A closed-form solution φ(r,θ) for Hill's surfaces in the CR3BP is obtained by solving a cubic equation that reproduces tadpole, horseshoe, Roche lobe, and quasi-spherical shapes.
Physics Of Eclipsing Binaries. II. Towards the Increased Model Fidelity
6 Pith papers cite this work, alongside 320 external citations. Polarity classification is still indexing.
6
Pith papers citing it
320
external citations · Pith
abstract
The precision of photometric and spectroscopic observations has been systematically improved in the last decade, mostly thanks to space-borne photometric missions and ground-based spectrographs dedicated to finding exoplanets. The field of eclipsing binary stars strongly benefited from this development. Eclipsing binaries serve as critical tools for determining fundamental stellar properties (masses, radii, temperatures and luminosities), yet the models are not capable of reproducing observed data well either because of the missing physics or because of insufficient precision. This led to a predicament where radiative and dynamical effects, insofar buried in noise, started showing up routinely in the data, but were not accounted for in the models. PHOEBE (PHysics Of Eclipsing BinariEs; http://phoebe-project.org) is an open source modeling code for computing theoretical light and radial velocity curves that addresses both problems by incorporating missing physics and by increasing the computational fidelity. In particular, we discuss triangulation as a superior surface discretization algorithm, meshing of rotating single stars, light time travel effect, advanced phase computation, volume conservation in eccentric orbits, and improved computation of local intensity across the stellar surfaces that includes photon-weighted mode, enhanced limb darkening treatment, better reflection treatment and Doppler boosting. Here we present the concepts on which PHOEBE is built on and proofs of concept that demonstrate the increased model fidelity.
years
2026 6representative citing papers
Theta Eridani's historical brightness is explained as a millenary common-envelope transient powered by orbital energy extraction in a previously more eccentric binary.
PHOEBE 2.5 incorporates TMAP and Tremblay atmospheres, atmosphere blending, and derived limb-darkening tables to model hot compact stars in eclipsing binaries without blackbody fallback.
TESS and ground-based photometry of two low-mass eclipsing binaries yield improved stellar parameters, evidence for tertiary companions via the light-time effect, and a flare frequency of one per 40 hours for NSVS 01031772.
AstroSkyFlow generates simulated time-series astronomical images with realistic noise and variability, outperforming SkyMaker in noise and PSF reproduction while recovering injected signals such as exoplanet transits and asteroid trails.
Multi-technique observations constrain the configuration of the ξ Tau system, detecting orbital oscillations on multiple timescales and suggesting component C is itself a binary.
citing papers explorer
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Hill's level surfaces in the circular restricted three-body problem solved
A closed-form solution φ(r,θ) for Hill's surfaces in the CR3BP is obtained by solving a cubic equation that reproduces tadpole, horseshoe, Roche lobe, and quasi-spherical shapes.
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The forgotten bright star: Theta Eridani as a millenary stellar transient observed by Hipparchus, Ptolemy and al-Sufi
Theta Eridani's historical brightness is explained as a millenary common-envelope transient powered by orbital energy extraction in a previously more eccentric binary.
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Physics of Eclipsing Binaries. VI. Hot, compact stars
PHOEBE 2.5 incorporates TMAP and Tremblay atmospheres, atmosphere blending, and derived limb-darkening tables to model hot compact stars in eclipsing binaries without blackbody fallback.
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TESS light curves and surface activity in two low-mass eclipsing binaries: NSVS 01031772 and 2MASS J04100497+2931023
TESS and ground-based photometry of two low-mass eclipsing binaries yield improved stellar parameters, evidence for tertiary companions via the light-time effect, and a flare frequency of one per 40 hours for NSVS 01031772.
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AstroSkyFlow: an astronomical sky image flow simulator for time domain survey validation and machine learning
AstroSkyFlow generates simulated time-series astronomical images with realistic noise and variability, outperforming SkyMaker in noise and PSF reproduction while recovering injected signals such as exoplanet transits and asteroid trails.
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Configuration of the $\xi$ Tau system constrained by multi-technique observations
Multi-technique observations constrain the configuration of the ξ Tau system, detecting orbital oscillations on multiple timescales and suggesting component C is itself a binary.