Cyclic variability of the circumstellar disk of the Be star ζ Tauri - II. Testing the 2D global disk oscillation model

A. C. Carciofi; A. T. Okazaki; J.-B. le Bouquin; S. Štefl; Th. Rivinius; D. Baade; J. E. Bjorkman; C. A. Hummel

doi:10.1051/0004-6361/200810962

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Volume 504 / No 3 (September IV 2009)

A&A, 504 3 (2009) 915-927

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Table 1:

Model parameters for $\zeta$ Tau.
Parameter	Value	Type	Ref.^a
Stellar parameters
Spectral Type	B1IVe shell	fixed	2, 3
$R_{\rm p}$	$5.9~R_{\hbox{$\odot$ }}$	fixed	2, 4
$R_{\rm e}$	$7.7~R_{\hbox{$\odot$ }}$	fixed^b	1
$T_{\rm p}$	$25~000~\rm K$	fixed	2
$T_{\rm e}$	$17~950~\rm K$	fixed^c	1
$V/V_{\rm crit}$	0.8	fixed	5
$V_{\rm crit}$	$530~\rm km~s^{-1}$	free	1
M	$11.3~M_{\hbox{$\odot$ }}$	fixed^d	1
L	$7400~L_{\hbox{$\odot$ }}$	fixed	1
$T_{\rm eff}$	$19~370~\rm K$	fixed^e	1
Disk parameters
$\Sigma_0$	$2.1~\rm g~cm^{-2}$	free	1
$\rho_0$	$5.9 \times 10^{-11}~\rm g~cm^{-3}$	fixed^g	1
$R_{\rm t}$	$130~R_{\hbox{$\odot$ }}$	fixed	1
H₀	$0.208~R_{\hbox{$\odot$ }}$	fixed^f	1
V/R parameters
P	1429 d	Fixed	2
T₀	50414	Fixed	2
k₂	0.006	Free	1
Weak line force	$5.74\times 10^{-2}(\varpi/R_{\rm e})^{0.1}$	Free	1
$\dot{M}$	$10^{-11}~M_{\hbox{$\odot$ }}~\rm yr^{-1}$	Free	1
$\alpha$	0.4	Free	1
$\delta$	0.95	Free	1
Geometrical parameters
i	$95\hbox{$^\circ$ }$	free	1
$\gamma$	$32\hbox{$^\circ$ }$	free	1
$\phi_0$	$280\hbox{$^\circ$ }$	free	1
distance	126 pc	fixed^h	6
Binary parameters
$P_{\rm orb}$	132.97 d	fixed	7
e	0	fixed	7
a	$257~R_{\hbox{$\odot$ }}$	fixed	7
q	0.121	fixed	7

^a References: 1) this work; 2) Paper I; 3) Yang et al. (1990); 4) Harmanec (1988); 5) Cranmer (2005); 6) Perryman et al. (1997); 7) Harmanec (1984); ^b $R_{\rm e}$ was calculated from $R_{\rm p}$ and $V/V_{\rm crit}$ for a rigidly rotating star in the Roche approximation; ^c the equatorial temperature, $T_{\rm e}$ , was calculated from $V/V_{\rm crit}$ and $T_{\rm p}$ for a rigidly rotating star in the Roche approximation; ^d M was calculated from $V_{\rm crit}$ ; ^e $T_{\rm eff}$ corresponds to the average effective temperature of a rotationally deformed, gravity darkened star; ^f H₀ was calculated from Eq. (8), assuming a mean molecular weight of 0.6 and an electron temperature of $18~000~\rm K$ after Carciofi & Bjorkman (2006); ^g $\rho_0$ is given by $\Sigma_0(2\pi)^{-1/2}H_0^{-1}$ (Eq. (10)); ^h d was considered a free parameter within the 113-148 pc range, corresponding to the accuracy in the distance determination the Hipparcos satellite.

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