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Long secondary periods of 2,877 LMC red giants lose phase between OGLE 1997-2009 and Gaia DR3 2014-2017, while short-period ellipsoidal binaries keep phase

Question: does the long secondary period (LSP) of LMC red giants keep a constant phase over two decades, as a light change locked to a binary orbit must do? Approach: for 2,877 OGLE-III LSP stars we fitted the OGLE-II/III I-band light curves (1997-2009), predicted the LSP phase at the middle of the Gaia DR3 epoch photometry (2014-2017), and measured the Gaia G phase at the same period. For each star we injected a strictly periodic signal into the same data to get the measurement noise. Red-giant ellipsoidal binaries from the same catalogue and the pulsation periods of the LSP stars are controls. Results: the median absolute LSP phase offset is 0.121 cycles against a median null SD of 0.053 cycles; 52% of the stars exceed the strictly periodic null at p <= 0.05. A random-walk phase model gives an effective diffusion D = 0.0045 cycles^2 per cycle (95% CI 0.0043-0.0048), which light-curve injections convert to an intrinsic D of about 0.003. Ellipsoidal binaries with periods below 200 d keep phase over a median of 19 cycles (D = 3e-5, upper limit 7e-5), and all ellipsoidal stars at Gaia S/N >= 10 give D <= 1e-4. A same-band test inside the OGLE data gives LSP D = 0.0043 for 4,953 stars and D = 0 for 444 ellipsoidal stars. The early and later drifts are not correlated, so the data agree with a stochastic phase wander, not a constant period change. Pulsation periods keep no phase memory. Conclusion: in this scope the photometric LSP is not a strict clock; a binary model needs obscuring material that moves in orbital longitude. Limitations: different bands (I against G), sparse Gaia sampling (median 36 epochs), a null that is somewhat optimistic for faint signals, LMC only, and no radial-velocity test.

long secondary period · red giants · Large Magellanic Cloud · OGLE · Gaia DR3 · phase coherence · binary hypothesis · ellipsoidal variables · period stability · variable stars

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References

10
  1. useshttps://arxiv.org/abs/0910.1354

    OGLE-III LMC long-period variable catalogue and photometry (Soszynski et al. 2009, Acta Astron. 59, 239).

  2. challengesdoi:10.3847/2041-8213/abf3c9

    Binary/dusty-cloud explanation of LSPs; a strictly orbital clock is not consistent with the measured phase wander unless the cloud moves in longitude.

  3. supportsdoi:10.48550/arXiv.2604.09767

    Gaia astrometry disfavors a binary origin of LSPs; our photometric phase test points the same way with different data.

  4. https://arxiv.org/abs/astro-ph/0701463

    Soszynski 2007, LSPs and binarity in red giants (ellipsoidal-like LSP light curves).

  5. doi:10.1086/382123

    Wood, Olivier and Kawaler 2004, origin of LSPs.

  6. doi:10.48550/arXiv.2311.04314

    Pawlak et al. 2024, LSPs in ASAS-SN and Gaia.

  7. usesdoi:10.1051/0004-6361/202243940

    Gaia DR3 summary paper; gaia_source and epoch photometry used.

  8. usesdoi:10.17876/gaia/dr.3/55

    Gaia DR3 epoch photometry at the AIP mirror.

  9. usesGaia DR3 and ZTF timing of 11,668 Mira-like stars (2014-2025) shows a weak persistent period-change signal and no confirmed rapid period change; a simple O-C extrapolation test is biased sci:sha256:daf0fd31dd887ab0209168a4aeffffffbcb57097f0d0cddc560cdff4cbfc0804

    Lesson that phase-persistence tests need light-curve-level nulls; AIP epoch-photometry recipe.

  10. Periods of 727 ASAS-3 Mira variables changed by 1.1 percent rms from 2000-2009 to 2013-2025 as random wander; early trends did not continue, and only NSV 08001 exceeded the wander sci:sha256:ac75c21920efbdcbf9253a485112a856d1469117a43383299ff3cdf30c5d9f92

    Related campaign study of Mira period wander.

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