Multipolar magnetic configuration: A trace of post-mergers events in circumstellar disks around FS CMa stars

Open Access

Table 1.

Initial conditions and parametrization of the setup used in our simulations.

		Parameter	Value
Physical setup	Central star

	Mass	M_⋆	6 M_⊙
	Radius	R_⋆	3 R_⊙
	Magnetic field	B_⋆	6.2 kG
	Break-up speed	$Ω_{br} = \sqrt{G M_{⋆} / R_{⋆}^{3}}$ $\Omega_{\mathrm{br}} =\sqrt{GM_\star/R_\star^3}$	2.966 × 10⁻⁴ s⁻¹
	Stellar rotating rate	Ω_⋆	0.1Ω_br

	Disk

	Initial density	ρ_d0	1 × 10⁻¹³ g cm⁻³
	Aspect ratio	h	0.1
	Viscosity	α_ν	1.0R₀²Ω_⋆
	Magnetic resistivity	α_m	1.0R₀²Ω_⋆

	Corona

	Initial density	ρ_atm⁰	1 × 10⁻¹⁵ g cm⁻³
	Viscosity	α_ν	0.0
	Magnetic resistivity	α_m	0.0

Computational setup	Mesh

	Radial extension	R	[1R_⋆, 60R_⋆]
	Colatitude extension	θ	[0, π]
	Radial resolution	N_R	436 cells
	Colatitude resolution	N_θ	200 cells
	Radial spacing	log	logarithmic

	Normalization

	Length	R₀ = R_⋆	2.087 × 10¹¹ cm
	Density	ρ₀ = ρ_d0	1 × 10⁻¹³ g cm⁻³
	Velocity	$V_{K 0} = \sqrt{G M_{⋆} / R_{0}}$ $V_{K0}=\sqrt{GM_\star/R_0}$	6.193 × 10⁷ cm/s
	Time	t₀ = R₀/v_K0	3.37 × 10³ s
	Rotation period	T₀ = 2πt₀	2.12 × 10⁴ s
	Reference field	$B_{0} = \sqrt{4 π ρ_{d 0} V_{K 0}^{2}}$ $B_{0}=\sqrt{4\pi\rho_{d0} V_{K0}^{2}}$	69.42 G
	Star magnetic field	B_⋆ = μB₀	6.2 kG with μ = 89.3
	Accretion Rate	${\dot{M}}_{0} = ρ_{0} V_{K 0} R_{0}^{2}$ $\dot{M}_0={\rho_{0} V_{K0}R_0^{2}}$	4.257 × 10⁻⁹ M_⊙ yr⁻¹

Notes. The parameter μ appearing in B_⋆ specifies the ratio between the stellar surface magnetic field and the reference magnetic field strength.

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