arXiv 1601.004742016-01-04astro-ph.SRastro-ph.HE

周期新星LMC 2009 a（LMC 1971 b）的全色观测

Pan-Chromatic observations of the Recurrent Nova LMC 2009a (LMC 1971b)

M. F. Bode, M. J. Darnley, A. P. Beardmore, J. P. Osborne, K. L. Page, F. M. Walter, J. Krautter, A. Melandri, J. -U. Ness, T. J. O'Brien, M. Orio, G. J. Schwar… 展开作者

M. F. Bode, M. J. Darnley, A. P. Beardmore, J. P. Osborne, K. L. Page, F. M. Walter, J. Krautter, A. Melandri, J. -U. Ness, T. J. O'Brien, M. Orio, G. J. Schwarz, M. M. Shara, S. Starrfield

备注：: 20 pages, 23 figures, accepted for publication in the Astrophysical Journal
DOI：: 10.3847/0004-637X/818/2/145

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摘要：

新星LMC 2009a与新星LMC 1971b位置重合，被确认为复发新星（RN）。观测数据集是任何银河系或河外RN最全面的数据集之一：从爆发到超过6年后的光学和近红外测光;前6个月的光谱，以及Swift卫星从爆发后9天到近1年的紫外线和X射线观测。我们发现$M_V = -8.4\pm0.8_{\mathrm{r}}\pm0.7_{\mathrm{s}}$和膨胀速度之间的1000和4000公里秒$^{-1}$。第9天之前的日冕线发射表明喷出物中存在激波。He II $λ$ 4686的强化先于$\sim63-70$天X射线中出现的超软源（SSS），而SSS最初是非常可变的。周期性的调制，$P=1.2$天，最有可能的轨道性质，是明显的紫外线和光学从第43天。随后，SSS示出具有相同周期但具有0.28P延迟的振荡。它的前身系统已经被确认，而第二个则很可能是一个次巨星，它正在吞噬一个发光的吸积盘。SSS的性质推断白矮星（WD）质量为$1.1 \mathrm{M}_\odot \lesssim M_{\rm WD} \lesssim 1.3 \mathrm{M}_\odot$。如果吸积发生在恒定的速度，$\dot{\it{M}}_{\rm acc} \simeq 3.6^{+4.7}_{-2.5} \times 10^{-7} \mathrm{M}_\odot$年$^{-1}$是必要的，符合新星模型的喷发间隔为38年，低爆发幅度，祖先的位置在颜色星等图，并在平静的光谱能量分布。我们注意到LMC 2009a和银河系新星KT Eri之间惊人的相似之处，这表明KT Eri是一个候选RN。

英文摘要：

Nova LMC 2009a is confirmed as a Recurrent Nova (RN) from positional coincidence with nova LMC 1971b. The observational data set is one of the most comprehensive for any Galactic or extragalactic RN: optical and near-IR photometry from outburst until over 6 years later; optical spectra for the first 6 months, and Swift satellite Ultraviolet and X-ray observations from 9 days to almost 1 year post-outburst. We find $M_V = -8.4\pm0.8_{\mathrm{r}}\pm0.7_{\mathrm{s}}$ and expansion velocities between 1000 and 4000 km s$^{-1}$. Coronal line emission before day 9 indicates shocks in the ejecta. Strengthening of He II $λ$4686 preceded the emergence of the Super-Soft Source (SSS) in X-rays at $\sim63-70$ days, which was initially very variable. Periodic modulations, $P=1.2$ days, most probably orbital in nature, were evident in the UV and optical from day 43. Subsequently, the SSS shows an oscillation with the same period but with a delay of 0.28P. The progenitor system has been identified; the secondary is most likely a sub-giant feeding a luminous accretion disk. Properties of the SSS infer a white dwarf (WD) mass $1.1 \mathrm{M}_\odot \lesssim M_{\rm WD} \lesssim 1.3 \mathrm{M}_\odot$. If the accretion occurs at constant rate, $\dot{\it{M}}_{\rm acc} \simeq 3.6^{+4.7}_{-2.5} \times 10^{-7} \mathrm{M}_\odot$ yr$^{-1}$ is needed, consistent with nova models for an inter-eruption interval of 38 years, low outburst amplitude, progenitor position in the color-magnitude diagram, and spectral energy distribution at quiescence. We note striking similarities between LMC 2009a and the Galactic nova KT Eri, suggesting that KT Eri is a candidate RN.

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