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 2 1 B ) 1 Log ( T / MeV k 0 1 2 9 10 11 12 13 14 15 16 Log( / g cm 3 ) Perego et al., EPJ A55:124 (2019) � 1 / 4

Motivation dynamical simulation stationary code 2 10 0 1 B ) 1 Log ( T / MeV k 0 1 10 1 10 2 2 9 10 11 12 13 14 15 16 Log( / g cm 3 ) Perego et al., EPJ A55:124 (2019) � 1 / 4

A new formulation for the Euler equation gravity & centrifugal buoyancy diff. rotation � �� � � �� � � �� � lapse ∇ p ∇ log + h ( p, s ) + F ( l , Ω) ∇ Ω = 0 Lorentz � �� � − Q � � � � d p � l (Ω) , Ω � � + − Q ( r, θ, Ω) + dΩ = const ∇ F � h p, s ( p ) d h = d p ρ + T ∇ Q = ∇ p d s + F ∇ Ω m n h � � h ( p, Ω) = ∂Q ( p, Ω) 1 ρ ( p, s ) = ∂h ( p, s ) 1 � � � � ∂p � ∂p � Ω s � � F ( p, Ω) = ∂Q ( p, Ω) T ( p, s ) = ∂h ( p, s ) � � � � ∂ Ω m n ∂s � � p p 2 / 4

Barotropic vs nonbarotropic star with the XNS code Q ( p, Ω) = const + H ( p ) + F (Ω) + bH ( p ) F (Ω) 6.0 3.6 2 km 5.3 3.4 4.7 3.2 1.90 4.0 3.0 3.3 2.8 4 p 1.60 0.1 2 2.7 2.5 10 0.5 10 0 2.0 2.3 3 0 . 1 . 1 1.3 2.1 0 1 . 1.5 0.7 1 1.9 0.0 1.7 6.0 3.6 2 km 5.3 3.4 4.7 3.2 4.0 3.0 1.90 3.3 2.8 4 p 0.1 1.60 2 2.7 2.5 10 10 7 . 0 2.0 2.3 1.30 1.4 1.3 2.1 0 2.0 0.7 1 1.9 . 1 0.0 1.7 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 non barotropic barotropic n 0 / 4.004 central rest mass density 4.002 4.000 3.998 3.996 0 2 4 6 8 10 time [ms]

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