A hierarchical pruning framework reduces the computational cost of fully coherent circular-orbit binary pulsar searches by up to 10 orders of magnitude, enabling sensitivity 3-5x better than acceleration searches.
Physics of Binary Star Evolution -- from Stars to X-ray Binaries and Gravitational Wave Sources
12 Pith papers cite this work, alongside 47 external citations. Polarity classification is still indexing.
12
Pith papers citing it
47
external citations · Pith
abstract
The majority of all stars are members of a binary system. The evolution of such binary stars and their subsequent production of pairs of compact objects in tight orbits, such as double neutron stars and double black holes, play a central role in modern astrophysics, Binary evolution leads to the formation of different types of violent cosmic events such as novae, supernova explosions, gamma-ray bursts, mass transfer and accretion processes in X-ray binaries, and the formation of exotic radio millisecond pulsars. In some cases, the binary systems terminate as spectacular collisions between neutron stars and/or black holes. These collisions lead to powerful emission of gravitational waves, as detected by LIGO since 2015. The coming decade is expected to reveal a large number of discoveries of binary compact systems, as well as their progenitors and merger remnants, from major instruments such as the radio Square-Kilometre Array; the gravitational wave observatories LIGO-Virgo-KAGRA-IndIGO and LISA; the astrometric space observatory Gaia; the James Webb Space Telescope; and the X-ray space observatories eXTP, STROBE-X, and Athena. In this light, it is important to have a modern textbook on the physics of binary stars evolution, from ordinary stars to X-ray binaries and gravitational wave sources. The scope of this book is that the reader (student or educated expert) will learn the physics of binary interactions, from stellar birth to compact objects, and relate this knowledge to the latest observations. The reader will learn about stellar structure and evolution, and detailed binary interactions covering a broad range of phenomena, including mass transfer and orbital evolution, formation and accretion onto compact objects (white dwarfs, neutron stars and black holes), and their observational properties. Exercises are provided throughout the book.
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citation-polarity summary
years
2026 12roles
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background 1representative citing papers
Discovery of PSR J0125-5854, a 24 ms pulsar in a binary with orbital period ~834 days, low eccentricity, and likely helium white dwarf companion.
First detection of relativistic angular deformation δ_θ in PSR J1757−1854 via MeerKAT-enhanced timing, ruling out two of four prior geometric solutions while confirming GR consistency for orbital decay.
Deep NIR adaptive-optics imaging rules out a helium-star companion to the eclipsing millisecond pulsar PSR J1928+1815, favoring a massive white dwarf.
Enhanced angular-momentum loss via outer-Lagrangian mass ejection shifts the ELM white-dwarf mass–period relation downward and reproduces most observed short-period systems.
Adiabatic mass-loss models for massive helium stars give critical mass ratios 0.7-3.0 on the main sequence and 1.5-27 on the Hertzsprung gap, lowered by winds and adjusted by isotropic re-emission.
Reconstruction of GRO J1655-40, SAX J1819.3-2525 and 4U 1543-47 requires CE efficiencies α_0.5U ≳6.7, α_U ≳4.2, α_H ≳1.7 with no solutions below unity, implying need for additional energy or formalism changes plus natal kicks ≳50 km/s for 4U 1543-47.
Population synthesis of pulsar-massive star binaries yields an estimate for the number of observable VHE gamma-ray sources in the Galaxy, incorporating anisotropic wind-interaction zones.
SKA-MID and SKA-LOW are predicted to discover 150–1700 new pulsars in Galactic globular clusters, more than doubling the current population of 345.
Review of high-precision astrometry applications to compact object astrophysics, emphasizing Gaia DR3 evidence for mass-dependent peculiar velocities and NS-BH similarities.
Follow-up observations of PSR J2338+4818 detect 27,228 single pulses with no nulling and measure scintillation timescales of 2.93-25.26 min and bandwidths of 1.68-27.41 MHz.
citing papers explorer
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Coherent Signal Detection with Pruning -- I. Finding Short-Period Binary Pulsars in Circular Orbits
A hierarchical pruning framework reduces the computational cost of fully coherent circular-orbit binary pulsar searches by up to 10 orders of magnitude, enabling sensitivity 3-5x better than acceleration searches.
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Discovery of a 24-millisecond pulsar in a very long orbit with the Murchison Widefield Array
Discovery of PSR J0125-5854, a 24 ms pulsar in a binary with orbital period ~834 days, low eccentricity, and likely helium white dwarf companion.
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Detection of relativistic orbital deformation from improved timing of PSR J1757$-$1854
First detection of relativistic angular deformation δ_θ in PSR J1757−1854 via MeerKAT-enhanced timing, ruling out two of four prior geometric solutions while confirming GR consistency for orbital decay.
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Deep Adaptive Optics Imaging Rules Out a Helium Star Companion to PSR J1928+1815
Deep NIR adaptive-optics imaging rules out a helium-star companion to the eclipsing millisecond pulsar PSR J1928+1815, favoring a massive white dwarf.
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Formation of Extremely Low-mass White Dwarf Binaries Undergoing Enhanced Angular Momentum Loss
Enhanced angular-momentum loss via outer-Lagrangian mass ejection shifts the ELM white-dwarf mass–period relation downward and reproduces most observed short-period systems.
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Adiabatic Mass Loss In Binary Stars. VI. Massive Helium Binary Stars
Adiabatic mass-loss models for massive helium stars give critical mass ratios 0.7-3.0 on the main sequence and 1.5-27 on the Hertzsprung gap, lowered by winds and adjusted by isotropic re-emission.
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A Path to Constraints on Common Envelope Ejection in Massive Binaries: Full Evolutionary Reconstruction of Three Black Hole X-ray Binaries
Reconstruction of GRO J1655-40, SAX J1819.3-2525 and 4U 1543-47 requires CE efficiencies α_0.5U ≳6.7, α_U ≳4.2, α_H ≳1.7 with no solutions below unity, implying need for additional energy or formalism changes plus natal kicks ≳50 km/s for 4U 1543-47.
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How many VHE gamma-ray binaries with young pulsars can be observed?
Population synthesis of pulsar-massive star binaries yields an estimate for the number of observable VHE gamma-ray sources in the Galaxy, incorporating anisotropic wind-interaction zones.
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Pulsars in Globular Clusters With the SKAO
SKA-MID and SKA-LOW are predicted to discover 150–1700 new pulsars in Galactic globular clusters, more than doubling the current population of 345.
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Compact Object Astrophysics with Frontline Astrometry
Review of high-precision astrometry applications to compact object astrophysics, emphasizing Gaia DR3 evidence for mass-dependent peculiar velocities and NS-BH similarities.
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A Pilot Study of Mildly Recycled Pulsars: A Case Study of PSR J2338+4818
Follow-up observations of PSR J2338+4818 detect 27,228 single pulses with no nulling and measure scintillation timescales of 2.93-25.26 min and bandwidths of 1.68-27.41 MHz.
- The GMRT High-Resolution Southern Sky Survey for pulsars and transients -- VIII: Orbital Variability and the Evolution of a 1-Day He-WD Millisecond Pulsar J2101-4208