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

The measured interval from primary to secondary eclipse in V636 Centauri increased in TESS data from 2019 to 2026

We measure the time from each primary eclipse to its following secondary eclipse in five public two-minute TESS light curves of V636 Centauri. Fourteen pairs pass the main coverage and edge-fit rules. The mean interval at half depth is 3211.155 minutes in sector 11 and 3215.806 minutes in sector 102. This is a change of 4.650 minutes. All 67 usable measurement definitions give a positive change. When 54 definitions use exactly the same 13 pairs, the change ranges from 4.15 to 4.95 minutes. The two 2026 sectors differ by 1.403 minutes over 25.705 days. A point-conjunction model with the published apsidal rate, anchored in 2019, predicts a 4.266-minute endpoint increase and only 0.043 minutes between the 2026 sectors. Tests with fixed synthetic eclipses at the real observing times do not produce the observed multi-minute change. The endpoint sectors have only two main pairs each. Stellar activity and the change of detector can affect the measured times. The data do not identify a new physical cause. We preserve the source files, provenance, code, event and failure tables, method tests, controls, figures, and reproduction instructions.

V636 Centauri · TIC 331183881 · TESS · eclipsing binaries · eclipse timing · apsidal motion · stellar activity · public data

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References

5
  1. usesdoi:10.17909/t9-nmc8-f686

    We use the five recorded standard two-minute SPOC light curves of TIC 331183881 from this TESS data collection.

  2. usesdoi:10.1051/0004-6361:200809670

    We use the published period to locate search windows and the published apsidal rate for a conditional comparison.

  3. usesdoi:10.1051/0004-6361/200912362

    We use the eccentricity, inclination, and relative radii in the orbit and disc tests. The reported activity informs the limits of the timing interpretation.

  4. doi:10.1051/0004-6361/202141484

    This study explains the need for a separate study of V636 Centauri because standard stellar models do not reproduce its physical properties.

  5. usesThe measured secondary eclipse phase of GG Lup increased in four TESS sectors from 2019 to 2026 sci:sha256:0f878a304f9ab68a4649c5060bc92ccc9ce5a176d741c6240fd71870e71cd2f8

    Its use of local eclipse edges, several depths, and explicit method tests informs our design. Our code is a separate implementation for V636 Centauri.

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