Abstract—The article presents the results of multicolor photometry, medium and low resolution spectroscopy of the red nova V838 Mon remnant for 16 years after the 2002 outburst. We also used the archival photometry with the photographic plates of the Sonneberg and Moscow collections from 1928 to 1994. Analysis of these observational data confirmed that the progenitor of the V838 Mon explosion was a wide pair of B3V type stars of reduced luminosity. A brighter component exploded; it was 36 per cent brighter than its companion, and located on the zero-age main sequence of the Spectrum–Luminosity Diagram. Immediately after the outburst, in the fall of 2002, the remnant was a brown L-type supergiant (sgL), but in the fall of 2003 its spectrum changed to M type with a blue radiation excess appeared in the spectral energy distribution, which we interpreted as the reflection effect of the B type companion on the dust formed on the M star. In 2008, the companion was engulfed by the expanding explosion remnant, a type M supergiant (sgM). When the companion was immersing in the expanding M-star, a void was discovered under the M-star upper layer, in which the companion moved for about 200 days. Over the past 10 years, the luminosity of the M star has increased in the V filter by a factor of 10, and the spectral type has changed from M7.5 to M5.5. Based on radial velocities in the BaII 6497 Å and CaI 6572 Å lines, a deceleration of the expanding envelope of the M supergiant was detected, and in 2018, the envelope velocity approached to the heliocentric velocity of the star +71 km s⁻¹. Quasi-periodic changes with a period of 320 days appeared then in the light curves, especially clearly expressed in I filter. We assume that the remnant has an elongated structure, and its rotation period is about 640 days. This is probably a gigantic contact system that will become a detached binary system in future development. The observations do not confirm the assumption that the explosion of one of the V838 Mon components was due to the merger of a compact binary system components located in a hierarchical triple one. Two hypotheses were proposed on the nature of the explosion of one of the V838 Mon components, directly based on the early age of this system: (1) the ignition of thermonuclear burning of hydrogen in the core after the gravitational compression of a protostar; (2) the fragmentation of the core inside a rapidly rotating star in the stage of gravitational compression of a protostar, and later, the subsequent defragmentation (merger of the core components) due to the loss of torque.

摘要—本文介绍了2002年爆发后16年内红色新星V838 Mon残留物的多色光度法，中分辨率和低分辨率光谱学的结果。我们还对1928年至1994年Sonneberg和Moscow收集的照相板使用了档案测光法。对这些观测数据的分析证实，V838 Mon爆炸的祖先是一对亮度降低的宽B3V型恒星。较亮的成分爆炸；它比它的同伴要亮36％，位于光谱-光度图的零年龄主序列上。爆发后，在2002年秋天，残余物立即变成了棕色L型超巨星（sgL），但在2003年秋天，其光谱变为M型，光谱能量分布中出现了蓝色辐射过量，我们将其解释为B型伴星对M星上形成的尘埃的反射效应。在2008年，同伴被不断膨胀的M型超级爆炸物（sgM）所吞没。当同伴沉浸在膨胀的M-star中时，在M-star上层下面发现了一个空隙，同伴在其中移动了约200天。在过去的10年中，M星的亮度在将V滤波器滤除10倍，光谱类型从M7.5变为M5.5。根据BaII 6497Å和CaI 6572Å线的径向速度，检测到M超巨星膨胀包膜的减速，并且在2018年，包膜速度接近恒星的日心速+71 km s ^-1。然后在光曲线中出现了周期为320天的准周期变化，尤其是在I过滤。我们假设残余物具有细长的结构，并且其旋转周期约为640天。这可能是一个巨大的联系系统，它将在将来的开发中成为独立的二进制系统。这些观察结果并不能证实这样的假设，即V838 Mon组件之一爆炸是由于合并了位于分层三元组中的紧凑型二进制系统组件。根据该系统的早期状态，提出了两个关于V838 Mon部件之一爆炸性质的假说：（1）在原恒星的重力压缩后，核中氢的热核燃烧着火；（2）在原恒星的重力压缩阶段，快速旋转的恒星内部的核破碎，然后，