An accreting dwarf star orbiting the S-type giant star π1 Gru

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Volume 699 (July 2025)

A&A, 699 (2025) A22

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Table 2.

Characteristics of the three components of the π¹ Gru system.

Parameter	A	B	C – MS scenario	C – WD scenario
Spectral type	S5,7 (1)	G0V (2)	K1V $_{K 7 V}^{F 9.5 V}$ ${}^\mathrm {F9.5V}_\mathrm {K7V}$	D?
R (R_⊙)	319±23 (3, 4)	1.10 (5)	$0 . 80_{- 0.17}^{+ 0.34}$ $0.80^{+0.34}_{-0.17}$	0.009±0.002
L (L_⊙)	7440 (6)	1.35 (5)	$0 . 41_{- 0.31}^{+ 1.10}$ $0.41^{+1.10}_{-0.31}$	Unknown
T_eff (K)	3200 (3)	5930 (5)	$5170_{- 1070}^{+ 820}$ $5170^{+820}_{-1070}$	Unknown
M_ZAMS (M_⊙)	2.0 (7)	1.06 (5)	$0 . 86_{- 0.20}^{+ 0.22}$ $0.86^{+0.22}_{-0.20}$	∼3−4
M_current (M_⊙)	1.5 (7)	1.06 (5)	$0 . 86_{- 0.20}^{+ 0.22}$ $0.86^{+0.22}_{-0.20}$	$0 . 86_{- 0.20}^{+ 0.22}$ $0.86^{+0.22}_{-0.20}$

Notes. R and L denote the radius and luminosity, respectively; T_eff is its effective temperature. For component C, the parameters are determined in this work. The MS spectral type, radius, luminosity, and effective temperature are taken from (5) using our derived mass. The WD radius is derived from (8) and its initial mass is inferred from (9). References: (1) Keenan (1954); (2) Feast (1953) and Ake & Johnson (1992); (3) Paladini et al. (2018); (4) Gaia Collaboration (2023); (5) Pecaut & Mamajek (2013); (6) Van Eck et al. (1998); (7) Mayer et al. (2014); (8) Nauenberg (1972); (9) Miller Bertolami (2016).

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