Fits in the known pulse band give a higher recorded J1912−4410 beat-to-pulse ratio in TESS data from 2025 than 2023
Two TESS visits with 200-second sampling give different recorded pulse mixtures for J1912−4410. Joint Fourier fits in the known pulse band give beat-to-pulse amplitude ratios of 0.277 in July 2023 and 1.186 in June and July 2025. Their conditional 95% one-day block intervals are 0.141 to 0.413 and 1.062 to 1.311. The beat is the line at the pulse frequency minus the orbital frequency. The ratio difference remains with the tested apertures, trends, weights, and pulse families. A 120-second visit in 2026 gives 0.358, close to an earlier SCI result. We also supply independent local frequencies for all three visits. The lower clock and the 2026 beat were already known; the older-visit comparison is the added result. The older sampling permits a lower-frequency alias, so the line labels depend on the known pulse band. The intervals assume independent residual block scores and an adequate signal model. Crowding, nonlinear frame rejection, and changing pulse shape limit a physical interpretation. The weak 2023 beat map has a diffuse contribution. The data do not establish a unique emission change or a rotation derivative. The package includes public inputs, provenance, code, results, figures, and reproduction instructions.
J1912-4410 · white dwarf pulsar · TESS · beat amplitude · orbital sidebands · time variability · public data · sampling alias
References
11- usesdoi:10.1038/s41550-023-01995-x
We use the target identity and orbital frequency. This paper gives the discovery pulse clock and earlier optical pulse mixture.
- doi:10.1051/0004-6361/202346589
This X-ray study uses a different pulse clock. It limits a unique interpretation of the frequency difference.
- doi:10.1093/mnras/stad3442
This work detected the ultraviolet beat and showed timing effects from wavelength and pulse shape.
- usesdoi:10.22323/1.514.0061
Figure 2 supplies the later radio reference frequency for a fixed-clock control. Its frequency is near the measured TESS pulse band.
- supportsA joint Fourier fit with a linear 120-second response gives a beat-to-spin amplitude ratio of 0.35 for J1912−4410 in TESS Sector 104 sci:sha256:e6d4b5b9b545c71f306f8098b437173f9028c71a7709fc5b4ea84803f05e046d
Our independent Sector 104 fit gives a recorded ratio close to its earlier result under a different amplitude-response convention. It already reports a local clock check. We add the two older 200-second visits.
- First spin sidebands of J1912−4410 fail a sinusoidal phase constraint in a finite linear model of TESS Sector 104 sci:sha256:4724224b6f6d48c602db74a49d2bf7ad497d07d3954f517e531b6ee9b7d6baba
This later Sector 104 study tests phase constraints and a travel-time bound. Those claims and the 2026 sideband detections are prior results.
- A joint Fourier fit gives a beat amplitude ratio of 0.435 for AR Scorpii in TESS Sector 91 sci:sha256:4805731d5d9730b904119cc7675c19014cbfb8f4612dfa5e0bf0e194f5212d9e
This related AR Scorpii study uses a joint Fourier fit and block errors. No source code was copied.
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We use Sector 67 calibrated full-frame images through an 11 by 11 pixel TESScut extraction.
- usesdoi:10.17909/b9pf-7e83
We use Sector 94 calibrated full-frame images through an 11 by 11 pixel TESScut extraction.
- usesdoi:10.17909/88f8-yy38
We use the Sector 104 TESS light curve for TIC 61510984.
- usesdoi:10.17909/n3ny-gp80
We use the matching Sector 104 target pixels for source maps and aperture closure.
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