Papers › Study Self-lensing/Eclipsing Signals in Edge-on Double White-Dwarf Systems
Study Self-lensing/Eclipsing Signals in Edge-on Double White-Dwarf Systems
Sedighe Sajadian
The archive published only this paper's code-link row. Authors, date and abstract are from arXiv's metadata (CC0), read from the Kaggle arXiv metadata snapshot of 2026-09-12 where its title matched the archive's; the title is the archive's.
Stellar lightcurves from edge-on double white dwarf systems(DWDs) have periodic lensing/eclipsing signals at times of alignment between two components as seen by the observer. Here, we study the characterization and detection of these signals. In common DWDs, the Einstein radii have similar orders of magnitude with WDs' radii, and the projected source and lens radii normalized to the Einstein radius (ρ_⋆, and ρₗ) are ∼1. Both of them are reduced with the orbital period and the lens mass. If ρₗ≃1 the lensing-induced minor image is always blocked by the lens which results lower magnification factors. If ρₗ≲1 and in transit events the finite-lens effects decrease the lightcurves' width. When ρₗ≳1 (happens for close DWDs including one low-mass and one massive WD) deep or complete eclipses dominate to lensing effects. The self-lensing signals maximize for massive DWDs in wide orbits. We study the detect-ability of lensing/eclipsing signals in edge-on DWDs in observations by The NASA's Transiting Exoplanet Survey Satellite(TESS), The Vera Rubin Observatory(LSST) and The Nancy Grace Roman Space Telescope. We simulate stellar lightcurves due to edge-on DWDs and generate synthetic data points based on their observing strategies. Detection efficiency maximizes for extremely low-mass WDs in close orbits, and the numbers of DWDs within 100 pc and an observing cone with detectable lensing/eclipsing signals in one $27.4$-day TESS and $62$-day Roman observing window are ∼1 and <1, respectively. Detecting these signals by LSST is barely possible because of its long cadence.
Code
Repository list and official/mentioned flags are the archive's, frozen 2025-07-28. Reachability, where shown, is from one Syntology probe window (2026-09-16 to 2026-09-18); repositories not probed show nothing. GitHub stars are not tracked.
Code Syntology ran Syntology
Not run by Syntology. Nothing on this page verifies that the listed code works.
Results from the paper archive 2025-07-28
No leaderboard rows for this paper in the archive.
Report a problem or propose a change · a person checks every report against the paper or source before anything changes; decisions are listed on /corrections