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Variations in the Radiation Intensity of Pulsar B0950+08: Nine Years of Monitoring at 110 MHz 脉冲星 B0950+08 辐射强度的变化:在 110 兆赫频率上的九年监测
IF 1.1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-10-25 DOI: 10.1134/S1063772924700707
T. V. Smirnova, M. O. Toropov, S. A. Tyul’bashev

Variations in the radiation intensity of pulsar B0950+08 from 2014 to 2022 with scales from minutes to years were analyzed. The observations were obtained in daily survey using the Large Phased Array (LPA) radio telescope. The high variability of radiation is shown both from pulse to pulse and on scales greater than 3 min. The average value of the estimated amplitude of these variations in 3.2 min is 25 Jy, the modulation index is unity. The average relative amplitude of the interpulse (IP) is (2.00 pm 0.28% ) of the main pulse. In individual pulses, the amplitude of the interpulse may exceed the amplitude of the main pulse (MP), but this is a rare event. Radiation is observed in almost the entire period of the pulsar. For the first time, the relative amplitude of radiation between the main pulse and the interpulse (radiation bridge) was measured. When averaging for ~10 h, it varies from 0.8 to 1.31% with an average value of (1.04 pm 0.28% ). A high correlation between MP and IP amplitude variations both when averaging profiles over 3.2 min and when averaging over years was found. This correlation is due to refractive interstellar scintillation. The frequency scale of IP diffraction interstellar scintillation was measured for the first time, and that the spectral shapes for IP and MP were shown to be well correlated and have the same frequency scale. There are strong variations in the frequency scale of scintillation ({{f}_{{{text{dif}}}}}) from session to session (time interval from one day) on scales of 200–800 kHz. The refractive scale of scintillation of 1–2 days was determined. A modulation of radiation with a characteristic scale of ~130 days, which, apparently, is also associated with refractive scintillation, was found.

分析了脉冲星B0950+08的辐射强度在2014年至2022年期间从分钟到年的变化。这些观测数据是利用大型相控阵(LPA)射电望远镜在日常巡天中获得的。无论是从脉冲到脉冲,还是从大于 3 分钟的时间尺度来看,辐射的变化都很大。这些变化在 3.2 分钟内的估计振幅平均值为 25 Jy,调制指数为 1。脉冲间(IP)的平均相对振幅是主脉冲的(2.00 pm 0.28% )。在个别脉冲中,间脉冲的振幅可能会超过主脉冲(MP)的振幅,但这种情况很少发生。几乎在脉冲星的整个周期都能观测到辐射。我们首次测量了主脉冲和间脉冲(辐射桥)之间的相对辐射振幅。当平均约 10 h 时,它在 0.8%到 1.31%之间变化,平均值为(1.04 pm 0.28 %)。在对 3.2 分钟的剖面图进行平均和对数年的剖面图进行平均时,发现 MP 和 IP 振幅变化之间有很高的相关性。这种相关性是由于折射星际闪烁造成的。首次测量了 IP 衍射星际闪烁的频率尺度,结果表明 IP 和 MP 的光谱形状具有良好的相关性和相同的频率尺度。不同时段(时间间隔为一天)闪烁的频标({{f}_{text{dif}}}}} )在 200-800 kHz 的范围内有强烈的变化。确定了 1-2 天的闪烁折射率。发现辐射的调制具有 ~130 天的特征尺度,显然也与折射闪烁有关。
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引用次数: 0
Non-Thermal Processes of Nitric Oxide Formation during Precipitation of Auroral Electrons into the Upper Atmospheres of Terrestrial Planets 极光电子沉降到地球星高层大气期间一氧化氮的非热形成过程
IF 1.1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-10-25 DOI: 10.1134/S1063772924700744
V. Shematovich, D. Bisikalo, G. Tsurikov, A. Zhilkin

Nitric oxide is a potential biomarker in the N2–O2 atmospheres of terrestrial exoplanets, which can be detected by space missions, including the planned launch of the Russian Spektr-UV observatory. From observations of the Earth’s thermosphere in the polar regions, it is known that important sources of formation of this molecule are the precipitation of high-energy electrons into the planet’s atmosphere, as well as the non-thermal processes accompanying them. In this paper, we study the non-thermal processes of nitric oxide formation in the polar regions of the Earth’s upper atmosphere, as well as the atmospheres of exoplanets located in the potential habitable zone of active stars. For this purpose the following models are developed: a numerical kinetic Monte Carlo model of the interaction of energetic electrons with atmospheric gas, a kinetic Monte Carlo model of the interaction of suprathermal N(4S) atoms formed as a result of dissociation of N2 molecules by electron impact with the surrounding gas; a model of odd nitrogen chemistry with molecular and eddy diffusion. Based on results of calculations, it is confirmed that the process of dissociation of N2 by an electron impact during the interaction of the stellar wind with the atmosphere of the planet is an important source of suprathermal N atoms, which contribute to a significant increase in the non-thermal formation of NO in the N2–O2 atmospheres of terrestrial planets (both locally, in the case of a planet’s own magnetic field, and throughout the whole planet’s surface, in case of its absence). Since the column concentration of NO during flares becomes larger, therefore, the chances of detecting of nitric oxide biomarker in the atmospheres of the terrestrial-type exoplanets located in the potential habitable zone of active stars are also become larger.

一氧化氮是地外行星大气中 N2-O2 的潜在生物标志物,可通过空间飞行任务(包括计划发射的俄罗斯 Spektr-UV 观测站)探测到。通过对地球极地热大气层的观测,我们知道形成这种分子的重要来源是进入行星大气层的高能电子沉淀,以及伴随这些电子沉淀的非热过程。在本文中,我们研究了地球高层大气极区以及位于活跃恒星潜在宜居带的系外行星大气中一氧化氮形成的非热过程。为此开发了以下模型:高能电子与大气气体相互作用的蒙特卡洛动力学数值模型、N2 分子在电子撞击下解离而形成的超热 N(4S)原子与周围气体相互作用的蒙特卡洛动力学模型;带有分子和涡流扩散的奇数氮化学模型。根据计算结果证实,在恒星风与行星大气相互作用过程中,电子撞击解离 N2 的过程是超热 N 原子的一个重要来源,它有助于显著增加陆地行星 N2-O2 大气中 NO 的非热形成(在行星自身有磁场的情况下是局部增加,而在没有磁场的情况下则是整个行星表面增加)。由于耀斑期间一氧化氮的柱浓度变得更大,因此在位于活跃恒星潜在宜居带的类地行星大气层中检测到一氧化氮生物标记的机会也变得更大。
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引用次数: 0
Analysis of Gradient Profiles and Morphology of the Vela Jr. Supernova Remnant 小维拉超新星残留物的梯度剖面和形态分析
IF 1.1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-10-25 DOI: 10.1134/S1063772924700690
S. A. Pronicheva, A. F. Iyudin

We present the study of gradient profiles of the Vela Jr. northwestern rim in X-ray emission and the morphology of this supernova remnant in various spectral ranges of electromagnetic radiation to estimate the distance to the object and its age. This work involves radiation intensity spatial distributions for the northwestern rim of the supernova remnant RX J0852.0–4622 in the X-ray energy range, 1000.0–2000.0 eV, obtained from measurements of the EPIC-pn camera of the XMM-Newton space observatory for four consecutive time intervals. From the calculated shifts over the period from 2004 to 2018 of the X-ray intensity profiles along the northwestern rim of Vela Jr., limits were obtained on the angular expansion rate of the shock wave of this remnant’s region into a cloud of gas, probably hydrogen: minimum speed (V_{theta }^{{{text{max}}}}) = 0.29('' ) ± 0.04('' ) year–1 and maximum (V_{theta }^{{60}}) = 0.82('' ) ± 0.11('' ) year–1. The hydrogen cloud with which the supernova shock wave interacts along the northwestern rim of Vela Jr. is very inhomogeneous. The upper limits for the age of the remnant and the distance to it based on the cloud density estimate are 1920 years and 450 pc, respectively. More stringent restrictions on such parameters of RX J0852.0–4622 as its age and distance to it were obtained by analyzing the remnant’s two-ring morphology based on its images in ultraviolet, X-ray, radio and gamma rays: 1190 ± 250 years and 280 ± 60 pc.

我们介绍了小维拉西北边缘在 X 射线辐射中的梯度剖面以及该超新星残余物在不同电磁辐射光谱范围内的形态研究,以估算该天体的距离和年龄。这项工作涉及超新星残余物RX J0852.0-4622西北边缘在X射线能量范围(1000.0-2000.0 eV)内的辐射强度空间分布,这是XMM-牛顿空间观测站的EPIC-pn照相机连续四个时间间隔的测量结果。通过计算 2004 年至 2018 年期间沿小维拉西北边缘的 X 射线强度剖面的偏移,得出了小维拉角扩张的极限、得出了这一残余区域的冲击波进入气体云(可能是氢)的角膨胀率极限:最小速度(V_{theta }^{{text{max}}}}) = 0.29(' ) ± 0.04(' ) year-1,最大速度(V_{theta }^{60}}) = 0.82(' ) ± 0.11(' ) year-1。沿小维拉西北边缘与超新星冲击波相互作用的氢云非常不均匀。根据云密度估算的残余物年龄和距离上限分别为1920年和450 pc。对 RX J0852.0-4622 的年龄和距离等参数进行更严格的限制,是通过分析残余物的双环形态,根据其紫外线、X 射线、射电和伽马射线图像得出的:1190 ± 250 年和 280 ± 60 pc。
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引用次数: 0
Relative Distances and Peculiar Velocities of 140 Groups and Clusters of Galaxies at Low Redshifts: the Hubble Diagram 低红移下 140 个星系群和星系团的相对距离和奇异速度:哈勃图
IF 1.1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-10-25 DOI: 10.1134/S1063772924700756
F. G. Kopylova, A. I. Kopylov

To determine the relative distances and peculiar velocities of 140 groups and clusters of galaxies at low redshifts (z < 0.12), we used the fundamental plane (FP) of early-type galaxies (from the Sloan Digital Sky Survey (SDSS) data). We constructed the Hubble diagram for the relative distances of galaxy groups/clusters versus their radial velocities in the cosmic microwave background (CMB) reference frame in the flat Λ cold dark matter (ΛLCDM) model (Ωm = 0.3 and H0 = 70 km s–1 Mpc–1). We have found that the standard logarithmic deviation for groups and clusters of galaxies on the Hubble diagram (minus peculiar velocities) is ±0.0173 (N = 140), which corresponds to a deviation of 70 ± 2.8 km s–1 Mpc–1 in the Hubble constant. For a sample of galaxy systems (N = 63), the X-ray luminosity of which is in an interval of (0.151‒4) × 1044 erg/s, this quantity turned out to be 70 ± 2.1 km s–1 Mpc–1. The root-mean-square deviations of peculiar velocities with quadratic accounting for errors are ({{langle V_{{{text{pec}}}}^{2}rangle }^{{1/2}}}) = 714 ± 7 and 600 ± 7 km/s, respectively. For five large superclusters of galaxies from the SDSS region, the average peculiar velocity relative to the CMB reference frame is +240 ± 250 km/s. We detected no outflow of galaxy systems from the void (Giant Void; α ≈ 13h, δ ≈ 40°, and z ≈ 0.107) formed by groups and clusters of galaxies.

为了确定低红移(z <0.12)时140个星系群和星系团的相对距离和奇特速度,我们使用了早期型星系的基面(FP)(来自斯隆数字巡天(SDSS)数据)。在平Λ冷暗物质(ΛLCDM)模型(Ωm = 0.3 和 H0 = 70 km s-1 Mpc-1)中,我们构建了星系团/星系簇在宇宙微波背景(CMB)参照系中的相对距离与径向速度的哈勃图。我们发现,哈勃图上星系群和星系团的标准对数偏差(减去奇特速度)为±0.0173(N = 140),相当于哈勃常数的偏差为 70 ± 2.8 km s-1 Mpc-1。对于 X 射线光度在 (0.151-4) × 1044 erg/s 之间的星系系统样本(N = 63)来说,这个量是 70 ± 2.1 km s-1 Mpc-1。计算误差的奇特速度均方根偏差分别为({{langle V_{{{pec}}}}^{2}rangle }^{{1/2}}} )= 714 ± 7 和 600 ± 7 km/s。对于来自SDSS区域的五个大型超星系团来说,相对于CMB参照系的平均奇特速度是+240 ± 250 km/s。我们没有探测到由星系群和星系团形成的星系系统从虚空(Giant Void;α ≈ 13h,δ ≈ 40°,z ≈ 0.107)中流出。
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引用次数: 0
A Survey of High-Mass Star Forming Regions in the Line of Singly Deuterated Ammonia NH2D 单氘化氨 NH2D 线高质量恒星形成区调查
IF 1.1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-10-25 DOI: 10.1134/S1063772924700719
E. A. Trofimova, I. I. Zinchenko, P. M. Zemlyanukha, M. Thomasson

The present survey represents a continuation of our study of high mass star forming regions in the lines of deuterated molecules, the first results of which were published in [1]. This paper present the results of observations of 50 objects in the line of ortho modification of singly deuterated ammonia NH2D (1_{{11}}^{s}{-} 1_{{01}}^{a}) at a frequency of 85.9 GHz, carried out using the 20-m radio telescope of the Onsala Space Observatory (Sweden). This line is detected in 29 sources. The analysis of obtained data, as well as the fact that the gas density in the investigated sources, according to independent estimates, is significantly lower than the critical density for this NH2D transition, indicate non-LTE excitation of NH2D. Based on non-LTE modeling, estimates of the relative content of the NH2D molecule and the degree of deuterium enrichment were obtain, and the dependencies of these parameters on temperature and velocity dispersion were analyzed with and without taking into account detection limits assuming the same gas density in all sources. An anti-correlation between the NH2D relative abundances and the kinetic temperature is revealed in a temperature range of 15–50 K. At the same time, a significant decrease in the ratio of the NH2D/NH3 abundances with increasing temperature, predicted by the available chemical models, is not observed under the adopted assumptions. An anti-correlation was also revealed between the relative content of the main isotopologue of ammonia NH(_{3}) and the velocity dispersion, while no statistically significant correlation with the kinetic temperature of sources in the same temperature range was found.

本次调查是我们对氘化分子谱线中高质恒星形成区研究的继续,其第一批结果发表于[1]。本文介绍了利用瑞典昂萨拉空间天文台(Onsala Space Observatory)的 20 米射电望远镜,在 85.9 千兆赫的频率下,对 50 个天体的单氘化氨 NH2D (1_{{11}}^{s}{-} 1_{{01}}^{a}) 正交修饰线的观测结果。在 29 个源中探测到了这条线。对所获数据的分析,以及根据独立估算得出的调查来源中的气体密度明显低于 NH2D 转变的临界密度这一事实,都表明 NH2D 受到了非 LTE 激发。在非 LTE 模型的基础上,对 NH2D 分子的相对含量和氘富集程度进行了估算,并分析了这些参数对温度和速度色散的依赖关系,同时假设所有来源中的气体密度相同,并将探测极限考虑在内。在 15-50 K 的温度范围内,发现 NH2D 相对丰度与动力学温度之间存在反相关关系。同时,在所采用的假设条件下,没有观察到现有化学模型所预测的 NH2D/NH3 丰度比随温度升高而显著降低的现象。氨的主要同位素NH(_{3})的相对含量与速度弥散之间也存在反相关关系,而在同一温度范围内,与源的动力学温度之间没有发现统计学上的显著相关性。
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引用次数: 0
Determining the Structure of the Atmosphere Exoplanet HD 189733b Based on Multicolor Photometric Transit Observations 根据多色测光凌日观测确定系外行星 HD 189733b 的大气层结构
IF 1.1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-10-25 DOI: 10.1134/S1063772924700689
E. V. Bekesov

In this paper, we analyze and interpret light curves obtained by observing with the HST telescope the transit of exoplanet HD 189733b across the disk of the star. Observations are carried out in a wide wavelength range of 5500–10 500 Å, which makes it possible to identify the relation between the wavelength and the data obtained during the interpretation of the radius of the planet. It is also shown that this dependence can be explained by the presence of a Rayleigh atmosphere on the planet while the possible parameters of this atmosphere are also approximately estimated.

在本文中,我们分析并解释了利用 HST 望远镜观测系外行星 HD 189733b 穿越恒星盘面所获得的光变曲线。观测是在 5500-10500 Å 的宽波长范围内进行的,这使得在解释行星半径的过程中确定波长与所获数据之间的关系成为可能。观测结果还表明,这种依赖关系可以用行星上存在的雷利大气层来解释,同时还对这种大气层的可能参数进行了近似估算。
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引用次数: 0
Interstellar Scintillations of Sources B0821+394 and B1812+412 as Observed by the LPA LPI Radio Telescope LPA LPI 射电望远镜观测到的星际闪烁源 B0821+394 和 B1812+412
IF 1.1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-10-25 DOI: 10.1134/S1063772924700720
S. A. Tyul’bashev, I. V. Chashei, I. A. Grishanova, G. E. Tyul’basheva, I. A. Subaev

The search for long-term variability of compact components of radio sources B0821+394 and B1812+412 over an interval of ten years was carried out. The LPA LPI radio telescope with an operating frequency of 111 MHz was used for observations. According to our estimates, the characteristic time of variability for both sources is 1.5–2.5 years. It is shown that the observed variability is not related to intrinsic variations in the radiation flux, but is due to refractive scintillation on inhomogeneities of the interstellar medium. From the obtained upper estimates of the apparent angular dimensions of the sources, it follows that the main contribution to the scattering of radio emission is made by turbulent plasma concentrated in sufficiently thin screens, the distance to which does not exceed 300–400 pc.

对射电源 B0821+394 和 B1812+412 的紧凑成分进行了为期十年的长期变化搜索。观测使用了工作频率为 111 MHz 的 LPA LPI 射电望远镜。根据我们的估计,这两个来源的特征变率时间为 1.5-2.5 年。观测结果表明,观测到的变异与辐射通量的内在变化无关,而是由于星际介质的不均匀性造成的折射闪烁。根据所获得的星源视角尺寸上限估计,无线电辐射散射的主要原因是集中在足够薄的屏幕中的湍流等离子体,其距离不超过 300-400 pc。
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引用次数: 0
Aeronomy of the Atmosphere of Ultra-Hot Jupiter Kelt9b with Allowance for the Kinetics of Hydrogen Atom Levels 考虑到氢原子水平动力学的超热木星 Kelt9b 大气层大气物理学
IF 1.1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-10-25 DOI: 10.1134/S1063772924700732
I. F. Shaikhislamov, I. B. Miroshnichenko, M. S. Rumenskikh, A. V. Shepelin, A. G. Berezutsky, S. S. Sharipov, M. P. Golubovsky, A. A. Chibranov, M. L. Khodachenko

Ultra-hot Jupiter Kelt9b impels to reconsider existing models of the upper atmospheres of hot exoplanets, which were previously developed using examples of G or M star systems such as HD209458b and GJ436b. The unique conditions of interaction between the radiation of an A-class star and the atmosphere necessitate kinetic modeling of excited levels of elements, primarily the hydrogen atom. Kelt9b shows the absorption for several Balmer lines and lines of a number of heavy elements, the quantitative interpretation of which is an urgent problem. In this study, for the first time, 3D modeling of the atmosphere of a planet with a close location of the Roche lobe is implemented with allowance for the aeronomy and kinetics of excited hydrogen.

超热木星Kelt9b促使人们重新考虑现有的热系外行星上层大气模型,这些模型以前是利用G或M恒星系统(如HD209458b和GJ436b)的例子建立的。A 级恒星的辐射与大气之间相互作用的独特条件要求对元素(主要是氢原子)的激发水平进行动力学建模。Kelt9b 显示了几条巴尔默线和一些重元素线的吸收,对它们的定量解释是一个亟待解决的问题。在这项研究中,首次对一颗罗氏叶位置较近的行星的大气层进行了三维建模,并考虑到了激发氢的气态和动力学。
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引用次数: 0
Secular Evolution and Stability of Rings Around Rotationally Asymmetrical Bodies. Revision of the Problem 旋转不对称天体周围环的世俗演化和稳定性。问题的修正
IF 1.1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-10-06 DOI: 10.1134/S106377292470063X
B. P. Kondratyev, V. S. Kornoukhov

A method for studying the secular evolution and stabilization of the shape of rings in small celestial bodies that do not have shepherd satellites is developed. A model of a compound ring consisting of two close, generally non-coplanar elliptical Gaussian rings is constructed. The self-gravitation of the ring is taken into account through the mutual gravitational energy of the boundary rings Wmut. The function Wmut is presented as a series with an accuracy of up to the 4th power of small eccentricities and mutual inclination of the rings. The secular evolution of a compound ring is described by differential equations in special (collective) variables. For rings without a central body (problem 1), a closed system of eight differential equations is obtained using the mutual energy function. The evolution of rings in the azimuthally averaged potential of a rotating triaxial body is also studied (problem 2), for which a second system of eight differential equations is derived. In both problems, besides the general case, two particular ones are considered: (i) the case of coplanar elliptical rings, and (ii) the case of circular rings with a tilt. The theory is applied to study the recently discovered ring of dwarf planet Haumea. It is shown that without taking into account self-gravity, the nodal precession time of the Haumea ring is equal to TΩ = 12.9 ± 0.7d but taking into account the self-gravity of the ring can reduce this period. It is established that self-gravity does indeed contribute to the preservation of the ring shape without invoking the hypothesis of shepherd satellites. Criteria for the preservation of the ring shape are obtained, which made it possible to estimate the interval for the ratio of the ring mass to the mass of Haumea 10–4 < m/M < 10–3. Taking into account the optical thickness of the ring τ ≈ 0.5, it is shown that the Haumea ring with a mass m/M ≈ (1–2) × 10–4 can consist of ice particles with a size of ({{d}_{0}} approx 0.7{-} 1) m.

本文提出了一种研究没有牧夫卫星的小天体的环形状的世俗演变和稳定的方法。构建了一个复合环模型,该模型由两个接近的、一般为非共面的椭圆形高斯环组成。通过边界环的相互引力能量 Wmut 考虑了环的自引力。函数 Wmut 以数列形式表示,精确度可达小偏心率和环的相互倾角的 4 次幂。复合环的世俗演化由特殊(集合)变量微分方程描述。对于没有中心体的环(问题 1),利用互能函数可以得到由八个微分方程组成的封闭系统。此外,还研究了旋转三轴体方位角平均电势中环的演变(问题 2),并得出了第二个八微分方程系统。在这两个问题中,除了一般情况外,还考虑了两个特殊情况:(i) 共面椭圆环的情况和 (ii) 带倾斜的圆环的情况。该理论被用于研究最近发现的矮行星妊神星的星环。结果表明,在不考虑自重力的情况下,妊神星环的节点前摄动时间等于 TΩ = 12.9 ± 0.7d,但考虑星环的自重力可以缩短这一周期。研究证实,自重力确实有助于保持环的形状,而无需援引牧夫卫星的假说。获得了保持星环形状的标准,从而可以估算出星环质量与 Haumea 质量之比 10-4 < m/M < 10-3 的区间。考虑到星环的光学厚度τ ≈ 0.5,可以证明质量为m/M ≈ (1-2) × 10-4的妊神星环可以由大小为({{d}_{0}} 大约 0.7{-} 1) m)的冰粒组成。
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引用次数: 0
Parameters of Star Formation Regions in Galaxies NGC 3963 and NGC 7292 NGC 3963 和 NGC 7292 星系中恒星形成区的参数
IF 1.1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-10-06 DOI: 10.1134/S1063772924700616
A. S. Gusev, F. Kh. Sakhibov, A. V. Moiseev, V. S. Kostiuk, D. V. Oparin

Results of a study of physical parameters of stellar population in star formation regions in galaxies with signs of peculiarity NGC 3963 and NGC 7292 are presented. The study was carried out based on the analysis of photometric (UBVRI bands), H(alpha ) and spectroscopic data obtained by the authors, using evolutionary models of stellar population. Among 157 star formation regions identified in galaxies, the young stellar population mass estimates were obtained for 16 of them and the age estimates were obtained for 15. The age of star formation regions clearly correlates with the presence of emission in the H(alpha ) line: H II regions in the galaxies are younger than 6–8 Myr, and the regions without gas emission are older. The studied objects are included in the version 3 of our catalogue of photometric, physical and chemical parameters of star formation regions, which includes 1667 objects in 21 galaxies. Key aspects of the technique used to estimate the physical parameters and different relations between observational and physical parameters of the young stellar population in star formation regions are discussed.

本文介绍了对具有特殊征象的星系NGC 3963和NGC 7292中恒星形成区恒星群物理参数的研究结果。这项研究是在分析作者获得的测光(UBVRI波段)、H(alpha )和光谱数据的基础上,利用恒星群进化模型进行的。在星系中发现的157个恒星形成区中,有16个获得了年轻恒星群质量估计值,15个获得了年龄估计值。恒星形成区的年龄与H(α )线发射的存在明显相关:星系中的H II区域的年龄小于6-8 Myr,而没有气体发射的区域的年龄则更大。所研究的天体包括在我们的第三版恒星形成区光度、物理和化学参数目录中,该目录包括了21个星系中的1667个天体。本文讨论了用于估算恒星形成区年轻恒星群物理参数的关键技术,以及观测参数和物理参数之间的不同关系。
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引用次数: 0
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