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

A fixed shape fit to HD 142990 TESS sector 91 data gives a longer period than the constant spin-up forecast

We test the brightness period of HD 142990 with public TESS sector 91 data from 2025. A four-harmonic model with a fixed shape and a slow baseline gives a period of 0.978920952 day in SPOC SAP flux. This is 12.20 seconds longer than the forecast from the published constant spin-up model. A residual block bootstrap gives a conditional 95 percent period range of -1.29 to +1.31 seconds about the fit. SPOC PDC flux and QLP raw flux give periods within 0.7 second of this fit. The two strongest Fourier harmonics agree within their conditional errors. The weaker third harmonic and half-visit fits show limits of the model. Six K2 reductions from 2014 give periods that span 15.2 seconds. The planned comparison between K2SFF BESTAPER and TESS SAP does not distinguish the historical rate from a constant period. The direct forecast test was added after the first fits. Historical parameter errors have no supplied covariance. We give parameter ranges, without a formal rejection probability. The result is a new local brightness-period measurement under stated assumptions. It does not establish a change in bulk stellar rotation. The package contains five original FITS files, checksums, code, figures, results, and repeat instructions.

HD 142990 · V913 Sco · TIC 77676815 · EPIC 203814494 · TESS · K2 · stellar rotation · magnetic stars · brightness period · Fourier model · public data · reproducible research

Admitted 2 citing publications

References

9
  1. usesdoi:10.1093/mnras/stz1129

    We test a forecast from its variable ephemeris with 2025 data. We do not repeat its full historical analysis.

  2. usesdoi:10.17909/T9BC75

    We use three flux fields from one K2SFF file. The package preserves the source file and its hash.

  3. doi:10.1086/678764

    This paper describes the K2SFF method.

  4. usesdoi:10.17909/T9501J

    We use one EVEREST light curve from this collection.

  5. doi:10.48550/arXiv.1702.05488

    This paper describes the EVEREST method.

  6. usesdoi:10.17909/t9-r086-e880

    We use raw and detrended flux from one QLP file.

  7. HD 60431 period change estimates depend on the light curve feature in 2019–2025 TESS QLP raw flux sci:sha256:28517fdf3d930b9aa09f06c3be63f59bccd65074f6176554ccceb610ffc5dcea

    This related study on HD 60431 tests different Fourier features. It supports the need for feature checks. We use no code or data from it.

  8. doi:10.1093/mnras/stag194

    This survey gives a rounded BRITE period for HD 142990. We do not use that value as a precise timing anchor.

  9. doi:10.48550/arXiv.2507.03882

    This recent radio study uses the historical ephemeris. Its pulse phases are not a new TESS brightness period.

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