Orbital Period Changes of Recurrent Nova T Pyxidis Demonstrate that M_ejecta >> 11.3xM_accreted and Is Not a Type Ia Supernova Progenitor
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| Format: | Preprint |
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2026
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| _version_ | 1866914318524612608 |
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| author | Schaefer, Bradley E. |
| author_facet | Schaefer, Bradley E. |
| contents | Recurrent nova (RN) T Pyxidis (T Pyx) has a complex history of mass accreting-onto and ejection-from the white dwarf, with a classical nova eruption around 1866 kick-starting a RN-phase with six RN eruptions from 1890--2011. T Pyx is a primary progenitor candidate for Type Ia supernovae (SNIa). This is chiefly a question of whether the mass accreted by the white dwarf ($M_{\rm accreted}$) is more-or-less than the mass ejected by the nova eruptions ($M_{\rm ejecta}$) over the entire eruption cycle. Prior attempts to measure $M_{\rm ejecta}$ from the traditional methods have a scatter of $>$130$\times$, so only a new technique can provide a measure of adequate accuracy and reliability. This new technique is the timing experiment of measuring the orbital period from 1986 to 2025, where the period increased by $+$50.3$\pm$7.9 parts-per-million across the 2011 eruption. With simple and sure physics, the best estimate for the mass ejected by one RN event is $>$2400$\times$10$^{-7}$ M$_{\odot}$, with an extreme inviolate limit of $\gg$354$\times$10$^{-7}$ M$_{\odot}$. Over all eruptions in a cycle, $M_{ejecta}$$>$17120$\times$10$^{-7}$ M$_{\odot}$, with an inviolate limit of $M_{ejecta}$$\gg$2144$\times$10$^{-7}$ M$_{\odot}$. Over the full eruption cycle, the white dwarf accreted 220$\times$10$^{-7}$ M$_{\odot}$. So M$_{\rm ejecta}$$\gg$11.3$\times$M$_{\rm accreted}$, and T Pyx can never become a SNIa. This paper is the seventh in a series proving that each of various popular candidate SNIa progenitors cannot possibly evolve to a supernova; including V445 Pup, U Sco, T CrB, all symbiotic stars, FQ Cir, V1405 Cas, and now T Pyx. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2602_09377 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | Orbital Period Changes of Recurrent Nova T Pyxidis Demonstrate that M_ejecta >> 11.3xM_accreted and Is Not a Type Ia Supernova Progenitor Schaefer, Bradley E. Solar and Stellar Astrophysics High Energy Astrophysical Phenomena Recurrent nova (RN) T Pyxidis (T Pyx) has a complex history of mass accreting-onto and ejection-from the white dwarf, with a classical nova eruption around 1866 kick-starting a RN-phase with six RN eruptions from 1890--2011. T Pyx is a primary progenitor candidate for Type Ia supernovae (SNIa). This is chiefly a question of whether the mass accreted by the white dwarf ($M_{\rm accreted}$) is more-or-less than the mass ejected by the nova eruptions ($M_{\rm ejecta}$) over the entire eruption cycle. Prior attempts to measure $M_{\rm ejecta}$ from the traditional methods have a scatter of $>$130$\times$, so only a new technique can provide a measure of adequate accuracy and reliability. This new technique is the timing experiment of measuring the orbital period from 1986 to 2025, where the period increased by $+$50.3$\pm$7.9 parts-per-million across the 2011 eruption. With simple and sure physics, the best estimate for the mass ejected by one RN event is $>$2400$\times$10$^{-7}$ M$_{\odot}$, with an extreme inviolate limit of $\gg$354$\times$10$^{-7}$ M$_{\odot}$. Over all eruptions in a cycle, $M_{ejecta}$$>$17120$\times$10$^{-7}$ M$_{\odot}$, with an inviolate limit of $M_{ejecta}$$\gg$2144$\times$10$^{-7}$ M$_{\odot}$. Over the full eruption cycle, the white dwarf accreted 220$\times$10$^{-7}$ M$_{\odot}$. So M$_{\rm ejecta}$$\gg$11.3$\times$M$_{\rm accreted}$, and T Pyx can never become a SNIa. This paper is the seventh in a series proving that each of various popular candidate SNIa progenitors cannot possibly evolve to a supernova; including V445 Pup, U Sco, T CrB, all symbiotic stars, FQ Cir, V1405 Cas, and now T Pyx. |
| title | Orbital Period Changes of Recurrent Nova T Pyxidis Demonstrate that M_ejecta >> 11.3xM_accreted and Is Not a Type Ia Supernova Progenitor |
| topic | Solar and Stellar Astrophysics High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2602.09377 |