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Fundamental Plane of Groups and Clusters of Galaxies: Distances and Pecular Velocities of Superclusters of Galaxies on Small Scales 星系群和星系团的基本平面：小尺度超星系团的距离和奇点速度

IF 1.2 4区物理与天体物理 Q3 Physics and Astronomy

Astrophysical Bulletin

Pub Date : 2024-05-08 DOI: 10.1134/s1990341324600054

F. G. Kopylova, A. I. Kopylov

Abstract

This work is a continuation of the work of Kopylova and Kopylov published in 2016 on constructing the fundamental plane (FP) of groups and clusters of galaxies. In this article, the sample of galaxy systems has been increased from 94 to 172 objects. We have studied the relationships between the main characteristics of groups and clusters of galaxies using archival data from the SDSS, 2MASX, and NED catalogs. The measured parameters ((log L_{K}), (log R_{e}) and (logsigma)) of galaxy clusters define the fundamental plane in the near-infrared region: (L_{K}propto R_{e}^{0.77pm 0.09}sigma^{1.44pm 0.12}). The shape of the FP of groups and clusters is consistent with the FP of early-type galaxies (SDSS, (r)-filter), determined in the same way. Regression against (log R_{e}) in kpc gives the projection of the FP: (log R_{e}=0.98(pm 0.06),logsigma-0.56(pm 0.04)langlelog I_{e}rangle+3.57(pm 0.07)), which can be used to determine the distances of galaxy systems. The (rms) scatter of the zero point is 0.07, which is equivalent to a 16(%) error in determining the distance to a group or cluster of galaxies. For the first time, we have determined the average relative FP distances and peculiar velocities of five large superclusters of galaxies. According to our estimates, the average peculiar velocity of these superclusters relative to the CMB is (+75pm 360) km s({}^{-1}).

摘要这项工作是Kopylova和Kopylov于2016年发表的关于构建星系群和星系团基本面（FP）的工作的延续。在这篇文章中，星系系统的样本从94个增加到了172个。我们利用来自SDSS、2MASX和NED星表的档案数据，研究了星系群和星系团主要特征之间的关系。星系团的测量参数（(log L_{K})，(log R_{e})和(logsigma)）定义了近红外区域的基本面：L_{K}propto R_{e}^{0.77pm 0.09}sigma^{1.44pm 0.12}).星系团和星团的FP形状与早期型星系的FP（SDSS，(r)-filter）是一致的，是用同样的方法确定的。以kpc为单位对(log R_{e})进行回归，就得到了FP的投影：(log R_{e}=0.98(pm 0.06),logsigma-0.56(pm 0.04)langlelog I_{e}rangle+3.57(pm 0.07))，它可以用来确定星系系统的距离。零点的（rms）散度是0.07，这相当于在确定一个星系群或星系团的距离时有16（%）的误差。我们首次测定了五个大型超星系团的平均相对FP距离和奇特速度。根据我们的估计，这些超星系团相对于CMB的平均奇特速度是(+75pm 360) km s({}^{-1}).

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引用次数: 0

Catalog of Variable Stars in the WD 0009 $$boldsymbol{+}$$ 501 and GRW $$boldsymbol{+}$$ 708247 Fields Based on Photometric Survey Data on Transiting Exoplanets 基于凌日系外行星测光巡天数据的 WD 0009 $$boldsymbol{+}$ 501 和 GRW $$boldsymbol{+}$ 708247 场中的变星表

IF 1.2 4区物理与天体物理 Q3 Physics and Astronomy

Astrophysical Bulletin

Pub Date : 2024-05-08 DOI: 10.1134/s1990341323600400

O. Ya. Yakovlev, A. F. Valeev, G. G. Valyavin, V. N. Aitov, G. Sh. Mitiani, T. A. Fathullin, G. M. Beskin, A. V. Tavrov, O. I. Korablev, G. A. Galazutdinov, V. V. Vlasyuk, E. V. Emelianov, V. V. Sasyuk, A. V. Perkov, S. F. Bondar, T. E. Burlakova, S. N. Fabrika, I. I. Romanyuk

Abstract

The light curves for almost 50 thousand stars with magnitudes (min[11overset{textrm{m}}{.}5,19overset{textrm{m}}{.}5]) have been obtained over 2.5 years at SAO RAS in the process of conducting an exoplanet survey in roughly (1overset{circ}{.}5)-sized fields around the white dwarfs WD 0009(+)501 and GRW (+)708247. In this paper we present a catalog of variable stars that have been found in the considered regions. Periodogram analysis was used as the main variation search method. The catalog includes 150 periodic variable stars: 113 of them have been known previously, and for the remaining 37 variations have been discovered for the first time. These stars were classified according to the nature of the variations into four eclipsing variable and three pulsating types, as well as rotating stars. We present the periods and variation amplitudes in the range of (Pin[0overset{textrm{d}}{.}036,32overset{textrm{d}}{.}14]) and (Delta min[0overset{textrm{m}}{.}0064,1overset{textrm{m}}{.}45]), determined from the investigated data.

Abstract The light curves for almost 50 thousand stars with magnitudes （m/in[11verset{textrm{m}}{.}5,19verset{textrm{m}}{.}5]） have been obtained over 2.在白矮星 WD 0009(+)501 和 GRW(+)708247 周围的大约 (1verset{circ}{.}5)大小的场中进行系外行星巡天的过程中，在 SAO RAS 进行了为期 5 年的观测。在本文中，我们介绍了在所考虑的区域内发现的变星星表。周期图分析被用作主要的变星搜索方法。星表中包括150颗周期变星：其中113颗是以前已知的，其余37颗变星是首次发现的。根据变异的性质，这些恒星被分为四种蚀变型和三种脉动型，以及旋转型恒星。我们给出了根据调查数据确定的周期和变幅范围（Pin[0verset{textrm{d}}{.}036,32verset{textrm{d}}{.}14]）以及（Delta min[0verset{textrm{m}}{.}0064,1overset{textrm{m}}{.}45] ）。

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引用次数: 0

Accretion-driven Spin-up of the White Dwarfs in AR Scorpii and AE Aquarii 天蝎座（AR Scorpii）和宝瓶座（AE Aquarii）白矮星的冲积驱动自旋上升

IF 1.2 4区物理与天体物理 Q3 Physics and Astronomy

Astrophysical Bulletin

Pub Date : 2024-05-08 DOI: 10.1134/s1990341323600254

N. G. Beskrovnaya, N. R. Ikhsanov

Abstract

The problem caused by the inconsistency between the age and spin-down time scale of the white dwarfs in the systems AR Sco and AE Aqr is discussed within the hypothesis of their accretion-driven spin-up during the previous epoch. Considering a scenario of accretion from a Keplerian disk, we conclude that the white dwarfs in these systems could be spun-up to the currently observed periods provided the radius of their magnetospheres at the spin-up phase was substantially smaller than the Alfven radius. We show that the required magnetospheric radius value can be reached if the accretion flow penetrates the magnetic field of the white dwarf at its magnetospheric boundary due to anomalous (Bohm) diffusion. In this case the spin-up of the white dwarfs in the systems under consideration can be described based on a model of stationary accretion from the Keplerian disk at an average rate of (10^{-9}{-}10^{-8}M_{odot}) yr({}^{-1}) without any additional assumptions about the evolution of the intrinsic magnetic field of the white dwarfs during the spin-up phase.

摘要我们讨论了 AR Sco 和 AE Aqr 系统中的白矮星的年龄和自旋下降时间尺度不一致所引起的问题，并提出了它们在上一纪元由吸积驱动自旋上升的假说。考虑到从开普勒盘吸积的情况，我们得出结论，如果这些星系中的白矮星在自旋上升阶段的磁层半径大大小于阿尔弗文半径，那么它们可以自旋上升到目前观测到的周期。我们的研究表明，如果吸积流由于反常（玻姆）扩散而穿透了白矮星磁层边界的磁场，就可以达到所需的磁层半径值。在这种情况下，我们所考虑的系统中白矮星的自旋上升可以根据开普勒磁盘的静态增殖模型来描述，其平均速率为(10^{-9}{-}10^{-8}M_{odot}) yr({}^{-1}) ，而不需要对自旋上升阶段白矮星固有磁场的演化做任何额外的假设。

引用次数: 0

Light Curves of Lensed Components and Time Delay Measurements in the Binary Gravtationally Lensed Quasars SDSS J2124 $$+$$ 1632 and SDSS J0806 $$+$$ 2006 双引力凝聚类星体 SDSS J2124 $+$$$ 1632 和 SDSS J0806 $+$$ 2006 中凝聚成分的光变曲线和时间延迟测量结果

IF 1.2 4区物理与天体物理 Q3 Physics and Astronomy

Astrophysical Bulletin

Pub Date : 2024-05-08 DOI: 10.1134/s1990341323600278

D. Kh. Bekov, T. A. Akhunov, O. A. Burkhonov, N. R. Alimova

Abstract

The article presents the results of long-term photometric monitoring of two binary gravitationally lensed quasars, SDSS J2124(+)1632 and SDSS J0806(+)2006, carried out at the Maidanak Observatory in 2017–2022. The obtained light curves of the lensed components of both systems are analyzed. The variability of SDSS J2124(+)1632 turned out to be quite large: up to (0overset{textrm{m}}{.}50) for the system as a whole and up to (0overset{textrm{m}}{.}75) for component A. Long-term microlensing was found against the background of a general increase in the apparent brightness of the quasar source. The brightness variations in SDSS J0806(+)2006 are less intense: the range is about (0overset{textrm{m}}{.}20) for the system as a whole, and up to (0overset{textrm{m}}{.}25) for both components. Analysis of the light curves did not show the presence of microlensing here. We also calculated the probable values of the time delay: (Delta t_{textrm{AB}}=102pm 20) days (component B is in the lead) and (Delta t_{textrm{AB}}=-53.0pm 6.0) days (component A is in the lead) in SDSS J2124(+)1632 and SDSS J0806(+)2006, respectively. The value of (Delta t_{textrm{AB}}) for SDSS J2124(+)1632 is consistent with previously found time delays for binary gravitationally lensed systems. In the case of the second system, the time delay is consistent with earlier theoretical calculations, which suggested that the time delay should be about 50 days.

摘要文章介绍了2017-2022年在迈达纳克天文台对两颗双引力透镜类星--SDSS J2124(+)1632 和 SDSS J0806(+)2006 --进行长期光度监测的结果。对所获得的这两个系统透镜组件的光变曲线进行了分析。结果发现SDSS J2124(+)1632 的变率相当大：整个系统高达(0overset{textrm{m}}{.}50)，A部分高达(0overset{textrm{m}}{.}75)。SDSS J0806(+)2006 的亮度变化并不那么强烈：整个系统的变化范围大约是 (0overset{textrm{m}}{.}20)，而两个部分的变化范围则高达 (0overset{textrm{m}}{.}25)。对光曲线的分析表明，这里并不存在微透镜现象。我们还计算了时间延迟的可能值：在SDSS J2124(+)1632 和SDSS J0806(+)2006 中，我们还分别计算了可能的时间延迟值：（Delta t_{textrm{AB}}=102pm 20 ）天（B成分处于领先地位）和（Delta t_{textrm{AB}}=-53.0pm 6.0 ）天（A成分处于领先地位）。SDSS J2124(+)1632 的(Delta t_{textrm{AB}})值与之前发现的双引力透镜系统的时间延迟一致。在第二个系统的情况下，时间延迟与早先的理论计算是一致的，后者认为时间延迟应该是大约50天。

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引用次数: 0

A Search for Evolutionary Changes in the Period of Classical Cepheid KN Cen 寻找经典仙王座 KN Cen 期间的进化变化

IF 1.2 4区物理与天体物理 Q3 Physics and Astronomy

Astrophysical Bulletin

Pub Date : 2024-05-08 DOI: 10.1134/s1990341324700251

L. N. Berdnikov, A. K. Dambis

Abstract

All available photometry for the Cepheid KN Cen is analyzed to construct its ((O-C)) diagram spanning a 134-year long time interval. This made it possible for the first time to compute the rate of evolutionary period increase of the Cepheid, (dP/dt=+2.91(pm{1.68})) s yr({}^{-1}), which is consistent with the results of model computations for the third crossing of the instability strip. The test for stability of pulsations proposed by Lombard and Koen confirmed the reality of the evolutionary period change.

Abstract 对仙王座KN Cen的所有现有光度测量进行了分析，以构建其跨越134年长时间间隔的（(O-C)）图。这使得首次计算出仙王座的演化周期增加率成为可能，（(dP/dt=+2.91(pm{1.68})) s yr({}^{-1}), 这与不稳定带第三次交叉的模型计算结果是一致的。Lombard 和 Koen 提出的脉动稳定性检验证实了演化周期变化的真实性。

引用次数: 0

Problems of Determining the Degree of Star Concentration Towards the Center of Globular Clusters 确定球状星团中心恒星集中程度的问题

IF 1.2 4区物理与天体物理 Q3 Physics and Astronomy

Astrophysical Bulletin

Pub Date : 2024-05-08 DOI: 10.1134/s1990341324600078

S. J. Turaev, S. N. Nuritdinov, A. S. Rastorguev, I. U. Tadjibaev

Abstract

In this paper, we analyze the apparent surface density observations of 81 globular clusters provided by Gaia DR2. The problems of analyzing these observations and their differences from similar data obtained using the HST are discussed. Based on the results of this analysis of the quality of observational data and a number of physical considerations, we separate globular clusters into three classes and then consider the issues of modeling the apparent surface density versus distance. The values of the free parameters of the model are found by the symplectic minimization method. The free parameters including the concentration parameter are for the first time found using the 4-parameter generalized model we propose.

摘要本文分析了Gaia DR2提供的81个球状星团的视表面密度观测数据。文中讨论了分析这些观测数据的问题，以及它们与利用 HST 获得的类似数据之间的差异。根据对观测数据质量的分析结果和一些物理方面的考虑，我们将球状星团分为三类，然后考虑视表面密度随距离变化的建模问题。模型的自由参数值是通过交点最小化方法求得的。通过我们提出的 4 参数广义模型，首次找到了包括浓度参数在内的自由参数。

引用次数: 0

Origin and Evolution of Large-Scale Magnetic Fields of Chemically Peculiar Stars. I. Intermediate-Age Clusters 化学奇异恒星大规模磁场的起源与演化。I. 中龄星团

IF 1.2 4区物理与天体物理 Q3 Physics and Astronomy

Astrophysical Bulletin

Pub Date : 2024-05-08 DOI: 10.1134/s1990341323600357

I. I. Romanyuk, I. A. Yakunin, A. V. Moiseeva, E. A. Semenko, D. O. Kudryavtsev, V. N. Aitov

Abstract

Chemically peculiar (CP) stars of early spectral types are the only Main-Sequence objects of the Hertzsprung–Russel diagram that have strong magnetic fields covering the entire surface of a star and maintaining a stable structure on a scale of at least decades. The origin and evolution of magnetic fields of CP stars are still a subject of discussion, despite significant progress in the field of observation of stellar magnetic fields and their theoretical description. This situation has developed not least because of the problem of accurately determining the age of CP stars. We performed a review of magnetic fields of CP stars in the Orion OB1 association and five intermediate-age clusters ((alpha) Per, Pleiades, NGC 7092, and IC 4756) and found evidence of a strong decrease in the proportion and strength of magnetic fields of CP stars relative to normal stars of the same spectral types. The found dependences can serve as confirmation of the fossil nature of large-scale magnetic fields of stars. The conclusions of this paper are based on the measurements of more than 800 spectra obtained in the period from 2013 to 2023 with the Main Stellar Spectrograph of the 6-m BTA Telescope for about 100 stars.

摘要早期光谱型的化学奇特（CP）恒星是赫兹普朗-鲁塞尔图中唯一具有覆盖恒星整个表面并保持至少几十年稳定结构的强磁场的主序天体。尽管在恒星磁场观测和理论描述领域取得了重大进展，CP 星磁场的起源和演化仍然是一个讨论主题。造成这种情况的主要原因是CP恒星年龄的准确测定问题。我们对猎户座OB1星团和五个中年星团（(α) Per、昴宿星团、NGC 7092和IC 4756）中的CP星的磁场进行了回顾，发现CP星的磁场比例和强度相对于相同光谱类型的正常恒星来说都有很强的下降。所发现的依赖关系可以证实恒星大尺度磁场的化石性质。本文的结论是基于 2013 年至 2023 年期间利用 6 米 BTA 望远镜的主恒星摄谱仪对大约 100 颗恒星的 800 多条光谱进行测量而得出的。

{"title":"Origin and Evolution of Large-Scale Magnetic Fields of Chemically Peculiar Stars. I. Intermediate-Age Clusters","authors":"I. I. Romanyuk, I. A. Yakunin, A. V. Moiseeva, E. A. Semenko, D. O. Kudryavtsev, V. N. Aitov","doi":"10.1134/s1990341323600357","DOIUrl":"https://doi.org/10.1134/s1990341323600357","url":null,"abstract":"<h3 data-test=\"abstract-sub-heading\">Abstract</h3>Chemically peculiar (CP) stars of early spectral types are the only Main-Sequence objects of the Hertzsprung–Russel diagram that have strong magnetic fields covering the entire surface of a star and maintaining a stable structure on a scale of at least decades. The origin and evolution of magnetic fields of CP stars are still a subject of discussion, despite significant progress in the field of observation of stellar magnetic fields and their theoretical description. This situation has developed not least because of the problem of accurately determining the age of CP stars. We performed a review of magnetic fields of CP stars in the Orion OB1 association and five intermediate-age clusters ((alpha) Per, Pleiades, NGC 7092, and IC 4756) and found evidence of a strong decrease in the proportion and strength of magnetic fields of CP stars relative to normal stars of the same spectral types. The found dependences can serve as confirmation of the fossil nature of large-scale magnetic fields of stars. The conclusions of this paper are based on the measurements of more than 800 spectra obtained in the period from 2013 to 2023 with the Main Stellar Spectrograph of the 6-m BTA Telescope for about 100 stars.","PeriodicalId":478,"journal":{"name":"Astrophysical Bulletin","volume":null,"pages":null},"PeriodicalIF":1.2,"publicationDate":"2024-05-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140932428","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Activity of K-Dwarf HIP 113103 and Atmospheric Losses of Its Exoplanets K 矮星 HIP 113103 的活动及其系外行星的大气损耗

IF 1.2 4区物理与天体物理 Q3 Physics and Astronomy

Astrophysical Bulletin

Pub Date : 2024-05-08 DOI: 10.1134/s199034132460008x

I. S. Savanov

Abstract

We present the results of analyzing the activity manifestations of the K3 V spectral type dwarf HIP 113103 (HD 216530) and estimate the matter loss from the atmospheres of two of its planets. HIP 113103 can be classified as a relatively young object with an age of about 470 million years—1 billion years. Using the standard method, based on the observed data from the TESS mission, we estimated the areas of spots on the surface of the star, which exceed the maximum area of spots on the Sun and are 6100 and 4950 MSH for sectors 1 and 28, respectively. According to the data from the observation archive of the All Sky Automated Survey, the activity cycles of HIP 113103 have been established to last about 610, 825, and 1030 days (1.7, 2.3, and 2.8 years, respectively). Both planets in the stellar system HIP 113103 are characterized as objects with radii of 1.829(R_{oplus}) and 2.400(R_{oplus}), with periods of 7.6 and 14.2 days, respectively, lying on opposite sides of the Fulton Gap in the ‘‘Period—Radius’’ diagram. The loss of matter from the planetary atmospheres was calculated using an approximation formula corresponding to the energy-limited atmospheric loss model. To estimate the flux of XUV photons, analytical dependences were used connecting flux values and the (log R^{prime}_{textrm{HK}}) parameter. It was found that the values (dot{M}) values for planets b and c are equal to (2.8times 10^{8}) g s({}^{-1}) and (1.9times 10^{8}) g s({}^{-1}), respectively. The planet HIP 113103 b attracts special attention because, with its radius (R_{p}=1.829R_{oplus}), it belongs to a small population of planets with the radii (1.5R_{oplus}<R_{p}<2.0R_{oplus}), which characterizes the evolution of super-Earths and mini-Neptunes. HIP 113103 c has a radius of (R_{p}=2.40R_{oplus}) and an equilibrium temperature of (585pm 10) K which characterizes the object as an already established warm mini-Neptune. A comparison of the properties of planets b and c is of interest, since they belong to the same system, are irradiated by the same star, probably have similar ages and conditions of formation, etc.

摘要我们展示了对K3 V光谱型矮星HIP 113103（HD 216530）的活动表现的分析结果，并估算了其两颗行星大气中的物质损失。HIP 113103可以归类为一个相对年轻的天体，年龄约为4.7亿年-10亿年。根据 TESS 任务的观测数据，我们使用标准方法估算出了恒星表面的光斑面积，它超过了太阳上光斑的最大面积，1 区和 28 区的光斑面积分别为 6100 MSH 和 4950 MSH。根据全天空自动巡天观测档案中的数据，HIP 113103 的活动周期分别为 610 天、825 天和 1030 天（1.7 年、2.3 年和 2.8 年）。恒星系统HIP 113103中的两颗行星的半径分别为1.829（R_{oplus}）和2.400（R_{oplus}），周期分别为7.6天和14.2天，位于 "周期-半径 "图中富尔顿缺口的两侧。行星大气中物质的损耗是通过与能量有限大气损耗模型相对应的近似公式计算得出的。为了估算 XUV 光子的通量，使用了通量值和(log R^{prime}_{textrm{HK}}) 参数之间的分析依赖关系。结果发现，行星b和c的(dot{M})值分别等于(2.8/times 10^{8}) g s({}^{-1}) 和(1.9/times 10^{8}) g s({}^{-1}) 。行星HIP 113103 b引起了特别的关注，因为它的半径为(R_{p}=1.829R_{oplus})，属于半径为(1.5R_{oplus}<R_{p}<2.0R_{oplus})的小行星群，这也是超级地球和小海王星演化的特征。HIP 113103 c的半径为(R_{p}=2.40R_{oplus})，平衡温度为(585/pm 10) K，这表明该天体是一颗已经确定的温暖的小海王星。对行星b和c的性质进行比较是很有意义的，因为它们属于同一个系统，受到同一颗恒星的辐照，可能具有相似的年龄和形成条件等等。

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引用次数: 0

Variations of the Properties of Magnetic Stars with Age 磁性恒星特性随年龄的变化

IF 1.2 4区物理与天体物理 Q3 Physics and Astronomy

Astrophysical Bulletin

Pub Date : 2024-05-08 DOI: 10.1134/s1990341324600091

Yu. V. Glagolevskij

Abstract

The age estimates of magnetic stars obtained from the ages of clusters and associations are compared with those determined using the grids of evolutionary paths and isochrones separately for each star. Large deviations between the age systems have been discovered. Analysis of the studies that use ‘‘cluster’’ ages shows that they differ significantly from those obtained using individual estimates.

摘要通过星团和星团的年龄获得的磁性恒星的年龄估计值，与使用演化路径网格和等时线分别为每颗恒星确定的年龄估计值进行了比较。发现这两种年龄系统之间存在很大的偏差。对使用''星团''年龄的研究进行的分析表明，它们与使用单个估计值得到的年龄有很大不同。

引用次数: 0

Programmable Radiometer-noise Model with Random Drift Contribution 具有随机漂移贡献的可编程辐射计噪声模型

IF 1.2 4区物理与天体物理 Q3 Physics and Astronomy

Astrophysical Bulletin

Pub Date : 2024-05-08 DOI: 10.1134/s199034132360045x

V. N. Chernenkov

Abstract

A method for radiometer-noise generation and its software implementation in the form of a Python library module is proposed. The method can be used to simulate radiometer noise with variable component properties: Gaussian white noise and flicker noise (random drift) with a power spectrum linearly increasing with decreasing frequency. The method is based on the transformation of spectral properties of Gaussian noise via sequential filtering by a differentiator, nonlinear threshold switch, and subsequent integration. By changing the integrator accumulation time constant and the threshold level relative to noise intensity (sigma) one can change the resulting form of the spectrum and the corresponding statistical parameters of the output noise over a wide range: from stationary white noise to noise dominated by a (1/f)-type spectrum component. Empirical polynomial approximation formulas for the dependence of the spectral index of the resulting noise records on the nonlinear threshold switch level in the 0.0–(3.5sigma) interval are derived based on numerical simulations using a software implementation of the model. Examples of noise-record implementations, their spectra, and autocorrelation functions are demonstrated. The generated noise is shown to be similar to the noise observed on radio telescopes of the Institute of Applied Astronomy of the Russian Academy of Sciences.

摘要提出了一种辐射计噪声生成方法及其 Python 库模块形式的软件实现。该方法可用于模拟具有可变成分特性的辐射计噪声：高斯白噪声和闪烁噪声（随机漂移）的功率谱随频率的降低而线性增加。该方法的基础是通过微分器、非线性阈值开关和随后的积分对高斯噪声的频谱特性进行转换。通过改变积分器的累积时间常数和相对于噪声强度的阈值水平，可以在很大范围内改变频谱的形式和输出噪声的相应统计参数：从静态白噪声到由(1/f)型频谱成分主导的噪声。根据使用模型软件实现的数值模拟，得出了在 0.0-(3.5sigma) 区间噪声记录的频谱指数对非线性阈值开关电平的依赖性的经验多项式近似公式。演示了噪声记录实现、其频谱和自相关函数的例子。结果表明，生成的噪声与俄罗斯科学院应用天文学研究所射电望远镜观测到的噪声相似。

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