Missing for 20 yr: MeerKAT Redetects the Elusive Binary Pulsar M30B
V. Balakrishnan, P. C. C. Freire, S. M. Ransom, A. Ridolfi, E D Barr, W Chen, V. Venkatraman Krishnan, D. J. Champion, M. Kramer, T. Gautam, P V Padmanabh, Yunpeng Men, Federico Abbate, B. W. Stappers, I. H. Stairs, E. F. Keane, Andrea Possenti
Abstract
Abstract PSR J2140−2311B is a 13 ms pulsar discovered in 2001 in a 7.8 hr Green Bank Telescope observation of the core-collapsed globular cluster M30 and predicted to be in a highly eccentric binary orbit. This pulsar has eluded detection since then; therefore, its precise orbital parameters have remained a mystery until now. In this work, we present the confirmation of this pulsar using observations taken with the UHF receivers of the MeerKAT telescope as part of the TRAPUM Large Survey Project. Taking advantage of the beamforming capability of our backends, we have localized it, placing it 1.′2(1) from the cluster center. Our observations have enabled the determination of its orbit: It is highly eccentric ( e = 0.879) with an orbital period of 6.2 days. We also measured the rate of periastron advance, <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mover accent="true"> <mml:mrow> <mml:mi>ω</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>̇</mml:mo> </mml:mrow> </mml:mover> <mml:mo>=</mml:mo> <mml:mn>0.078</mml:mn> <mml:mo>±</mml:mo> <mml:mn>0.002</mml:mn> <mml:mspace width="0.25em"/> <mml:mi>deg</mml:mi> <mml:mspace width="0.25em"/> <mml:msup> <mml:mrow> <mml:mi>yr</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1</mml:mn> </mml:mrow> </mml:msup> </mml:math> . Assuming that this effect is fully relativistic, general relativity provides an estimate of the total mass of the system, M TOT = 2.53 ± 0.08 M ⊙ , consistent with the lightest double neutron star systems known. Combining this with the mass function of the system gives the pulsar and companion masses of m p < 1.43 M ⊙ and m c > 1.10 M ⊙ , respectively. The massive, undetected companion could either be a massive white dwarf or a neutron star. M30B likely formed as a result of a secondary exchange encounter. Future timing observations will allow the determination of a phase-coherent timing solution, vastly improving our uncertainty in <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mover accent="true"> <mml:mrow> <mml:mi>ω</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>̇</mml:mo> </mml:mrow> </mml:mover> </mml:math> and likely enabling the detection of additional relativistic effects, which will determine m p and m c .