TESS Light Curve of the Interacting Binary W Serpentis
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arXiv
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| Format: | Preprint |
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2025
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| _version_ | 1866916690811420672 |
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| author | Gies, Douglas R. Shepard, Katherine A. Kar, Aman Richardson, Noel D. |
| author_facet | Gies, Douglas R. Shepard, Katherine A. Kar, Aman Richardson, Noel D. |
| contents | The unusual light curve of the massive eclipsing binary W Ser was recently observed with high S/N and fast cadence by the NASA TESS mission. The TESS light curve records two eclipses and relatively fast variations outside of the eclipses. The eclipse timings verify the period increase of the binary, and the period derivative implies a mass transfer rate in excess of 10^{-5} solar masses per year.. The light curve shows a fading trend from just after an eclipse until the start of the next eclipse. The brightest flux source in the system is the accretion torus surrounding the mass gainer star, and we argue that these orbital-phase related fadings are the result of the injection of cooler gas from the mass donor entering the outskirts of the accretion torus. There are cyclic variations in the out-of-eclipse sections of the light curve that vary on a 2.8 day timescale. This equals the orbital period for gas in the outer regions of the accretion torus, so the photometric variations are probably the result of transitory, over-dense regions that form at the rim of the accretion torus. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2504_10608 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | TESS Light Curve of the Interacting Binary W Serpentis Gies, Douglas R. Shepard, Katherine A. Kar, Aman Richardson, Noel D. Solar and Stellar Astrophysics The unusual light curve of the massive eclipsing binary W Ser was recently observed with high S/N and fast cadence by the NASA TESS mission. The TESS light curve records two eclipses and relatively fast variations outside of the eclipses. The eclipse timings verify the period increase of the binary, and the period derivative implies a mass transfer rate in excess of 10^{-5} solar masses per year.. The light curve shows a fading trend from just after an eclipse until the start of the next eclipse. The brightest flux source in the system is the accretion torus surrounding the mass gainer star, and we argue that these orbital-phase related fadings are the result of the injection of cooler gas from the mass donor entering the outskirts of the accretion torus. There are cyclic variations in the out-of-eclipse sections of the light curve that vary on a 2.8 day timescale. This equals the orbital period for gas in the outer regions of the accretion torus, so the photometric variations are probably the result of transitory, over-dense regions that form at the rim of the accretion torus. |
| title | TESS Light Curve of the Interacting Binary W Serpentis |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2504.10608 |