Recurrent novae (RNe) play an important role as one of the suspected progenitor systems of Type Ia supernovae (SNe) which are used as primary distance indicators in cosmology. Thus, it is important to investigate the nature of their central binary systems to determine the relation between the parameters of the central system and outburst type, and finally ascertain the population of novae that might be available to give rise to the progenitors of Type Ia SNe. The details of the preliminary investigation looking for characteristics that may distinguish recurrent and classical novae (CNe) systems, the selection of initial targets for detailed study, and preliminary results are presented. We identified 10 suspected RNe among the Galactic CNe for investigation with the Liverpool Telescope population and our initial photometric observations of their quiescent systems suggest 2 may belong to the RS Oph type and 2 to the U Sco type RNe. Spectroscopic follow-up is now underway.
在银河系已知的大约400颗经典新星中，只有10颗，即周期性新星，被发现爆发不止一次。已知至少有八个这样的回归星拥有演化的次级恒星，而不是典型的经典新星中的次级主序星。在本文中，我们提出了一个新的新星分类系统，完全基于二级的演化状态，而不是（像目前的计划）基于爆发的属性。使用档案光学和近红外光度观测的样本38静止的银河新星，我们表明，在一个静止的系统中的次要恒星的演化状态可以预测和几个对象被确定为后续观测; CI Aql，V2487 Oph，DI Lac和欧盟Sct。
The study presents a simplified method to identify potential bright red nova progenitors based on the amplitude of the light curve and infrared (J-H) colour of a contact binary system. We employ published criteria for contact binary orbital instability to show that the amplitude of the light curve for a given contact system with a low mass (< 1.4Msun) primary must be less than a specified value for it to be potentially unstable. Using this we search the photometric data of a large survey to identify about 50 potential bright red nova progenitors. We analyse the survey photometry of each to det…
T Pyx是一颗周期性的新星，几乎每20年就会爆发一次，直到1967年至2011年之间达到长期的平静。我们观察到期待已久的2011年爆炸在光学和近红外与中等光谱分辨率。在本文中，我们报告的光谱类型的新星（在其上升和衰落期间）的变化，以及观测到的膨胀速度的变化。我们还提出了这些变化的解释，并将它们设置在一个新的理解新星分类的一般框架。
ZZ PsA is a neglected bright southern contact binary system with maximum V magnitude of 9.26. We present the first multi-band photometric analysis and find the system to be in deep contact (>95%) with an extremely low mass ratio of 0.078. The primary has a mass of 1.213 M? in keeping with its reported spectral class of F6. In order to determine if ZZ PsA is a merger candidate we outline the current status regarding the instability mass ratio and develop new relationship linking the mass of the primary to the instability mass ratio of the system and the degree of contact. We find that ZZ PsA al…
We present a complete dynamical study of the intermediate polar and dwarf nova cataclysmic variable GK Per (Nova Persei 1901) based on a multi-site optical spectroscopy and $R$-band photometry campaign. The radial velocity curve of the evolved donor star has a semi-amplitude $K_2=126.4 \pm 0.9 \, \mathrm{km}\,\mathrm{s}^{-1}$ and an orbital period $P=1.996872 \pm 0.000009 \, \mathrm{d}$. We refine the projected rotational velocity of the donor star to $v_\mathrm{rot} \sin i = 52 \pm 2 \, \mathrm{km}\,\mathrm{s}^{-1}$ which, together with $K_2$, provides a donor star to white dwarf mass ratio $…
We present photometric analysis of three bright red nova progenitor contact binary systems: ASAS J082151-0612.6, TYC 7281-269-1 and TYC 7275-1968-1. The primary components in all three systems are solar-type low mass stars with radii somewhat larger than their Zero Age Main Sequence counterparts. The secondaries, as in most contact binary systems, have radii and luminosities well above their main sequence counterparts. All three have extreme low mass ratios ranging from 0.075 to 0.097 and two have high degrees of contact, in excess of 75%. All three have mass ratios and separations below the t…
The first hours and days of the 2021 explosion of the recurrent symbiotic nova RS Ophiuchii
Astronomical Institute, Slovak Academy of Sciences（斯洛伐克科学院天文研究所）；Private observatory Liptovská Štiavnica（利普托夫斯卡什佳夫尼察私人天文台）；ARAS Eruptive Stars Group（ARAS爆发恒星小组）；Fujii Kurosaki Observatory（藤井黑崎天文台）；Astronomical Institute, Czech Academy of Sciences（捷克科学院天文研究所）；Astronomical Institute of Charles University（查理大学天文研究所）
A remarkable recurrent nova in M31 - The optical observations
2013年11月下旬，M31经常性新星M31 N 2008- 12 a在五年内第五次爆发。目的：在这封信中，我们解决的光学光变曲线和祖系统的M31 N 2008- 12 a。研究方法：2013年的光学成像数据从利物浦望远镜，拉帕尔马，丹麦1.54米望远镜，拉西拉，和档案哈勃太空望远镜近红外，光学和近紫外数据的爆发进行天体测量和光度分析。结果如下：2013年爆发的光度测量，结合之前的三次爆发，使一个非常快的新星，t2（V）~4天的模板光变曲线的建设成为可能。档案数据允许恢复的祖先系统的光学和近紫外数据，表明一个红巨星二次与明亮的吸积盘，或者是一个系统与亚巨星二次，但占主导地位的磁盘。结论：M31 N 2008- 12 a的爆发和一些历史性的X射线探测表明，这是一个独特的系统，重现时间约为1年。这意味着一个非常高质量的白矮星和高吸积率的存在。我们鼓励更多的观测，特别是在2014年底。
Multiwavelength modelling the SED of supersoft X-ray sources. II. RS Ophiuchi: From the explosion to the SSS phase
RS Oph是一颗周期性的共生新星，在20年的时间尺度上经历了类似新星的爆发。它的最后两次喷发（1985年和2006年）是从X射线到无线电的密集多波长观测活动的主题。这一贡献的目的是确定物理参数和电离结构的新星从爆炸到第一次出现的超软X射线（第26天）通过使用的方法多波长建模的SED。从爆发的一开始，SED模型就揭示了光谱中存在强烈的恒星和星云辐射成分。在最初的4天里，这颗新星显示出一个双锥电离结构。$\sim 8200$ K温暖和160 - 200 R $_{\odot}$扩展的伪光球围绕白矮星（WD）的赤道到纬度$>40^{\circ}$。WD两极周围的剩余空间被电离，通过WD的快风产生了一个发射测量值为$EM \sim 2.3 \times 10^{62}$ cm $^{-3}$的强星云连续体。燃烧WD的光度是高度超爱丁顿的整个调查期间。风的质量损失率为$10^{-4} - 10^{-5}$ M $_{\odot}$ yr $^{-1}$和喷流的存在表明整个盘以高速率吸积，这有助于维持吸积体的超爱丁顿光度很长一段时间。
Luminous Red Novae (LRNe) are astrophysical transients associated with the partial ejection of a binary system's common envelope (CE) shortly before its merger. Here we present the results of our photometric and spectroscopic follow-up campaign of AT2018bwo (DLT18x), a LRN discovered in NGC45, and investigate its progenitor system using binary stellar-evolution models. The transient reached a peak magnitude of $M_r=-10.97\pm0.11$ and maintained this brightness during its optical plateau of $t_p = 41\pm5$days. During this phase, it showed a rather stable photospheric temperature of ~3300K and a…
The explosion outcome and diagnostics of core-collapse supernovae depend sensitively on the nature of the stellar progenitor, but most studies to date have focused exclusively on one-dimensional, spherically-symmetric massive star progenitors. We present some of the first core-collapse supernovae simulations of three-dimensional massive star supernovae progenitors, a 12.5- and a 15-M$_{\odot}$ model, evolved in three-dimensions from collapse to bounce through explosion with the radiation-hydrodynamic code F{\sc{ornax}}. We compare the results using those starting from three-dimensional progeni…
Nicolaus Copernicus Astronomical Center（尼古拉·哥白尼天文学中心）；Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (UB)（巴塞罗那大学宇宙科学研究所）；Departament de Física Quàntica i Astrofísica (FQA), Universitat de Barcelona (UB)（巴塞罗那大学量子物理与天体物理学系）；Institut d’Estudis Espacials de Catalunya (IEEC)（加泰罗尼亚空间研究研究所）
Erratum: Progenitor-explosion connection and remnant birth masses for neutrino-driven supernovae of iron-core progenitors (2012, ApJ, 757, 69)
对流体动力学结果的错误解释导致Ugliano等人（2012）对后备质量的错误确定，这也（在较小的水平上）影响了该论文中提供的中子星质量。Ertl et al.（2015）和Sukhbold et al.（2015）在后续工作中已经解决并纠正了这个问题。因此，建议读者使用后两篇出版物的新数据。在本勘误表的其余部分，我们详细介绍了新旧回退结果的差异，并解释了Ugliano等人（2012）原始分析中错误的起源。
