The formation of low-mass helium white dwarfs orbiting pulsars - Evolution of low-mass X-ray binaries below the bifurcation period

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Volume 571 (November 2014)

A&A, 571 (2014) A45

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Table 1

Observed MSPs with He WD companions in tight circular orbits.

Pulsar name	P _orb	M _WD	M _NS	Eccentricity	P _spin	Ṗ	WD age	Optical data
	(h)	(M_⊙)	(M_⊙)		(ms)	(ss^-1)	(Gyr)	reference

PSR J0348+0432	2.46	0.17	2.01	2.6 × 10^-6	39.1	2.41 × 10^-19	2.1 ± 0.5	Antoniadis et al. (2013)
PSR J0751+1807	6.31	0.14	1.34	7.1 × 10^-7	3.48	7.79 × 10^-21	–	Lundgren et al. (1995)
PSR J1738+0333	8.52	0.18	1.47	4.0 × 10^-6	5.85	2.41 × 10^-19	–	Antoniadis et al. (2012)
PSR J1816+4510	8.66	0.21^a	2.0^a	8 × 10^-6	3.19	4.31 × 10^-20	–	Kaplan et al. (2013)

PSR J0024−7204U	10.3	0.15^b	1.5^b	< 10^-4	4.34	–	0.6	Edmonds et al. (2001)
PSR J1748−2446M	10.6	0.17^b	1.5^b	< 10^-4	3.57	–	–
PSR J1748−2446V	12.1	0.15^b	1.5^b	< 10^-4	2.07	–	–
PSR J0024−7204Y	12.5	0.17^b	1.5^b	< 10^-4	2.20	–	–
PSR J1641+3627D	14.2	0.22^b	1.5^b	< 10^-4	3.12	–	–
PSR J1012+5307	14.5	0.16	1.64	< 8.4 × 10^-7	5.26	1.71 × 10^-20	–	Callanan et al. (1998)

Notes. The top four systems have P_orb< 9h (i.e. solutions) and are found in the Galactic field. The bottom six systems are intermediate systems with P_orb = 9−15h, of which five systems are located in globular clusters.

^(a)

This value is very uncertain. Kaplan et al. (2013) find M_WDsin³i = 0.193 ± 0.012 M_⊙ and M_NSsin³i = 1.84 ± 0.11 M_⊙, where i is the unknown orbital inclination angle. Assuming M_NS ≤ 2.0 M_⊙ yields M_WD ≤ 0.21 M_⊙. From pulsar timing (Stovall et al. 2014) a strict lower limit on the minimum companion mass is M_WD = 0.16 M_⊙ (assuming i = 90° and M_NS = 1.4 M_⊙).

^(b)

For these systems we estimated M_WD by assuming M_NS = 1.5 M_⊙ and an orbital inclination angle of 60°.

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