The interplay between disk wind and magnetospheric accretion mechanisms in the innermost environment of RU Lup

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Volume 689 (September 2024)

A&A, 689 (2024) A124

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Table 1

RU Lup model configurations compared to VLTI GRAVITY data.

	Mag. accretion I	Mag. accretion II	Disk wind I	Disk wind II	Hybrid model I	Hybrid model II
	Axisymmetric	Non-axisymmetric	Single peaked	Double peaked	Cool + compact	Hot + extended
	(MA I)	(MA II)	(DW I)	(DW II)	(HM I)	(HM II)
R_* [R_⊙]	2.5	2.5	2.5	2.5	2.4	2.5
M_* [M_⊙]	0.8	0.8	0.8	0.8	1.2	0.8
T_* [K]	4050	4050	4050	4050	4050	4050
P_* [days]	7	7	7	7	9.05	7
R_co [R_*]	5.71	5.71	5.71	5.71	8.1	5.71
R_mi [R_*]	7	7	−	−	6	7
δR_m [R_*]	2	2	−	−	1	2
${\dot{M}}_{acc} [10^{- 8} M_{⊙} {y r}^{- 1}]$ $\[\dot{M}_{\text {acc }}\left[10^{-8} ~M_{\odot} ~\mathrm{yr}^{-1}\right]\]$	23	23	−	−	10	23
T_mag [K]	8600	8600	−	−	7100	8600
R_wi [R_*]	−	−	7.1	9.1	7.1	9.1
δR_w [R_*]	−	−	5	3	8	3
d_fp [R_*]	−	−	15	15	15	15
R_dd [R_*]	−	−	14.5	13	13	13
β_wind	−	−	0.62	0.05	0.2	0.05
α_wind	−	−	0.4	0.7	0	0.7
z_crit [au]	−	−	0.0516	0.02	0.005	0.02
M_loss [10⁻⁸ M_⊙ yr⁻¹]	−	−	5.1	12	10	12
β_ma [deg]	0	30	−	−	0	0

Notes. Descriptions of the physical nature of the respective model parameters are given in Sec. 3.2 for the accretion model and in Sec. 3.3 for the disk wind model. Note that R_co is implicitly defined by the stellar parameters.

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