Rotating neutron stars with nonbarotropic thermal profile Giovanni - - PowerPoint PPT Presentation

Rotating neutron stars with nonbarotropic thermal profile

Giovanni Camelio with Tim Dietrich, Miguel Marques, and Stephan Rosswog PRD 100:123001 (2019) 2020 February 10 Compact objects for all @ Lund

Motivation

dynamical simulation stationary code

9 10 11 12 13 14 15 16 Log( / g cm

3 )

2 1 1 2 Log ( T / MeV k

1 B )

• Perego et al., EPJ A55:124 (2019)

1 / 4

Motivation

dynamical simulation stationary code

9 10 11 12 13 14 15 16 Log( / g cm

3 )

2 1 1 2 Log ( T / MeV k

1 B )

10

2

10

1

100

• Perego et al., EPJ A55:124 (2019)

1 / 4

A new formulation for the Euler equation

gravity & centrifugal

• ∇ log

lapse Lorentz

• −Q

+ buoyancy ∇p

h (p, s) +

• diff. rotation
• F(l , Ω)∇Ω = 0

∇

• −Q(r, θ, Ω) +
• dp

h

• p, s(p)

+

• F

l (Ω), Ω

• dΩ = const
• dh = dp

ρ + T mn ds 1 ρ(p, s) = ∂h(p, s) ∂p

• s

T(p, s) mn = ∂h(p, s) ∂s

• p

∇Q = ∇p

h

+ F∇Ω 1

h (p, Ω) = ∂Q(p, Ω)

∂p

• Ω

F(p, Ω) = ∂Q(p, Ω) ∂Ω

• p

2 / 4

Barotropic vs nonbarotropic star with the XNS code

Q(p, Ω) = const + H(p) + F(Ω) + bH(p)F(Ω)

1 . 1 1 . 3 1.60 1.90 0.1 0.5 1 . 1.5 2 km 0.0 0.7 1.3 2.0 2.7 3.3 4.0 4.7 5.3 6.0 10

4 p

1.7 1.9 2.1 2.3 2.5 2.8 3.0 3.2 3.4 3.6 10

2

1 . 1 1.30 1.60 1.90 0.1 . 7 1.4 2.0 2 km 0.0 0.7 1.3 2.0 2.7 3.3 4.0 4.7 5.3 6.0 10

4 p

1.7 1.9 2.1 2.3 2.5 2.8 3.0 3.2 3.4 3.6 10

2

3 / 4

Conclusions

realistic thermal profiles are possible! Outlooks: ◮ restriction to Newtonian stars! ◮ modeling of the merger remnant (work in progress) ◮ modeling of the strange star after the hadron-quark transition ◮ accretion disks (work in progress) ◮ magnetic field & meridional currents ◮ neutrino-driven quasistationary evolution

4 / 4

Thanks!

Camelio, Dietrich, Marques, Rosswog, Rotating neutron stars with nonbarotropic thermal profile, PRD 100:123001, 2019 (arXiv:1908.11258) Editor’s suggestion

I am looking for job!

Validation with the dynamical BAM code

2 4 6 8 10 time [ms] 3.996 3.998 4.000 4.002 4.004 non barotropic barotropic central rest mass density

0/ n

Self consistent field method

Einstein equations (metric) Euler equation (matter) converged? no yes initial condition (spherical) end