The power of binary pulsars in testing Gauss-Bonnet gravity

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Volume 687 (July 2024)

A&A, 687 (2024) A17

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Table 1.

Parameters of the NS–WD pairs that were used to constrain the theory using the Ṗ_b method.

Quantity	J0348+0432 values	J1012+5307 values
Orbital period (P_b) in days	0.102424062722 ± 7 × 10⁻¹²	0.60467271355 ± 3 × 10⁻¹¹
Eccentricity (e)	2.6 × 10⁻⁶ ± 9 × 10⁻⁷	1.2 × 10⁻⁶ ± 3 × 10⁻⁷
Intrinsic ${\dot{P}}_{b}^{int}$ $\dot{P}_{\mathrm{b}}^{\mathrm{int}}$ in (fs.s⁻¹)	−274 ± 45	−2.1 ± 8.6
NS to WD mass ratio q ≡ m_p/m_c	11.70 ± 0.13	10.44 ± 0.11
Pulsar mass $m_{p}^{obs}$ $m_{\mathrm{p}}^{\mathrm{obs}}$ in M_⊙	$2 . 0065_{- 0.0570}^{+ 0.0755}$ $2.0065^{+0.0755}_{-0.0570}$	$1 . 72_{- 0.17}^{+ 0.18}$ $1.72^{+0.18}_{-0.17}$
Observed WD mass $m_{c}^{obs}$ $m_{\mathrm{c}}^{\mathrm{obs}}$ in M_⊙	$0 . 1715_{- 0.0030}^{+ 0.0045}$ $0.1715^{+0.0045}_{-0.0030}$	0.165 ± 0.015

Quantity	J2222−0137 values	J1738+0333 values

Orbital period (P_b) in days	2.445759995471 ± 6 × 10⁻¹²	0.3547907398724(13)
Eccentricity (e)	3.8092 × 10⁻⁴ ± 4 × 10⁻⁸	(3.4 ± 1.1)×10⁻⁷
Intrinsic ${\dot{P}}_{b}^{int}$ $\dot{P}_{\mathrm{b}}^{\mathrm{int}}$ in (fs.s⁻¹)	−10 ± 8	−25.9 ± 3.2
NS to WD mass ratio q ≡ m_p/m_c	n/a	8.1 ± 2
Pulsar mass $m_{p}^{obs}$ $m_{\mathrm{p}}^{\mathrm{obs}}$ in M_⊙	1.81 ± 0.03	$1 . 46_{- 0.05}^{+ 0.06}$ $1.46^{+ 0.06}_{-0.05}$
Observed WD mass $m_{c}^{obs}$ $m_{\mathrm{c}}^{\mathrm{obs}}$ in M_⊙	1.312 ± 0.009	$0 . 181_{- 0.007}^{+ 0.008}$ $0.181^{+0.008}_{-0.007}$

Notes. Antoniadis et al. (2013), Lazaridis et al. (2009), Guo et al. (2021), Mata Sánchez et al. (2020), Ding et al. (2020), Freire et al. (2012), Shao et al. (2017).

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