PSR J1930–1852: A Pulsar in the Widest Known Orbit Around Another Neutron Star

Swiggum, Joseph K.; Rosen, Rachel A.; McLaughlin, M. A.; Lorimer, D. R.; Heatherly, Sue Ann; Lynch, R.; Scoles, Sarah; Hockett, T.; Filik, E.; Marlowe, J. A.; Barlow, B. N.; Weaver, M.; Hilzendeger, Michael A; Ernst, Sonny; Crowley, R. J.; Stone, E. J.; Miller, Bruce N.; Nuñez, Rafael; Trevino, G.; Doehler, M.; Cramer, A.; Yencsik, D.; Thorley, J.; Andrews, R. G.; Laws, Anna; Wenger, K.; Teter, L.; Snyder, Tomas; Dittmann, Alexander J.; Gray, S. McK.; Carter, M.; McGough, C.; Dydiw, S.; Pruett, Chelsea; Fink, J.; Vanderhout, Amy R.

doi:10.1088/0004-637x/805/2/156

Cited by 70 publications

(44 citation statements)

References 59 publications

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“…We want to highlight that this is (i) a slightly larger mass ratio than the largest predicted by the population synthesis models discussed in Appendix A 1, (ii) the largest mass ratio computed for a realistic (irrotational) binary configuration in quasiequilibrium, 5 and (iii) the largest mass ratio evolved in full general relativity 6 ; see Sec. VA. We employ a grid with n A ¼ n B ¼ 28, n φ ¼ 8, n Cart ¼ 24 and construct a sequence varying the distance parameter b ∈ ½16; 30.…”

Section: Unequal Massesmentioning

confidence: 90%

“…Moreover, of these 12 systems, only seven have well-determined masses, and only six systems (all with well-determined masses) will merge within a Hubble time, and thus contribute directly to merger rate calculations; see, e.g., Table 2 of Ref. [6] and Table 1 in Refs. [1,2].…”

Section: Introductionmentioning

confidence: 99%

“…[21] (see that paper's Table 1), one of us computed corotating binary neutron star initial data with baryonic mass ratios up to 3 for large separations, using a polytropic EOS and small baryonic masses. 6 Up to now the highest mass ratio evolved in full general relativity was q ¼ 1.5 [34,35].…”

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confidence: 98%

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Binary neutron stars with generic spin, eccentricity, mass ratio, and compactness: Quasi-equilibrium sequences and first evolutions

Dietrich¹,

Moldenhauer²,

et al. 2015

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Information about the last stages of a binary neutron star inspiral and the final merger can be extracted from quasiequilibrium configurations and dynamical evolutions. In this article, we construct quasiequilibrium configurations for different spins, eccentricities, mass ratios, compactnesses, and equations of state. For this purpose we employ the SGRID code, which allows us to construct such data in previously inaccessible regions of the parameter space. In particular, we consider spinning neutron stars in isolation and in binary systems; we incorporate new methods to produce highly eccentric and eccentricity-reduced data; we present the possibility of computing data for significantly unequal-mass binaries with mass ratios q ≃ 2; and we create equal-mass binaries with individual compactness up to C ≃ 0.23. As a proof of principle, we explore the dynamical evolution of three new configurations. First, we simulate a q ¼ 2.06 mass ratio which is the highest mass ratio for a binary neutron star evolved in numerical relativity to date. We find that mass transfer from the companion star sets in a few revolutions before merger and a rest mass of ∼10 −2 M ⊙ is transferred between the two stars. This amount of mass accretion corresponds to ∼10 51 ergs of accretion energy. This configuration also ejects a large amount of material during merger (∼7.6 × 10 −2 M ⊙ ), imparting a substantial kick to the remnant neutron star. Second, we simulate the first merger of a precessing binary neutron star. We present the dominant modes of the gravitational waves for the precessing simulation, where a clear imprint of the precession is visible in the (2,1) mode. Finally, we quantify the effect of an eccentricity-reduction procedure on the gravitational waveform. The procedure improves the waveform quality and should be employed in future precision studies. However, one also needs to reduce other errors in the waveforms, notably truncation errors, in order for the improvement due to eccentricity reduction to be effective.

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Section: Unequal Massesmentioning

confidence: 90%

Section: Introductionmentioning

confidence: 99%

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Binary neutron stars with generic spin, eccentricity, mass ratio, and compactness: Quasi-equilibrium sequences and first evolutions

Dietrich¹,

Moldenhauer²,

et al. 2015

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“…Students taking part in the programme have discovered several new pulsars (Rosen et al 2013). This includes PSR J1930-1852, a pulsar in a double neutron star system (Swiggum et al 2015).…”

Section: Summary Interfacesmentioning

confidence: 99%

Fifty years of pulsar candidate selection: from simple filters to a new principled real-time classification approach

Lyon

Stappers

Cooper

et al. 2016

Mon. Not. R. Astron. Soc.

193

174

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Improving survey specifications are causing an exponential rise in pulsar candidate numbers and data volumes. We study the candidate filters used to mitigate these problems during the past fifty years. We find that some existing methods such as applying constraints on the total number of candidates collected per observation, may have detrimental effects on the success of pulsar searches. Those methods immune to such effects are found to be ill-equipped to deal with the problems associated with increasing data volumes and candidate numbers, motivating the development of new approaches. We therefore present a new method designed for on-line operation. It selects promising candidates using a purpose-built tree-based machine learning classifier, the Gaussian Hellinger Very Fast Decision Tree (GH-VFDT), and a new set of features for describing candidates. The features have been chosen so as to i) maximise the separation between candidates arising from noise and those of probable astrophysical origin, and ii) be as survey-independent as possible. Using these features our new approach can process millions of candidates in seconds (∼1 million every 15 seconds), with high levels of pulsar recall (90%+). This technique is therefore applicable to the large volumes of data expected to be produced by the Square Kilometre Array (SKA). Use of this approach has assisted in the discovery of 20 new pulsars in data obtained during the LOFAR Tied-Array All-Sky Survey (LOTAAS).

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“…Observed pulsars in Milky Way DNSs. References: a (Breton et al 2008;Ferdman et al 2013), b (Cameron et al 2018), c (Champion et al 2004), d (Faulkner et al 2004;Ferdman et al 2014), e (Nice et al 1996;Janssen et al 2008), f (Lazarus et al 2016Ferdman 2017), g (Lyne et al 2000;Corongiu et al 2006), h (Martinez et al 2015), i (Martinez et al 2017), j (Stovall et al 2018), k (Swiggum et al 2015), l (Fonseca et al 2014), m (Lynch et al 2018), n (Hulse & Taylor 1975;Weisberg & Huang 2016), o (Keith et al 2009), p (Ng et al 2018a), q (van Leeuwen et al 2015, r (Lynch et al 2012), s (Anderson et al 1990). Systems marked * are in globular clusters, whereas systems marked † may contain a white dwarf companion.…”

Section: Introductionmentioning

confidence: 99%

Modelling double neutron stars: radio and gravitational waves

Chattopadhyay

Stevenson

Hurley

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We have implemented prescriptions for modelling pulsars in the rapid binary population synthesis code COMPAS. We perform a detailed analysis of the double neutron star (DNS) population, accounting for radio survey selection effects. The surface magnetic field decay timescale (≈1000 Myr) and mass scale (≈0.02 M ) are the dominant uncertainties in our model. Mass accretion during common envelope evolution plays a non-trivial role in recycling pulsars. We find a best-fit model that is in broad agreement with the observed Galactic DNS population. Though the pulsar parameters (period and period derivative) are strongly biased by radio selection effects, the observed orbital parameters (orbital period and eccentricity) closely represent the intrinsic distributions. The number of radio observable DNSs in the Milky Way at present is ≈ 2500 in our model, only ≈ 10% of the predicted total number of DNSs in the galaxy. Using our model calibrated to the Galactic DNS population, we make predictions for DNS mergers observed in gravitational waves. The DNS chirp mass distribution varies from ≈1.1M to ≈2.1M and median is obtained to be 1.14 M . The expected effective spin χ eff for isolated DNSs is 0.03 from our model. We predict that ≈34% of the current Galactic isolated DNSs will merge within a Hubble time, and have a median total mass of 2.7 M . Finally, we discuss implications for fast radio bursts and post-merger remnant gravitational-waves.

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PSR J1930–1852: A Pulsar in the Widest Known Orbit Around Another Neutron Star

Cited by 70 publications

References 59 publications

Binary neutron stars with generic spin, eccentricity, mass ratio, and compactness: Quasi-equilibrium sequences and first evolutions

Binary neutron stars with generic spin, eccentricity, mass ratio, and compactness: Quasi-equilibrium sequences and first evolutions

Fifty years of pulsar candidate selection: from simple filters to a new principled real-time classification approach

Modelling double neutron stars: radio and gravitational waves

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