Soft X-ray emission from the classical nova AT 2018bej

IF 5.4 2区 物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS Astronomy & Astrophysics Pub Date : 2024-09-23 DOI:10.1051/0004-6361/202451195
A. Tavleev, L. Ducci, V. F. Suleimanov, C. Maitra, K. Werner, A. Santangelo, V. Doroshenko
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Abstract

Context. Classical novae are known to demonstrate a supersoft X-ray source (SSS) state following outbursts. This state is associated with residual thermonuclear burning on the white dwarf (WD) surface. During its all-sky survey (eRASS1), the eROSITA telescope on board the Spectrum-Roentgen-Gamma observatory discovered a bright new SSS, whose position is consistent with the known classical nova AT 2018bej in the Large Magellanic Cloud. There were two eROSITA spectra obtained during the eRASS1 and eRASS2 monitoring epochs and one XMM-Newton grating spectrum close to the eRASS1 epoch.Aims. We aim to describe the eROSITA and follow-up XMM-Newton spectra of AT 2018bej with our local thermodynamic equilibrium (LTE) atmosphere models. We focussed on the evolution of the hot WD properties between the eRASS1 and eRASS2 epochs, especially with respect to the change in carbon abundance.Methods. A grid of LTE model atmosphere spectra was calculated for different values of the effective temperature (from Teff = 525 to 700 kK in steps of 25 kK), surface gravity (six values), and chemical composition, assuming approximately equal hydrogen and helium number fractions, and five different values of carbon and nitrogen abundances.Results. Both eRASS1 and XMM 0.3–0.6 keV spectral analyses yield a temperature of the WD of Teff~ 600 kK and a WD radius of 8000–8700 km. A simultaneous fitting of the eROSITA spectra for two epochs (eRASS1 and eRASS2) with a common WD mass parameter demonstrates a decrease in Teff, accompanied by an increase in the WD radius and a decrease in the carbon abundance. However, these changes are marginal and remain within the errors. The derived WD mass is estimated to be 1.05–1.15 M.Conclusions. We traced a minor evolution of the source on a half-year timescale accompanied by a decrease in the carbon abundance and concluded that LTE model atmospheres can be used to analyse the available X-ray spectra of classical novae during their SSS state.
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经典新星AT 2018bej的软X射线辐射
背景众所周知,经典新星在爆发后会出现超软 X 射线源(SSS)状态。这种状态与白矮星(WD)表面残余的热核燃烧有关。在全天空巡天(eRASS1)期间,光谱-伦琴-伽马天文台上的eROSITA望远镜发现了一个明亮的新SSS,其位置与大麦哲伦云中已知的经典新星AT 2018bej一致。在 eRASS1 和 eRASS2 监测纪元期间获得了两个 eROSITA 光谱,在 eRASS1 纪元附近获得了一个 XMM 牛顿光栅光谱。我们的目的是利用我们的局部热力学平衡(LTE)大气模型来描述 AT 2018bej 的 eROSITA 光谱和后续 XMM-Newton 光谱。我们重点研究了 eRASS1 和 eRASS2 两个纪元之间热 WD 特性的演变,尤其是碳丰度的变化。计算了不同有效温度值(从 Teff = 525 到 700 kK,每步 25 kK)、表面重力(六个值)和化学成分的 LTE 大气模型光谱网格,假设氢和氦的数量分数大致相等,碳和氮的丰度有五个不同值。eRASS1 和 XMM 0.3-0.6 keV 光谱分析得出 WD 的温度为 Teff~ 600 kK,WD 半径为 8000-8700 公里。用一个共同的 WD 质量参数同时拟合了两个纪元(eRASS1 和 eRASS2)的 eROSITA 光谱,结果表明 Teff 下降,同时 WD 半径增大,碳丰度下降。不过,这些变化微不足道,仍在误差范围之内。得出的 WD 质量估计为 1.05-1.15 M⊙。我们追踪了伴随着碳丰度下降的源在半年时间尺度上的微小演变,并得出结论:LTE 大气模型可用于分析经典新星在其 SSS 状态下的现有 X 射线光谱。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
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