Missing for 20 yr: MeerKAT Redetects the Elusive Binary Pulsar M30B

Balakrishnan, V.; Freire, P. C. C.; Ransom, S. M.; Ridolfi, A.; Barr, E. D.; Chen, W.; Krishnan, V. Venkatraman; Champion, D. J.; Krämer, M.; Gautam, T.; Padmanabh, P. V.; Men, Yunpeng; Abbate, F.; Stappers, B. W.; Stairs, I. H.; Keane, E. F.; Possenti, A.

doi:10.3847/2041-8213/acae99

Cited by 8 publications

(2 citation statements)

References 66 publications

(93 reference statements)

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“…The magnetic field strength and the small P  suggest that PSR J2150+3427 may be slightly recycled. The high eccentricity is likely the aftermath of the supernova explosion of the companion star, which is consistent with the DNS systems showing high eccentricity (Tauris et al 2017;Pol et al 2019;Balakrishnan et al 2023) and two NS-WD systems (Davies et al 2002).…”

Section: Discussionsupporting

confidence: 85%

“…Most binary MSPs in our Galaxy are highly recycled (P 10 ms) and in highly circularized orbits (e 10 −3 ). The intermediate spin-period pulsars (10 ms P 20 ms; Camilo et al 2001;Balakrishnan et al 2023) tend to have a WD companion (Ferdman et al 2010), and their orbits have very low eccentricities. The rare DNS systems are survivors from two supernova explosions (Tauris et al 2017).…”

Section: System Originmentioning

confidence: 99%

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PSR J2150+3427: A Possible Double Neutron Star System

Wu,

Wang,

Yuan

et al. 2023

ApJL

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PSR J2150+3427 is a 0.654 s pulsar discovered by the Commensal Radio Astronomy FAST Survey. From the follow-up observations, we find that the pulsar is in a highly eccentric orbit (e = 0.601) with an orbital period of 10.592 days and a projected semimajor axis of 25.488 lt-s. Using 2.7 yr of timing data, we also measured the rate of periastron advance ω ̇ = 0.0115(4) deg yr−1. An estimate for the total mass of the system using the ω ̇ gives M tot = 2.59(13)M ⊙, which is consistent with most of the known double neutron star (DNS) systems and one neutron star (NS)–white dwarf (WD) system named B2303+46. Combining ω ̇ with the mass function of the system gives the masses of M p < 1.67 and M c > 0.98 M ⊙ for the pulsar and the companion star, respectively. This constraint, along with the spin period and orbital parameters, suggests that it is possibly a DNS system, and we cannot entirely rule out the possibility of an NS–WD system. Future timing observations will vastly improve the uncertainty in ω ̇ , and are likely to allow the detection of additional relativistic effects, which can be used to modify the values of M p and M c . With a spin-down luminosity of E ̇ = 5.07(6) × 1029 erg s−1, PSR J2150+3427 is a very low-luminosity pulsar, with only the binary pulsar J2208+4610 having a smaller E ̇ .

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Section: Discussionsupporting

confidence: 85%

Section: System Originmentioning

confidence: 99%

PSR J2150+3427: A Possible Double Neutron Star System

Wu,

Wang,

Yuan

et al. 2023

ApJL

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Discovery and timing of ten new millisecond pulsars in the globular cluster Terzan 5

Padmanabh,

Ransom,

Freire

et al. 2024

A&A

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We report the discovery of ten new pulsars in the globular cluster Terzan 5 as part of the Transients and Pulsars with MeerKAT (TRAPUM) Large Survey Project. We observed Terzan 5 at L-band (856--1712 MHz) with the MeerKAT radio telescope for four hours on two epochs, and performed acceleration searches of 45 out of 288 tied-array beams covering the core of the cluster. We obtained phase-connected timing solutions for nine discoveries, covering nearly two decades of archival observations from the Green Bank Telescope for all but one. Highlights include PSR J1748$-$2446ao which is an eccentric ($e = 0.32$) wide-orbit (orbital period $ = 57.55$ d) system. We were able to measure the rate of advance of periastron (omegadot ) for this system allowing us to determine a total mass of $3.17 With a minimum companion mass (Mc ) of $ PSR J1748$-$2446ao is a candidate double neutron star (DNS) system. If confirmed to be a DNS, it would be the fastest spinning pulsar ($P = 2.27$ ms) and the longest orbital period measured for any known DNS system. PSR J1748$-$2446ap has the second highest eccentricity for any recycled pulsar ($e 0.905$) and for this system we can measure the total mass ($1.997 and estimate the pulsar and companion masses and respectively). PSR J1748$-$2446ar is an eclipsing redback (minimum $ system whose properties confirm it to be the counterpart to a previously published source identified in radio and X-ray imaging. We were also able to detect omegadot for PSR J1748$-$2446au leading to a total mass estimate of $1.82 and indicating that the system is likely the result of Case A Roche lobe overflow. With these discoveries, the total number of confirmed pulsars in Terzan 5 is 49, the highest for any globular cluster so far. These discoveries further enhance the rich set of pulsars known in Terzan 5 and provide scope for a deeper understanding of binary stellar evolution, cluster dynamics and ensemble population studies.

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Neutron star mass in dark matter clumps

Deliyergiyev,

Del Popolo,

Le Delliou

2023

Monthly Notices of the Royal Astronomical Society

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This paper investigates a hypothesis proposed in previous research relating neutron star (NS) mass and its dark matter (DM) accumulation. As DM accumulates, NS mass decreases, predicting lower NS masses toward the Galactic center. Due to limited NSs data near the galactic center, we examine NSs located within DM clumps. Using the CLUMPY code simulations, we determine the DM clumps distribution, with masses from 10 to 108 M⊙ and scales from 10−3 to 10 kpc. These clumps’ DM exhibit a peak at the center, tapering toward the outskirts, resembling our Galaxy’s DM distribution. We analyse these DM clumps’ NS mass variations, considering diverse DM particle masses and galaxy types. We find relatively stable NS mass within 0.01 to 5 kpc from the clump center. This stability supports the initial hypothesis, particularly for NSs located beyond 0.01 kpc from the clump center, where NS mass reaches a plateau around 0.1 kpc. Nevertheless, NS mass near the clump’s periphery reveals spatial dependence: NS position within DM clumps influences its mass in Milky Way-type galaxies. Moreover, this dependence varies with the DM model considered. In summary, our study investigates the proposed link between NS mass and DM accumulation by examining NSs within DM clumps. While NS mass remains stable at certain distances from the clump center, spatial dependencies arise near the clump’s outer regions, contingent on the specific DM model.

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Missing for 20 yr: MeerKAT Redetects the Elusive Binary Pulsar M30B

Cited by 8 publications

References 66 publications

PSR J2150+3427: A Possible Double Neutron Star System

PSR J2150+3427: A Possible Double Neutron Star System

Discovery and timing of ten new millisecond pulsars in the globular cluster Terzan 5

Neutron star mass in dark matter clumps

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