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arXiv 2602.09377astro-ph.SRastro-ph.HE
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复发新星T Pyxidis的轨道周期变化表明M_ejecta远大于11.3倍M_accreted且不是Ia型超新星前身

Orbital Period Changes of Recurrent Nova T Pyxidis Demonstrate that M_ejecta >> 11.3xM_accreted and Is Not a Type Ia Supernova Progenitor

Louisiana State University（路易斯安那州立大学）

Bradley E. Schaefer

备注：
7th in a series of ApJ papers, each proving that popular progenitor candidates cannot become Type Ia supernovae: 1. V445 Pup (arXiv:2412.17286), 2. T CrB (arXiv:2510.01587), 3. U Sco (arXiv:2510.01589), 4. FQ Cir (arXiv:2511.16594), 5. all symbiotic stars (arXiv:2511.19948), 6. V1405 Cas (ApJ submitted), 7. T Pyx (ApJ in press)
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AI总结：

T Pyx的轨道周期变化表明其喷射质量远大于吸积质量，且不可能成为Ia型超新星前身。

摘要：

复发新星T Pyxidis（T Pyx）具有复杂的质量吸积和喷射历史，其经典新星爆发于1866年开启了六次复发新星爆发，从1890年至2011年。T Pyx是Ia型超新星（SNIa）的主要前身候选者。这主要是一个问题：白矮星吸积的质量（M_accreted）是否比新星爆发喷射的质量（M_ejecta）更大或更小。传统方法测量M_ejecta的散射超过130倍，因此只有新的技术才能提供足够准确和可靠的测量。这种新技术是通过从1986年到2025年的轨道周期测量实验，其中周期在2011次爆发时增加了+50.3±7.9个百万分之一。通过简单而确定的物理，一次复发新星事件喷射的质量的最佳估计是>2400×10⁻⁷ M☉，极端不可侵犯的下限为>>354×10⁻⁷ M☉。在一次完整爆发周期内，M_ejecta>17120×10⁻⁷ M☉，不可侵犯的下限为M_ejecta>>2144×10⁻⁷ M☉。在整个爆发周期内，白矮星吸积了220×10⁻⁷ M☉。因此，M_ejecta>>11.3×M_accreted，T Pyx永远不可能成为SNIa。本文是系列论文中的第七篇，证明各种流行的Ia型超新星前身候选者不可能演变成超新星；包括V445 Pup、U Sco、T CrB等所有双星系统，FQ Cir、V1405 Cas和现在T Pyx。

英文摘要：

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.

机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。

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