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astro-ph.SR · Solar and Stellar Astrophysicsastro-ph.IM · Instrumentation and Methods for Astrophysicsastro-ph.EP · Earth and Planetary Astrophysics

Selected V471 Tauri eclipse times from 2015, 2021, and 2023 give an 18.7 s contrast against a fixed 2022 clock

We measured 307 white dwarf eclipses in selected public K2 and TESS data for V471 Tauri. We compared times from 2015, 2021, and 2023 with the fixed central clock in Kundra et al. (2022), Table 4. A contrast of three fitted visit offsets removes an added epoch and constant orbital period. The residual contrast is 18.68 s, with a conditional error of 2.19 s from deletion of observing-day groups. Seven-day groups give 2.57 s. We tested baseline functions, corrected flux, separate contact fits, transferred eclipse shapes, and timing weights. These controls give contrasts from 17.98 s to 21.37 s. The paired 20 s and 120 s products show large scatter for some events. The error does not include all shape, processing, or absolute clock errors. Eclipse-time variation in this system is already known. This result checks one central prediction; it does not establish a planet or reject all companion models. The package preserves nine original light curves, 422 timing measurements including cadence controls, source code, provenance, numerical checks, figures, and reproduction instructions.

V471 Tauri · eclipse times · white dwarf · K2 · TESS · light travel time · finite exposure · public astronomical data · reproducible research

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References

10
  1. usesdoi:10.1093/mnras/stac2812

    Table 4 supplies the fixed central clock. Table 3 supplies 32 factual eclipse times for historical context. This paper already reports structured residuals after its companion model.

  2. usesExposure averaging reduces a false timing cycle in a fixed-shape test of RR Cae's 2020 TESS data sci:sha256:51af457250640586b8275fa396f43ee1a0be39615625d53560785e17815c70c0

    We adapt the MIT analytic disk-edge functions and exposure integrals from its verified code. We add event selection, common-shape fits, local clock contrasts, controls, and this data set.

  3. usesdoi:10.17909/T9WS3R

    K2 light-curve collection. The package preserves the exact Campaign 4 short-cadence input, original headers, MAST URI, and SHA-256.

  4. usesdoi:10.17909/t9-st5g-3177

    TESS 20 s light-curve collection. The package preserves the exact Sector 42, 43, and 44 inputs, original headers, MAST URIs, and SHA-256 hashes.

  5. usesdoi:10.17909/t9-nmc8-f686

    TESS 120 s light-curve collection. The package preserves exact inputs from sectors 42, 43, 44, 70, and 71 with their MAST URIs and hashes. The 2021 files serve as cadence controls.

  6. doi:10.1093/mnras/stag358

    This 2026 study includes V471 Tauri in a sample of 43 white dwarf binaries with eclipse-time variation. We read the full text for prior work; its ground-based times are not inputs to our restricted space-data test.

  7. doi:10.3847/2515-5172/ac6df2

    This earlier work gives a corrected mean epoch from 68 K2 eclipses in 2015. Kundra et al. include this literature timing work among their fit inputs. The 2015 visit is therefore not an independent prediction test. We do not add that mean as a separate event.

  8. doi:10.1016/j.newast.2025.102513

    Prior K2 and TESS work on activity and eclipse depths in V471 Tauri. We read the available abstract and preview. We make no claim to first use of these light curves.

  9. doi:10.1111/j.1365-2966.2010.17242.x

    Prior analysis of the effect of finite integration in light-curve models. We use exposure-averaged eclipse profiles.

  10. doi:10.48550/arXiv.2604.27609

    A recent magnetic model of eclipse-time variation that discusses V471 Tauri. Our restricted clock check does not select its physical mechanism or exclude other causes.

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