standard candles
EXPANSION OF THE UNIVERSE 2011
Saul PerlmutterBrian P. SchmidtAdam G. Riess
”for the discovery of the accelerating expansion of the Universe through
observations of distant supernovae”
Properties of White Dwarfs
→ But, motivated by observations of supernova that appears to bemore luminous than expected (e.g. SN 2003fg, SN 2006gz, SN 2007if,SN 2009dc), it has been argued that the progenitor of such super-novaeshould be a white dwarf with mass above the well-known Chandrasekharlimit: 2.0 - 2.8 Msun .
→ Several magnetized WDs discovered with surface fields of 105 − 109
G→ For a typical white dwarf: Bmax ∼ 1013 G→ It has been suggested that strongly magnetized white dwarfs canviolate the Chandrasekhar mass limit significantly (Kundu,Mukhopadhyay 2012)
• The new mass limit could explain super-luminous Type Iasupernovae from exploding white dwarfs
Mass-radius diagram for magnetized white dwarfs
0
2
4
6
8
10
12
14
16
18
0 0.2 0.4 0.6 0.8 1 1.2 1.4 1.6 1.8 2 2.2 2.4
WD mass (Msun)
Radius (106 m)
Chandrasekhar white dwarfs
Bc = 1.1x1011
Gauss
Bc = 1.3x1012
Gauss
Bc = 5.4x1012
Gauss
Bc = 3.9x1013
Gauss
Franzon, B. ; Schramm, S. 2015, Physical Review D, 92, 083006
→ Magnetic field effects can considerably increase the star masses and,therefore, might be the source of superluminous SNIa.
Summary
• Self-consistent stellar model including a poloidal magnetic field• Effects of the magnetic field on the equation of state, includingthe magnetization.• Leading contribution to the macroscopic properties of stars, likemass and radius, comes from the pure field contribution of theenergy-momentum tensor.• Assuming that the magnetic field decays over time, stars wouldnot only become less massive and smaller over time, but also gothrough phase transitions to more exotic phases.• Observables: distinct change in the cooling and stellar brakingindex: in preparation.• Magnetic field effects can considerably increase WD masses
Thank you!