Triple trouble with PSR J1618−3921: Mass measurements and orbital dynamics of an eccentric millisecond pulsar

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Volume 691 (November 2024)

A&A, 691 (2024) A22

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Table 1.

Binary parameters for all currently known Galactic-disc eccentric MSPs.

Pulsar	P (ms)	P_b (d)	e	M_PSR (M_⊙)	M_c (M_⊙)	M_c, theo (M_⊙)	Presumable	Refs.
							nature of system
J1903+0327	2.1499	95.1741	0.4367	1.667(21)	1.029(8)	–	Disrupted triple	i, j

J1618−3921	11.9873	22.7456	0.0274	$1 . 20_{- 0.20}^{+ 0.19}$ $1.20^{+0.19}_{-0.20}$	$0 . 20_{- 0.03}^{+ 0.11}$ $0.20^{+0.11}_{-0.03}$	0.269–0.297	Triple	e, f, here

J1950+2414	4.3048	22.1914	0.0798	1.496(23)	0.2795 $_{- 0.0038}^{+ 0.0046}$ $^{+0.0046}_{-0.0038}$	0.268–0.296	Binary	a, b
J2234+0611	3.5766	32.0014	0.1293	1.353 $_{- 0.017}^{+ 0.014}$ $^{+0.014}_{-0.017}$	0.298 $_{- 0.012}^{+ 0.015}$ $^{+0.015}_{-0.012}$	0.281–0.310	Binary	c, d
J1946+3417	3.1701	27.0199	0.1345	1.827(13)	0.2654(13)	–	Binary	g, h
J1146−6610	3.7223	62.7712	0.0074	–	–	0.307–0.339	Binary	k
J0955−6150	1.9993	24.5784	0.1175	1.71(2)	0.254(2)	0.271–0.300	Binary	l

Notes. The first columns show the pulsar period, P, in milliseconds, their orbital period, P_b, in days and their orbital eccentricity, e. In case mass measurements are available, the pulsar and companion mass, M_PSR and M_c, respectively, are given as well. For comparison, we also calculated the companion mass, M_c, theo, theoretically expected from the P_b-M_WD relation by Tauris & Savonije (1999).

Refs: (a) Knispel et al. (2015), (b) Zhu et al. (2019), (c) Deneva et al. (2013), (d) Stovall et al. (2019), (e) Edwards & Bailes (2001), (f) Octau et al. (2018), (g)Barr et al. (2013), (h) Barr et al. (2017), (i) Champion et al. (2008), (j) Freire et al. (2011), (k) Lorimer et al. (2021), (l) Serylak et al. (2022).

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