Similarity of PSR J1906+0746 to PSR J0737–3039: a Candidate of a New Double Pulsar System?

Yang, Yi; Zhang, Chengmin; Li, Di; Wang, Dehua; Pan, Y. Y.; Lingfu, Rong-Feng; Zhou, Zhuwen

doi:10.3847/1538-4357/835/2/185

Cited by 13 publications

(7 citation statements)

References 46 publications

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“…Therefore, the companion of PSR J1906+0746 is included in the category of recycled NSs. Although the possibility of a massive white dwarf companion cannot be ruled out from radio observations, we take PSR J1906+0746 to be in a DNS system, as its orbital characteristics and mass estimates are consistent with other Galactic DNSs, especially the double pulsar (Yang et al 2017).…”

Section: Masses Of Galactic Dnsmentioning

confidence: 99%

The Mass Distribution of Galactic Double Neutron Stars

Farrow

Zhu

Thrane

2019

ApJ

181

144

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The conventional wisdom, dating back to 2012, is that the mass distribution of Galactic double neutron stars (DNSs) is well-fit by a Gaussian distribution with a mean of 1.33M and a width of 0.09M . With the recent discovery of new Galactic DNSs and GW170817, the first neutron star merger event to be observed with gravitational waves, it is timely to revisit this model. In order to constrain the mass distribution of DNSs, we perform Bayesian inference using a sample of 17 Galactic DNSs effectively doubling the sample used in previous studies. We expand the space of models so that the recycled neutron star need not be drawn from the same distribution as the nonrecycled companion. Moreover, we consider different functional forms including uniform, single-Gaussian, and two-Gaussian distributions. While there is insufficient data to draw firm conclusions, we find positive support (a Bayes factor (BF) of 9) for the hypothesis that recycled and nonrecycled neutron stars have distinct mass distributions. The most probable model -preferred with a BF of 29 over the conventional model -is one in which the recycled neutron star mass is distributed according to a two-Gaussian distribution, and the nonrecycled neutron star mass is distributed uniformly. We show that precise component mass measurements of ≈ 20 DNSs are required in order to determine with high confidence (a BF of 150) whether recycled and nonrecycled neutron stars come from a common distribution. Approximately 60 DNSs are needed in order to establish the detailed shape of the distributions.

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Section: Masses Of Galactic Dnsmentioning

confidence: 99%

The Mass Distribution of Galactic Double Neutron Stars

Farrow

Zhu

Thrane

2019

ApJ

181

144

View full text Add to dashboard Cite

show abstract

“…In combination with the low mass and higher magnetic field of the secondborn NS, it suggests that PSR J1906+0746 originated from an electron-capture collapse of a degenerate ONeMg core. [3] Its energy released during formation should not be higher than 10 51 erg of the usual SN-type Ic. The discovery of SN 2014ft, a type Ic SN with a fast-evolving light curve, indicates that it has an extremely low ejecta mass (≈ 0.2 M ) and low kinetic energy (2 × 10 50 erg).…”

Section: Introductionmentioning

confidence: 96%

“…[1] It is generally assumed to be a double neutron star (DNS) rather than neutron star-white dwarf system, although an alternative possibility is that the first-formed object could be a white dwarf. [2,3] Furthermore, the possibility that such a pulsar could in fact be strange quark stars also cannot be expelled. [4,5] Several studies have been carried out on this candidate DNS since its discovery.…”

Section: Introductionmentioning

confidence: 99%

“…[4,5] Several studies have been carried out on this candidate DNS since its discovery. [1][2][3] Due to the companion mass, the substantial eccentricity of the binary orbit, the small spin-down age, the significant spin-down energy loss rate, and the relatively higher magnetic field, it is suggested that the pulsar in this DNS system could be a non-recycled and second-born neutron star (NS). [6] The recycled one should be an unusual pulsar or a potential candidate for another new double pulsar system.…”

Section: Introductionmentioning

confidence: 99%

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Constraints on the kinetic energy of type-Ic supernova explosion from young PSR J1906 + 0746 in a double neutron star candidate*

Yi-Yan¹,

Zhang²,

Zhang³

et al. 2021

Chinese Phys. B

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So far among the nineteen pairs of detected double neutron star (DNS) systems, it is a usual fact that the first-born recycled pulsar is detected, however the youngest DNS system PSR J1906+0746, with the characteristic age of 113 kyr, is one of the three detected DNS as a non-recycled and second-born NS, which is believed to be formed by an electron capture or a low energy ultra-stripped iron core-collapse supernova (SN) explosion. The SN remnant around PSR J1906+0746 is too dim to be observed by optical telescopes, then its x-ray flux limit has been given by Chandra. A reference pulsar PSR J1509-5850 with the young characteristic age of 154 kyr was chosen as an object of comparison, which has an SN remnant observed by Chandra and is believed to be formed by iron core SN explosion. We impose a restriction on the maximum kinetic energy of electron-capture (EC) SN explosion that induces the formation of PSR J1906+0746. The estimated result is (4–8)×1050 erg (1 erg = 10−7 J), which is consistent with that of the published simulations of the EC process, i.e., a lower value than that of the conventional iron core SN explosion of (1–2) × 1051 erg. As suggested, EC process for NS formation is pertained to the subluminous type Ic SN by the helium star with ONeMg core, thus for the first time we derived the kinetic energy of EC SN explosion of DNS, which may be reconciled with the recent observation of type Ic SN 2014ft with kinetic energy of 2 × 1050 erg.

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“…PSR J0737-3039A/B is the only known double pulsar binary. There are thirteen pulsar binary systems in which the companion is likely to be a neutron star (Double Neutron Stars or DNS, see the catalogue in Yang et al 2017). These invisible neutron star-companions can be pulsars whose radiating beams miss the line of sight.…”

Section: Introductionmentioning

confidence: 99%

Probing the properties of the pulsar wind via studying the dispersive effects in the pulses from the pulsar companion in a double neutron-star binary system

Cheng

2017

Monthly Notices of the Royal Astronomical Society

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The velocity and density distribution of e ± in the pulsar wind are crucial distinction among magnetosphere models, and contains key parameters determining the high energy emission of pulsar binaries. In this work, a direct method is proposed, which might probe the properties of the wind from one pulsar in a double-pulsar binary. When the radio signals from the first-formed pulsar travel through the relativistic e ± flow in the pulsar wind from the younger companion, the components of different radio frequencies will be dispersed. It will introduce an additional frequency-dependent time-of-arrival delay of pulses, which is function of the orbital phase. In this paper, we formulate the above-mentioned dispersive delay with the properties of the pulsar wind. As examples, we apply the formula to the double pulsar system PSR J0737-3039A/B and the pulsar-neutron star binary PSR B1913+16. For PSR J0737-3039A/B, the time delay in 300 MHz is 10µs near the superior-conjunction, under the optimal pulsar wind parameters, which is ∼ half of the current timing accuracy. For PSR B1913+16, with the assumption that the neutron star companion has a typical spin down luminosity of 10 33 ergs/s, the time delay is as large as 10 ∼ 20µs in 300 MHz. The best timing precision of this pulsar is ∼ 5µs in 1400 MHz. Therefore, it is possible that we can find this signal in archival data. Otherwise, we can set an upper-limit on the spin down luminosity. Similar analysis can be apply to other eleven known pulsar-neutron star binaries.

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Similarity of PSR J1906+0746 to PSR J0737–3039: a Candidate of a New Double Pulsar System?

Cited by 13 publications

References 46 publications

The Mass Distribution of Galactic Double Neutron Stars

The Mass Distribution of Galactic Double Neutron Stars

Constraints on the kinetic energy of type-Ic supernova explosion from young PSR J1906 + 0746 in a double neutron star candidate*

Probing the properties of the pulsar wind via studying the dispersive effects in the pulses from the pulsar companion in a double neutron-star binary system

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