AX Dra is characterized as a 0.568-day semi-detached eclipsing binary with component masses 1.717 and 0.804 solar masses, radii 1.541 and 1.237 solar radii, and four independent gamma Dor pulsation frequencies in the primary, making it the shortest such system and suggesting the primary is an accret
Formation and Evolution of Compact Stellar X-ray Sources
9 Pith papers cite this work. Polarity classification is still indexing.
9
Pith papers citing it
abstract
In this chapter we review the formation and evolution of compact binaries with neutron star and/or black hole components (i.e. LMXBs, HMXBs, binary pulsars). After an introduction we discuss stellar evolution in binaries and the processes involved in the mass-transfer phases of close binaries (RLO, CE, ang.mom.loss) with radiative/convective hydrogen or helium donor stars. We also describe the effects of accretion, asymmetric SN and systems merging as a result of gravitational wave radiation.
representative citing papers
Mass-ratio reversal in isolated binaries offers a viable formation path for GW241011-like events under specific stellar-evolution and interaction conditions.
Simulations show that intermediate-mass progenitors with non-degenerate cores before helium burning produce a mass-orbital period relation for massive white dwarfs that accounts for long-period systems.
PSR J2101-4802 is a transitional millisecond pulsar with a ~1-day orbit, 0.15 solar mass He-WD companion, and large orbital period derivative that links redback-like systems to detached binaries.
Natal kicks from supernovae are proposed to disrupt Gaia progenitor binaries containing low-mass black holes more frequently than those leading to gravitational-wave mergers, accounting for the observed difference in the 2.5-5 solar mass gap.
Chandra HETGS observations of X1908+075 detect variable Fe Kα fluorescence, model NH orbital changes to derive inclination 46° and wind mass-loss rate 9.1e-7 solar masses per year, confirming a classical wind-fed supergiant X-ray binary.
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.
Binary evolution simulations identify short (20-500 days) and long (2000-4000 days) orbital period ranges where massive star-black hole systems retain enough angular momentum for GRB jet production with negligible mass loss.
citing papers explorer
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The Double-lined Eclipsing $\gamma$ Doradus System AX Draconis in a 0.568-day Orbit
AX Dra is characterized as a 0.568-day semi-detached eclipsing binary with component masses 1.717 and 0.804 solar masses, radii 1.541 and 1.237 solar radii, and four independent gamma Dor pulsation frequencies in the primary, making it the shortest such system and suggesting the primary is an accret
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Mass-Orbital Period Distribution of Massive White Dwarfs Formed Through Stable Mass Transfer
Simulations show that intermediate-mass progenitors with non-degenerate cores before helium burning produce a mass-orbital period relation for massive white dwarfs that accounts for long-period systems.
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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.