Radio Pulsar Populations

Lorimer, D. R.; Pol, N.; Rajwade, K.; Aggarwal, K.; Agarwal, D.; Strader, J.; Lewandowska, N.; Kaplan, D.; Cohen, T.; Demorest, P.; E., Fonseca,; Chatterjee, S.

doi:10.48550/arxiv.1903.06526

Cited by 3 publications

(3 citation statements)

References 73 publications

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“…The resulting Φ( 𝑓 ) is shown in Figure 1. Even though the number of NSs used to construct Φ( 𝑓 ) is just a tiny fraction of the pulsars within our Galaxy and clusters of galaxies, the frequency distribution is expected to not be significantly biased by selection effects (Lorimer 2008;Lorimer et al 2019) for millisecond pulsars. Moreover, this distribution is consistent with those obtained from population synthesis models (Story et al 2007;Talukder et al 2014).…”

Section: Modelling the Sourcementioning

confidence: 99%

Stochastic gravitational-wave background searches and constraints on neutron-star ellipticity

De Lillo,

Suresh,

Miller

2022

Preprint

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Rotating neutron stars (NSs) are promising sources of gravitational waves (GWs) in the frequency band of ground-based detectors. They are expected to emit quasi-monochromatic, long-duration GW signals, called continuous waves (CWs), due to their deviations from spherical symmetry. The degree of such deformations, and hence the information about the internal structure of a NS, is encoded in a dimensionless parameter 𝜀 called ellipticity. Searches for CW signals from isolated Galactic NSs have shown to be sensitive to ellipticities as low as 𝜀 ∼ O (10 −9 ). These searches are optimal for detecting and characterising GWs from individual NSs, but they are not designed to measure the properties of NSs as population, such as the average ellipticity 𝜀 av . These ensemble properties can be determined by the measurement of the stochastic gravitational-wave background (SGWB) arising from the superposition of GW signals from individually-undetectable NSs. In this work, we perform a cross-correlation search for such a SGWB using the data from the first three observation runs of Advanced LIGO and Virgo. Finding no evidence for a SGWB signal, we set upper limits on the dimensionless energy density parameter Ω gw ( 𝑓 ). Using these results, we also constrain the average ellipticity of Galactic NSs and five NS "hotspots", as a function of the number of NSs emitting GWs within the frequency band of the search 𝑁 band . We find 𝜀 av < ∼ 1.8 × 10 −8 , with 𝑁 band = 1.6 × 10 7 , for Galactic NSs, and 𝜀 av < ∼ [3.5 − 11.8] × 10 −7 , with 𝑁 band = 1.6 × 10 10 , for NS hotspots.

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Section: Modelling the Sourcementioning

confidence: 99%

Stochastic gravitational-wave background searches and constraints on neutron-star ellipticity

De Lillo,

Suresh,

Miller

2022

Preprint

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“…In the computation The GW sensitivity curves for LIGO, LISA and PTA are borrowed from [23]. The minimal radio flux density for Arecibo, MeerKAT and FAST are taken to be 0.2, 0.017 and 0.0038 [19,21,24,25]. Other parameters are chosen as MB = 1.4M , q = 1 and an average pulsar pseudoluminosity at 1.4 GHz, L1400 = 1 mJy kpc 2 .…”

Section: B Timing Accuracymentioning

confidence: 99%

Gravitational Collider Physics via Pulsar-Black Hole Binaries

Ding,

Tong,

Wang

2020

Preprint

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We propose to use pulsar-black hole binaries as a probe of gravitational collider physics. Induced by the gravitation of the pulsar, the atomic transitions of the boson cloud around the black hole backreact on the orbital motion. This leads to the deviation of binary period decrease from that predicted by general relativity, which can be directly probed by the Rømer delay of pulsar time-of-arrivals. The sensitivity and accuracy of this approach is estimated for two typical atomic transitions. It is shown that once the transitions happen within the observable window, the pulsar-timing accuracy is almost always sufficient to capture the resonance phenomenon.

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“…INTRODUCTION Since the discovery of the first pulsar (Hewish et al 1968), the number of known neutron stars has grown to more than three thousands, including a rich ensemble of binary and millisecond pulsars (Manchester et al 2005) 1 . The study of pulsars combines a wide range of physical processes, which shed light on the fundamental laws of nature and the structure of our Galaxy (e.g., Lorimer & Kramer 2004;Lorimer et al 2019). Timing of pulsars in binary systems has not only allowed exquisite tests of strong gravity, but has also given insights into the equation of state that describes them and the nature of the binary systems they inhabit (e.g., Hulse…”

mentioning

confidence: 99%

Impact of Natal Kicks on Merger Rates and Spin–Orbit Misalignments of Black Hole–Neutron Star Mergers

Fragione

Loeb

Rasio

2021

ApJL

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Neutron stars are born out of core-collapse supernovae, and they are imparted natal kicks at birth as a consequence of asymmetric ejection of matter and possibly neutrinos. Unless the force resulting from the kicks is exerted exactly at their center, it will also cause the neutron star to rotate. In this paper, we discuss the possibility that neutron stars may receive off-center natal kicks at birth, which imprint a natal rotation. In this scenario, the observed pulsar spin and transverse velocity in the Galaxy are expected to correlate. We develop a model of the natal rotation imparted to neutron stars and constrain it by the observed population of pulsars in our Galaxy. At 90% confidence, we find that the location of the off-center kick is R kick = 1.12 +4.79 −0.97 km. Our result is robust when considering pulsars with different observed periods, transverse velocities, and ages. Our constraint can be used as a guide for core-collapse simulations of massive stars.1. INTRODUCTION Since the discovery of the first pulsar (Hewish et al. 1968), the number of known neutron stars has grown to more than three thousands, including a rich ensemble of binary and millisecond pulsars (Manchester et al. 2005) 1 . The study of pulsars combines a wide range of physical processes, which shed light on the fundamental laws of nature and the structure of our Galaxy (e.g., Lorimer & Kramer 2004;Lorimer et al. 2019). Timing of pulsars in binary systems has not only allowed exquisite tests of strong gravity, but has also given insights into the equation of state that describes them and the nature of the binary systems they inhabit (e.g., Hulse

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Radio Pulsar Populations

Cited by 3 publications

References 73 publications

Stochastic gravitational-wave background searches and constraints on neutron-star ellipticity

Stochastic gravitational-wave background searches and constraints on neutron-star ellipticity

Gravitational Collider Physics via Pulsar-Black Hole Binaries

Impact of Natal Kicks on Merger Rates and Spin–Orbit Misalignments of Black Hole–Neutron Star Mergers

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