Detecting double neutron stars with LISA

Lau, Mike Y. M.; Mandel, Ilya; Vigna-Gómez, Alejandro; Neijssel, Coenraad J.; Stevenson, S. P.; Sesana, Alberto

doi:10.1093/mnras/staa002

Cited by 82 publications

(83 citation statements)

References 71 publications

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“…after 10 years observation with MeerKAT, MeerKAT+ and SKA 1-mid, and 0.5% precision after 15 years. Moreover, LISA is expected to find DNS systems with a characteristic orbital period of 20 minutes in the near future (Lau et al 2020). Such discoveries can significantly tighten the constraints for the EOS.…”

Section: Resultsmentioning

confidence: 87%

Constraining the dense matter equation-of-state with radio pulsars

Krämer

Wex

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Radio pulsars provide some of the most important constraints for our understanding of matter at supranuclear densities. So far, these constraints are mostly given by precision mass measurements of neutron stars (NS). By combining single measurements of the two most massive pulsars, J0348+0432 and J0740+6620, the resulting lower limit of 1.98 M⊙ (99% confidence) of the maximum NS mass, excludes a large number of equations of state (EOSs). Further EOS constraints, complementary to other methods, are likely to come from the measurement of the moment of inertia (MOI) of binary pulsars in relativistic orbits. The Double Pulsar, PSR J0737−3039A/B, is the most promising system for the first measurement of the MOI via pulsar timing. Reviewing this method, based in particular on the first MeerKAT observations of the Double Pulsar, we provide well-founded projections into the future by simulating timing observations with MeerKAT and the SKA. For the first time, we account for the spin-down mass loss in the analysis. Our results suggest that an MOI measurement with 11% accuracy (68% confidence) is possible by 2030. If by 2030 the EOS is sufficiently well known, however, we find that the Double Pulsar will allow for a 7% test of Lense-Thirring precession, or alternatively provide a ∼3σ-measurement of the next-to-leading order gravitational wave damping in GR. Finally, we demonstrate that potential new discoveries of double NS systems with orbital periods shorter than that of the Double Pulsar promise significant improvements in these measurements and the constraints on NS matter.

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Section: Resultsmentioning

confidence: 87%

Constraining the dense matter equation-of-state with radio pulsars

Krämer

Wex

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…Lau et al (2020) use a synthesised DNS population to predict that a 4-yr Laser Interferometer Space Antenna (LISA) mission (Amaro-Seoane et al 2017; Baker et al 2019) will detect 35 Galactic DNSs. Andrews et al (2020) predict between 46 and 240 Galactic DNSs for the same mission, depending on the assumed physical assumptions.…”

Section: Discussionmentioning

confidence: 99%

“…However, this extrapolation does not account for differences between the Galaxy and other environments (Abadie et al 2010), and all rate intervals are broad. Lau et al (2020) use a synthesised DNS population to predict that a 4-yr Laser Interferometer Space Antenna (LISA) mission (Amaro-Seoane et al 2017;Baker et al 2019) will detect 35 Galactic DNSs. Andrews et al (2020) predict between 46 and 240 Galactic DNSs for the same mission, depending on the assumed physical assumptions.…”

Section: Dns Merger Ratesmentioning

confidence: 99%

Common envelope episodes that lead to double neutron star formation

Vigna-Gómez

MacLeod

Neijssel

et al. 2020

Publ. Astron. Soc. Aust.

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Close double neutron stars (DNSs) have been observed as Galactic radio pulsars, while their mergers have been detected as gamma-ray bursts and gravitational wave sources. They are believed to have experienced at least one common envelope episode (CEE) during their evolution prior to DNS formation. In the last decades, there have been numerous efforts to understand the details of the common envelope (CE) phase, but its computational modelling remains challenging. We present and discuss the properties of the donor and the binary at the onset of the Roche lobe overflow (RLOF) leading to these CEEs as predicted by rapid binary population synthesis models. These properties can be used as initial conditions for detailed simulations of the CE phase. There are three distinctive populations, classified by the evolutionary stage of the donor at the moment of the onset of the RLOF: giant donors with fully convective envelopes, cool donors with partially convective envelopes, and hot donors with radiative envelopes. We also estimate that, for standard assumptions, tides would not circularise a large fraction of these systems by the onset of RLOF. This makes the study and understanding of eccentric mass-transferring systems relevant for DNS populations.

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“…As a result, these systems are closer to merger and spend a relatively short amount of time in this subclass of DNS systems compared to the larger orbital period merging DNS systems from Pol et al (2019), which results in an overall smaller population size of ultra-compact DNS systems. The upper limit on the number of ultra-compact DNS systems is also consistent with recent estimates of the size of this population made by Lau et al (2020) and Andrews et al (2020).…”

Section: Size Of Populationsupporting

confidence: 88%

“…These UCB systems can consist of any combination of white dwarf, neutron star or black holes, with the most common source (∼ 10 7 in the Galaxy) being double white dwarf (DWD) binaries (Nelemans et al, 2001a,b). However, population synthesis simulations have shown that LISA should also detect a few tens of ultra-compact double neutron star (DNS) and neutron star-white dwarf (NS-WD) systems (Andrews et al, 2020;Lau et al, 2020). UCB systems are "verification binaries" for LISA, i.e.…”

Section: Introductionmentioning

confidence: 99%

Modeling the Galactic Compact Binary Neutron Star Population and Studying the Double Pulsar System

Pol¹

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Modeling the Galactic Compact Binary Neutron Star Population and Studying the Double Pulsar System Nihan Pol Binary neutron star (BNS) systems consisting of at least one neutron star provide an avenue for testing a broad range of physical phenomena ranging from tests of General Relativity to probing magnetospheric physics to understanding the behavior of matter in the densest environments in the Universe. Ultra-compact BNS systems with orbital periods less than few tens of minutes emit gravitational waves with frequencies ∼mHz and are detectable by the planned space-based Laser Interferometer Space Antenna (LISA), while merging BNS systems produce a chirping gravitational wave signal that can be detected by the ground-based Laser Interferometer Gravitational-Wave Observatory (LIGO). Thus, BNS systems are the most promising sources for the burgeoning field of multi-messenger astrophysics. In this thesis, we estimate the population of different classes of BNS systems that are visible to gravitational-wave observatories. Given that no ultracompact BNS systems have been discovered in pulsar radio surveys, we place a 95% confidence upper limit of ∼850 and ∼1100 ultra-compact neutron starwhite dwarf and double neutron star (DNS) systems respectively. We show that among all of the current radio pulsar surveys, the ones at the Arecibo radio telescope have the best chance of detecting an ultra-compact BNS system. We also show that adopting a survey integration time of t int ∼ 1 min will maximize the signal-to-noise ratio, and thus, the probability of detecting an ultra-compact BNS system. Similarly, we use the sample of nine observed DNS systems to derive a Galactic DNS merger rate of R MW = 37 +24 −11 Myr −1 , where the errors represent 90% confidence intervals. Extrapolating this rate to the observable volume for LIGO, we derive a merger detection rate of R = 1.9 +1.2 −0.6 ×(D r /100 Mpc) 3 yr −1 , where D r is the range distance for LIGO. This rate is consistent with that derived using the DNS mergers observed by LIGO. Finally, to illustrate the unique opportunities for science presented by compact DNS systems, we study the J0737-3039 DNS system, also known as the Double Pulsar system. This is the only known DNS system where both of the neutron stars have been observed as pulsars. We measure the sense of rotation of the older millisecond pulsar, pulsar A, in the DNS J0737-3039 system and find that it rotates prograde with respect to its orbit. This is the first direct measurement of the sense of rotation of a pulsar and a direct confirmation of the rotating lighthouse model for pulsars. This result confirms that the spin angular momentum vector is closely aligned with the orbital angular momentum, suggesting that kick of the supernova producing the second born pulsar J0737-3039B was small.

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Detecting double neutron stars with LISA

Cited by 82 publications

References 71 publications

Constraining the dense matter equation-of-state with radio pulsars

Constraining the dense matter equation-of-state with radio pulsars

Common envelope episodes that lead to double neutron star formation

Modeling the Galactic Compact Binary Neutron Star Population and Studying the Double Pulsar System

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