我们讨论MASTER机器人望远镜网络研究变红巨星的能力。我们报告了三个与长周期变红巨星相关的光学暂现源的发现，并基于MASTER机器人网络全天候巡天观测和存档的MASTER光变曲线，在Lomonosov数据库存储中呈现了这些暂现源的检测帧和光变曲线。我们证明了三个Mira型变量：MASTER OT J083717.54-573411.1、MASTER OT J190436.33+192828.7和MASTER OT J07010810-6818548的暂现检测帧和光变曲线。光谱学验证的碳星MASTER OT J07010810-6818548显示平均亮度增长但恒定脉动周期，这可能表明存在长周期二次星。作为MASTER宽视场图像分析在Lomonosov超级计算机数据存储中的结果，我们为所有三个对象提供了8年历史光变曲线，并为所有三个Mira型变量计算了周期。我们估算了所有三个Mira型变量的基本天体物理参数：光度、半径和零年龄主序（ZAMS）质量。
英文摘要：
We are discussing the capabilities of MASTER network of robotic telescopes to study variable red giant stars. We report the discovery and present archival light curves for three optical transients, connected with long period variable red giants, based on MASTER Robotic Net all-sky survey observations and archival MASTER light curves at Lomonosov database storage. We demonstrate transient detection frames and light curves for three Mira-type variables: MASTER OT $J083717.54-573411.1$, MASTER OT $J190436.33+192828.7$ and MASTER OT $J07010810-6818548$. Spectroscopically validated carbon star MASTER OT $J07010810-6818548$ shows mean magnitude growth but constant pulsation period which may indicate the presence of a long secondary period. As the result of MASTER wide-field images analysis at Lomonosov supercomputer data storage we present the 8-years historical light curves for all three objects with period calculations for all three Mira-type variables. We estimated fundamental astrophysical parameters for all three Mira-type variables: luminosities, radii, and zero age main sequence (ZAMS) masses.
The long secondary period (LSP) phenomenon, which is commonly observed in pulsating red giants, has not been detected in any Mira yet. The goal of this paper is to verify, if there is a physical reason for this or if it is simply an observational bias. The OGLE-III Sample of Long Period Variables in the Large Magellanic Cloud, containing 1663 Miras, is used to perform a search for secondary periodicity in these objects and identify candidates for the long secondary period stars based on the location on the period-luminosity diagram. Out of 1663 Miras, 108 were identified as potential candidate…
Semi-regular variables (SRVs) are similar to Miras in brightness, and they also follow PLRs, though not necessarily the same as Miras. As potential standard candles they are more challenging than Miras due to their smaller variability amplitudes and less regular light curves, but they are substantially more numerous and especially promising to probe old stellar populations. We aim to characterize the variability of SRVs, with focus on their connection with Miras, in order to prepare the ground for investigating their potential as distance indicators. We examine SRVs and Miras in the Magellanic…
We investigate infrared properties of OGLE4 Mira variables in our Galaxy. For each object, we cross-identify the AllWISE, 2MASS, Gaia, and IRAS counterparts. We present various IR two-color diagrams (2CDs) and period-magnitude and period-color relations for the Mira variables. Generally, the Mira variables with longer periods are brighter in the IR fluxes and redder in the IR colors. In this work, we also revise and update the previous catalog of AGB stars in our Galaxy using the new sample of OGLE4 Mira variables. Now, we present a new catalog of 74,093 (64,609 O-rich and 9484 C-rich) AGB sta…
The Mira discovery problem -- Observations by David Fabricius in 1596 and 1609 (and by others before?): Positional accuracy, brightness, color index, and period
本文回顾并分析了 David Fabricius 在 1596 和 1609 年对脉动变星 Mira 的历史观测记录，重新测定了其位置精度、亮度和色指数，探讨了观测偏差对发现的影响，并证实 330.2 天的周期在古今数据中保持一致，无长期变化。
The goal of this paper is to characterise the light variation properties of Mira variables in the Small Magellanic Cloud. We have investigated a combined optical and near infrared multi-epoch dataset of Mira variables based on our monitoring data obtained over 15 years. Bolometric correction relations are formulated for various near-infrared colours. We find that the same bolometric correction equation holds for both the bolometricly brightest and faintest pulsation phases. Period-bolometric magnitude relations and period-colour relations were derived using time-averaged values. Phase lags bet…
Hen 3-160 - the first symbiotic binary with Mira variable S star
鸡3-160报道于Belczynski et al.（2000）的星表作为一个与M7巨供体共生的双星系统。利用20多年来收集的$V$和$I$波段测光资料，我们发现这颗巨星是一颗周期为242.5天的Mira变星。周期光度关系将亨3-160定位在距离约9.4千秒差距处，其银河系坐标（$l=267.7^{\circ}$，$b=-7.9^{\circ}$）将其定位在盘上方$\sim$ 1.3千秒差距处。这个位置加上相对较高的自行（pm $_{\rm{RA}}=-1.5$ mas yr $^{-1}$，pm $_{\rm{DEC}}=+2.9$ mas yr $^{-1}$，盖亚DR 2）表明母鸡3-160必须是银河系扩展的厚盘天体。我们的红色光学和红外光谱显示ZrO和YO分子带的存在下，出现相对较强的TiO带相比。在这里，我们建议，在这个系统中的巨人是内在的S星，在AGB阶段，这将使亨3-160的第一个共生系统与米拉变量S星在其内部发生的慢中子捕获过程中的产品丰富。
Zwicky Transient Facility and Globular Clusters: the gr-Band Period-Luminosity Relations for Mira Variables at Maximum Light and Their Applications to Local Galaxies
The symbiotic X-ray binary Sct X-1 was suggested as the first known neutron star accreting from a red supergiant companion. Although known for nearly 50 years, detailed characterization of the donor remains lacking, particularly due to the extremely high reddening towards the source ($A_V\gtrsim25$ mag). Here, we present i) improved localization of the counterpart using Gaia and Chandra observations, ii) the first broadband infrared spectrum ($\approx1-5\,μ$m; $R\approx 2000$) obtained with SpeX on the NASA Infrared Telescope Facility and iii) $J$-band light curve from the Palomar Gattini-IR s…
The Period--Luminosity relation (PLR) of Mira variable stars is an important tool to determine astronomical distances. The common approach of estimating the PLR is a two-step procedure that first estimates the Mira periods and then runs a linear regression of magnitude on log period. When the light curves are sparse and noisy, the accuracy of period estimation decreases and can suffer from aliasing effects. Some methods improve accuracy by incorporating complex model structures at the expense of significant computational costs. Another drawback of existing methods is that they only provide poi…
Mass loss by red giants is an important process to understand the final stages of stellar evolution and the chemical enrichment of the interstellar medium. Mass-loss rates are thought to be controlled by pulsation-enhanced dust-driven outflows. Here we investigate the relationships between mass loss, pulsations, and radiation, using 3213 luminous Kepler red giants and 135000 ASAS-SN semiregulars and Miras. Mass-loss rates are traced by infrared colours using 2MASS and WISE and by observed-to-model WISE fluxes, and are also estimated using dust mass-loss rates from literature assuming a typical…
