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Newly found Mayan records of astronomical phenomena in Dresden Codex 德累斯顿手抄本中新发现的玛雅天文现象记录
IF 0.5 4区 物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-01-01 DOI: 10.2298/saj2306029v
J. Vondrák, V. Böhm, B. Böhm
The rich culture of old Maya gave birth to a very complicated and complex calendar; they also recorded important historical events and many significant astronomical phenomena. The main source of information is represented by Dresden Codex (DC), one of the four preserved Mayan hieroglyphic literal legacies. DC roughly covers the interval between 280 and 1325 AD. The old problem of precise Mayan dating with respect to our calendar is traditionally called correlation; it expresses the difference in days between the Long Count of the Mayan calendar and the Julian Date, used in presentday astronomy. There exist more than fifty published correlations that differ one from the other by as much as several centuries. Historians mostly accept the so called Goodman-Mart?nez-Thompson (GMT) value of 584 283 days, which is based mostly on historical events extracted from the sources of a postclassical period of Mayan history. On the contrary, brothers B?hm used precisely dated astronomical data from classical period to derive the B?hm correlation (BB) of 622 261 days. Unlike the GMT correlation it is in excellent agreement with the astronomical phenomena recorded in DC. Since then we published several papers supporting the validity of BB correlation and its advantage over GMT in the classical period of Mayan history. To this end, we used more records of astronomical phenomena discovered in DC. This study describes six records of planetary conjunctions that we found recently on p. 37 of DC that concern planets Mercury, Venus, Mars, Jupiter, and Saturn. All of these records coincide with the real occurrences of these phenomena within several days, if BB correlation is applied.
古老玛雅丰富的文化产生了非常复杂的历法;他们还记录了重要的历史事件和许多重要的天文现象。信息的主要来源是德累斯顿抄本(DC),这是四个保存完好的玛雅象形文字遗产之一。DC大致涵盖了公元280年到1325年之间的时间间隔。根据我们的历法精确测定玛雅人的年代的老问题传统上被称为相关性;它表示了玛雅历法的长历法和现代天文学中使用的儒略历之间的天数差异。有超过50种已发表的相关性,它们之间的差异可达几个世纪之久。历史学家大多接受所谓的Goodman-Mart?nez-Thompson(格林尼治标准时间)的值为584 283天,这主要是基于从玛雅历史的后古典时期的资料中提取的历史事件。相反,B兄弟?他利用古典时期精确的天文数据推导出了B?hm相关性(BB)为622 261天。与格林尼治标准时间的相关性不同,它与DC记录的天文现象非常吻合。从那时起,我们发表了几篇论文,支持BB相关性的有效性,以及它在玛雅历史的古典时期相对于GMT的优势。为此,我们使用了更多在华盛顿发现的天文现象的记录。这项研究描述了我们最近在《华盛顿邮报》第37页发现的关于水星、金星、火星、木星和土星的六个行星连接的记录。如果应用BB相关性,所有这些记录都与这些现象在几天内的实际发生一致。
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引用次数: 0
A search for fast radio bursts associated with gamma-ray bursts using the YNAO 40-m radio telescope 使用YNAO 40米射电望远镜搜索与伽马射线暴相关的快速射电暴
IF 0.5 4区 物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-01-01 DOI: 10.2298/saj2306039z
Y.F. Zhang, Z. Wen, N. Wang, L. Hao, J. Yuan, R. Yuen, X. Duan, Z. Wang
We report on the search results of Fast Radio Bursts (FRBs) from three Gamma- ray Bursts (GRBs) at 2256 MHz using the 40-m radio telescope located at the YunNan Astronomical Observatory (YNAO). The search for signals was triggered by the Burst Alert Telescope (BAT) on- board the Swift satellite. Radio single pulses are searched in the data over a large range of dispersion measure from 0 to 5000 pc/cm3 in step of 50 pc/cm3. No FRB-like emission from the prompt phase of GRBs are detected with significance > 5?. If there are FRBs related to the GRBs, we set an upper limit on the ux density of radio pulses of 2.5 Jy for GRB140512A and 8.0 Jy for GRBs 140629A and 140703A with the sensitivity of the telescope. A statistical analysis of the GRB data reveals that the events detected above 5? are consistent with the thermal noise uctuations.
本文报道了云南天文台40米射电望远镜在2256 MHz波段对3个伽玛射线暴(GRBs)的快速射电暴(FRBs)的搜索结果。对信号的搜索是由雨燕卫星上的突发警报望远镜(BAT)触发的。在0 ~ 5000pc /cm3的大色散测量范围内,以50pc /cm3的步进搜索射电单脉冲数据。在grb的提示阶段没有检测到类似frb的辐射,具有显著性bbbb50 ?如果存在与grb相关的快速射电暴,我们根据望远镜的灵敏度将GRB140512A的射电脉冲ux密度上限设定为2.5 Jy, grb140629a和140703A的射电脉冲ux密度上限设定为8.0 Jy。对GRB数据的统计分析表明,探测到的事件高于5?与热噪声波动一致。
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引用次数: 0
The influence of metallicity on helium and CO core masses in massive stars 金属丰度对大质量恒星中氦和CO核心质量的影响
IF 0.5 4区 物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-01-01 DOI: 10.2298/saj2306001p
Jelena Petrović
We present the results of 58 detailed evolutionary models of massive single stars and close binary systems with the Solar and Small Magellanic Cloud (SMC) metallicity computed with the MESA (Modules for Experiments in Stellar Astrophysics) numerical code. Helium core masses of single stars (30 M? - 75 M?) with metallicities of 0.02 and 0.0021 are in the range of 9.26 M? - 29.56 M? and 11.62 M? - 33.96 M?, respectively. Their carbon-oxygen (CO) core masses are between 5.44 M? and 25.04 M? vs. 8.23 M? and 28.38 M? for the Solar vs. SMC metallicity, accounting for an average difference of 25%. To investigate the influence of metallicity on helium and carbon-oxygen core masses in massive close Case A binary systems, detailed evolutionary models of binary systems in the mass range of 30 M? to 40 M? are calculated. The initial orbital period is set to 3 days and the accretion efficiency to 10%. The helium core mass range for primary stars with lower metallicity is 10.61 - 16.21 M? vs. 7.94 - 11.69 M? for z = 0.02. The resulting CO core masses of primary stars for the SMC metallicity are on average about 50% larger than for the Solar metallicity, so the effect is more prominent than in the case of single stars. The black hole formation limit for primary stars with the SMC metallicity is under 30 M?. While the least massive primary stars with Solar metallicity end up as neutron stars, all primary stars with the SMC metallicity and all secondary stars complete their evolution as black holes. The double compact objects resulting from the presented models are of two types: mixed neutron star-black hole systems (4 models) and double black holes (18 models). We also derive the relation between the final helium core mass and the carbon-oxygen core mass and show that it does not depend on metallicity. We confirm the CO/helium core mass ratio to be larger in binary systems than for single stars.
用MESA (Modules for Experiments in Stellar Astrophysics)数值代码计算了58个具有太阳和小麦哲伦云(SMC)金属丰度的大质量单星和紧密双星系统的详细演化模型的结果。单星氦核质量(30m ?金属丰度为0.02和0.0021的金属在9.26 M?- 29.56米?11点62分?- 33.96米?,分别。它们的碳氧(CO)核心质量在5.44 M?25分04秒?vs. 8.23 M?28.38 M?对于Solar与SMC的金属丰度,占比平均相差25%。为了研究金属丰度对大质量紧密的Case A双星系统中氦和碳氧核心质量的影响,详细建立了质量范围为30 M?到40米?计算。初始轨道周期设置为3天,吸积效率设置为10%。金属丰度较低的主星的氦核质量范围为10.61 ~ 16.21 M?vs. 7.94 - 11.69 ?对于z = 0.02。SMC金属丰度的主恒星的CO核心质量比太阳金属丰度的主恒星的CO核心质量平均大50%左右,因此这种效应比单星的情况更为突出。具有SMC金属丰度的主星的黑洞形成极限在30 μ M以下。而质量最小的具有太阳金属丰度的主星最终成为中子星,所有具有SMC金属丰度的主星和所有的副星都完成了黑洞的演化。由这些模型得到的双致密天体有两种类型:混合中子星-黑洞系统(4个模型)和双黑洞(18个模型)。我们还推导了最终氦核质量与碳氧核质量之间的关系,并表明它不依赖于金属丰度。我们确认双星系统的CO/氦核心质量比大于单星。
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引用次数: 0
A potential survival strategy during the late heavy bombardment 在猛烈轰炸后期可能的生存策略
IF 0.5 4区 物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-01-01 DOI: 10.2298/saj2306009h
Hegner von
The Late Heavy Bombardment (LHB) represents a period of time in which an increased number of impactors collided with the Earth. While there were continuous collisions of impactors globally, these would be perceived by populations of life as locally infrequent, as they occurred at different times and locations across the planet. These impactions presented a severe and unpredictable environmental pressure on life, as they could at any moment destroy organisms and their local habitats. However, such an environment could potentially lead to the selection of a particular evolutionary strategy, bet hedging, which is an adaptation to unpredictability itself. Thus, a model for analysing this has been put forward in the form of a system of rings arising from an impact-consisting of the inner primary and outer secondary rings, which demonstrates the dynamic interplay between the external pressure from impact dynamics and life's evolutionary response towards it. The model demonstrates that there is a longer relaxed period where organisms thrive and a short violent period where they must survive three violent events and respond to a potentially different environment. This evolutionary strategy consistently results in a higher number of surviving organisms compared to other evolutionary strategies; thus, it may have played a crucial role in life's endurance through the LHB-an insight relevant to astrobiology.
晚期重轰击(LHB)代表了一段时间,在这段时间里,越来越多的撞击物与地球相撞。虽然全球范围内不断有撞击物发生碰撞,但由于它们发生在地球上不同的时间和地点,因此这些碰撞在当地的生命种群中并不常见。这些撞击给生命带来了严重的、不可预测的环境压力,因为它们随时可能破坏生物及其当地的栖息地。然而,这样的环境可能会导致选择一种特定的进化策略,即下注对冲,这是对不可预测性本身的一种适应。因此,我们提出了一种分析这一现象的模型,其形式是由撞击产生的环系统——由内初级环和外次级环组成,它展示了撞击动力学产生的外部压力与生命对它的进化反应之间的动态相互作用。该模型表明,有一个较长的放松期,生物体在此期间茁壮成长,而在一个短暂的暴力期,它们必须在三次暴力事件中生存下来,并对可能不同的环境做出反应。与其他进化策略相比,这种进化策略始终导致更高数量的存活生物体;因此,它可能在通过lhb的生命耐力中发挥了至关重要的作用——这是与天体生物学相关的见解。
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引用次数: 0
Astronomical observatory site selection using fuzzy AHP and BWM methods 基于模糊层次分析法和BWM方法的天文台选址
4区 物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-01-01 DOI: 10.2298/saj230530001y
A. Yılmaz
Establishing an observatory often involves complex decisions, such as choosing a site based on multiple conicting criteria. In this study, we develop a multi-criteria decision analysis process by combining Geographic Information System (GIS) analysis with the (MCDA) Multi-Criteria Decision Analysis and use this process to determine the most suitable sites for the construction of an observatory in the Malatya urban area. GIS was used to calculate, classify, and analyze criteria, while FAHP (Fuzzy Analytic Hierarchy Processes, Buckley's method) and BWM(MCDA type Best-Worst Method) methods were used to weight the decision criteria and determine their effects on alternative sites. While the Cloud Cover criterion in the BWM method was the most important criterion with 28%, the most important criterion for the FAHP method had a comparable value of 27.8%. Meteorological criteria were the most important criteria group with values of 50.4% according to the FAHP method and 44.6% according to the BWM method. The study is based on meteorological, geographic, and anthropogenic datasets, suggesting the most appropriate sites for the astronomical observatory within the boundaries of the study area. The proposed sites are the result of site selection, which is the first phase of site selection for astronomical observatories. This site selection is important to limit the number of field alternatives. It is necessary to conduct field tests among the proposed areas and select the final site according to the results. The successful use of GIS and more than one MCDA method will pave the way for the development of various methods for astronomical observatory site determination.
建立观测站通常涉及复杂的决策,例如根据多种相互矛盾的标准选择地点。在本研究中,我们通过将地理信息系统(GIS)分析与(MCDA)多标准决策分析相结合,开发了一种多标准决策分析过程,并使用该过程确定在马拉提亚市区建设天文台的最合适地点。GIS用于计算、分类和分析标准,而FAHP(模糊层次分析法,巴克利方法)和BWM(MCDA类型最佳最差方法)方法用于权衡决策标准并确定其对备选地点的影响。而BWM方法中的云覆盖标准是最重要的标准,占28%,FAHP方法中最重要的标准具有27.8%的可比值。气象判据是最重要的判据组,FAHP法占50.4%,BWM法占44.6%。该研究基于气象、地理和人为数据集,建议在研究区域范围内最合适的天文台地点。选址是天文台选址的第一阶段,是选址的结果。这种选址对于限制备选场地的数量非常重要。有必要在建议区域之间进行实地试验,并根据结果选择最终地点。地理信息系统和多种MCDA方法的成功应用将为发展各种天文台选址方法铺平道路。
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引用次数: 0
Stellar coronal mass ejections 恒星日冕物质抛射
IF 0.5 4区 物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS Pub Date : 2022-12-18 DOI: 10.2298/SAJ2205001L
M. Leitzinger, P. Odert
Stellar coronal mass ejections (CMEs) are a growing research field, especially during the past decade. The large number of so far detected exoplanets raises the open question for the CME activity of stars, as CMEs may strongly affect exoplanetary atmospheres. In addition, as CMEs contribute to stellar mass and angular momentum loss and are therefore relevant for stellar evolution, there is a need for a better characterization of this phenomenon. In this article we review the different methodologies used up to now to attempt the detection of stellar CMEs. We discuss the limitations of the different methodologies and conclude with possible future perspectives of this research field.
恒星日冕物质抛射(CMEs)是一个新兴的研究领域,特别是在过去的十年中。迄今为止探测到的大量系外行星提出了恒星CME活动的开放问题,因为CME可能强烈影响系外行星的大气。此外,由于日冕物质抛射导致恒星质量和角动量损失,因此与恒星演化有关,因此需要更好地描述这一现象。在这篇文章中,我们回顾了迄今为止用来尝试探测恒星cme的不同方法。我们讨论了不同方法的局限性,并总结了该研究领域可能的未来前景。
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引用次数: 0
Dark matter mass loss in galaxy flybys: dependence on impact parameter 星系飞掠中的暗物质质量损失:对撞击参数的依赖
IF 0.5 4区 物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS Pub Date : 2022-03-16 DOI: 10.2298/SAJ210915001M
A. Mitravsinovi'c
Galaxy flybys, interactions where two independent halos inter-penetrate but detach at a later time and do not merge, occur frequently at lower redshifts. These interactions can significantly impact the evolution of individual galaxies from mass loss and shape transformation to the emergence of tidal features and the formation of morphological disc structures. The main focus of this paper is on the dark matter mass loss of the secondary, intruder galaxy, with the goal of determining a functional relationship between impact parameter and dark matter mass loss. Series of N-body simulations of typical galaxy flybys (10:1 mass ratio) with differing impact parameters show that dark matter halo leftover mass of intruder galaxy follows logarithmic growth law with impact parameter, regardless of the way total halo mass is estimated. Lost mass then, clearly, follows exponential decay law. Stellar component stretches faster as impact parameter decreases, following exponential decay law with impact parameter. Functional dependence on impact parameter in all cases seems universal, but fitting parameters are likely sensitive to interaction parameters and initial conditions (e.g. mass ratio of interacting galaxies, the initial relative velocity of intruder galaxy, interaction duration). While typical flybys, investigated here, could not be the sole culprit behind the formation of ultra-diffuse or dark matter deficient galaxies, their effects should not be disregarded as they can at least contribute substantially. Rare, atypical and stronger flybys are worth exploring further.
星系飞掠,两个独立的光晕相互渗透,但在稍后的时间分离而不合并的相互作用,经常发生在较低的红移。这些相互作用可以显著影响单个星系的演化,从质量损失和形状转变到潮汐特征的出现和形态盘结构的形成。本文主要关注次级侵入星系的暗物质质量损失,目的是确定撞击参数与暗物质质量损失之间的函数关系。一系列不同撞击参数下典型星系飞掠(质量比为10:1)的n体模拟表明,无论采用何种方式估算总晕质量,入侵星系的暗物质晕剩余质量都遵循随撞击参数的对数增长规律。显然,质量损失遵循指数衰减定律。随着冲击参数的减小,恒星成分的拉伸速度加快,且随冲击参数的增大呈指数衰减规律。在所有情况下,对冲击参数的函数依赖似乎是普遍的,但拟合参数可能对相互作用参数和初始条件(如相互作用星系的质量比、入侵星系的初始相对速度、相互作用持续时间)敏感。虽然这里研究的典型飞掠并不是形成超漫射星系或缺乏暗物质星系的唯一罪魁祸首,但它们的影响不应被忽视,因为它们至少可以做出实质性的贡献。罕见的,非典型的和更强的飞掠值得进一步探索。
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引用次数: 0
Mercury and orbfit packages for numerical integration of planetary systems: implementation of the yarkovsky and yorp effects 行星系统数值集成的水星和轨道包:亚尔科夫斯基和约普效应的实现
IF 0.5 4区 物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS Pub Date : 2022-02-28 DOI: 10.2298/SAJ2204051F
M. Fenucci, B. Novakovi'c
For studies of the long-term evolution of small Solar System objects, it is fundamental to add the Yarkovsky and Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effects in the dynamical model. Still, implementations of these effects in publicly available N-body codes is either lacking, or the effects are implemented using significantly simplified models. In this paper, we present an implementation of the coupled Yarkovsky/YORP effects in the mercury and orbfit N-body codes. Along with these two effects, we also included the effects of non-destructive collisions and rotationally induced breakups to model the asteroid spin state properly. Given the stochastic nature of many incorporated effects, the software is suitable for statistical dynamical studies. Here we primarily explained the scientific aspect of the implementation, while technical details will be made freely available along with the source codes.
对于研究太阳系小天体的长期演化,在动力学模型中加入Yarkovsky和Yarkovsky- o 'Keefe-Radzievskii-Paddack (YORP)效应是至关重要的。然而,在公开可用的n体代码中实现这些效果要么是缺乏的,要么是使用非常简化的模型实现的。在本文中,我们提出了一个在汞和轨道n体代码中耦合Yarkovsky/YORP效应的实现。除了这两种影响,我们还包括了非破坏性碰撞和旋转引起的分裂的影响,以正确地模拟小行星的自旋状态。鉴于许多合并效应的随机性质,该软件适用于统计动力学研究。在这里,我们主要解释了实现的科学方面,而技术细节将与源代码一起免费提供。
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引用次数: 1
The influence of initial orbital period on helium and carbon-oxygen core masses in massive case a binary systems with low accretion efficiency 低吸积效率双星大质量情况下初始轨道周期对氦和碳氧核心质量的影响
IF 0.5 4区 物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS Pub Date : 2022-01-01 DOI: 10.2298/saj2205045p
Jelena Petrović
The evolutionary models of 33 massive Case A binary systems in mass range from 30M? to 40M? with initial orbital periods of 3, 4 and 5 days, accretion efficiency of 10% and at the solar metallicity are presented. The models are obtained with the MESA (Modules for Experiments in Stellar Astrophysics) numerical code. The evolution is followed from a double O-type star, through Case A and Case mass transfer, to the formation of a carbon-oxygen (CO) core in the primary. The evolution of the secondary star in each binary system is further modeled with the same numerical code in an approximation of a single star, also to the formation of a carbon-oxygen core. The resulting helium core masses are in the range of 7.94M? - 13.19M? and 12.30M? and 19.12M? for primary and secondary stars, respectively. The carbon-oxygen core masses are between 5.26M? and 10M? for primaries and between 8.96M? and 15.32M? for secondaries. A clear influence of the initial orbital period on the resulting helium and CO core masses is demonstrated: primary stars in binary systems with initial orbital periods of 3, 4 and 5 days have on average about 15%, 8% and 2.5% smaller CO cores than single stars with the same initial masses. On the other hand, it was found that the correlation between the CO and helium core mass does not depend on the initial orbital period and can be approximated with the same linear fit for all binary systems. The CO/helium core mass ratio is found to be larger in binary systems than for single stars. It is also shown that the black hole formation limit for primary stars depends on the initial orbit and is between 33M? - 34M?, 32M? - 33M? and 30M? - 31M?, for the initial orbital periods of 3, 4 and 5 days, respectively. The resulting double compact objects are of two types: mixed neutron star - black hole systems (6 models) and double black holes (27 models). The resulting black hole masses are estimated to be in the range of 5M? to 17M?.
33个质量范围从30M?40米?在初始轨道周期为3、4和5天时,吸积效率为10%,并达到太阳金属丰度。这些模型是用MESA (Modules for Experiments in Stellar Astrophysics)数值代码得到的。从双o型恒星开始,经过情况a和情况传质,直到在初级恒星中形成碳氧(CO)核心。在每个双星系统中,副星的演化进一步用相同的数值代码模拟,近似于单星,也模拟碳氧核心的形成。由此产生的氦核质量在7.94M?——13.19米?和12.30米?和19.12米?分别是主星和副星。碳氧核心质量在5.26M?和10米?在896万美元之间?和15.32米?二期梅毒疹。初始轨道周期对氦和CO核心质量的明显影响得到了证明:在初始轨道周期为3,4和5天的双星系统中,主星的CO核心平均比具有相同初始质量的单星小15%,8%和2.5%。另一方面,我们发现CO和氦核质量之间的相关性不依赖于初始轨道周期,并且可以用相同的线性拟合近似于所有双星系统。双星系统的CO/氦核心质量比大于单星。还表明,主星的黑洞形成极限取决于初始轨道,在33M?- 34米?32米?- 33米?30米?- 31米?初始轨道周期分别为3、4和5天。得到的双致密天体有两种类型:中子星-黑洞混合系统(6种模型)和双黑洞(27种模型)。由此产生的黑洞质量估计在5M?17 m ?。
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引用次数: 0
Dependence of stellar substructures in M31 type galaxy on satellite morphology in galaxy mergers M31型星系中恒星亚结构与星系合并中卫星形态的关系
IF 0.5 4区 物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS Pub Date : 2022-01-01 DOI: 10.2298/saj220704004m
S. Milosevic
Stellar streams and shells are observed in halos of spiral galaxies. In this paper, we investigated the formation of these structures due to mergers between the host spiral galaxy and its dwarf satellite galaxies. We run the N-body simulations with two morphological models of a dwarf galaxy for different initial positions. One model is a spheroidal dwarf, dSph, and the other is a dwarf with a disk. We found that both models form stellar shells and streams and, in the case of the progenitor with a disk, streams are more prominent. After several pericentric passages, there is a possibility of formation of several streams. The remnant of the progenitor is more likely to disrupt later into the merger in the case of spiral progenitor than in the case of dSph.
在螺旋星系的光晕中可以观察到恒星流和恒星壳。在本文中,我们研究了这些结构的形成是由于宿主螺旋星系和它的矮卫星星系之间的合并。我们用两种矮星系形态模型对不同初始位置的n体进行了模拟。一种是球状矮星(dSph),另一种是带圆盘的矮星。我们发现,这两种模型都形成了恒星壳和恒星流,在有圆盘的祖星系中,恒星流更为突出。经过几条绕心通道后,有可能形成几条溪流。在螺旋祖星系中,祖星系的残余物比在dSph中更有可能在后来的合并中被破坏。
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引用次数: 0
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Serbian Astronomical Journal
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