Astrophysics and Space Science最新文献_第3页

Accelerating cosmological (f(R,L_{m},T)) gravity model along with bulk viscous fluid 加速宇宙学(f(R,L_{m},T))重力模型与大块粘性流体

IF 1.8 4区物理与天体物理

Astrophysics and Space Science Pub Date : 2024-12-06 DOI: 10.1007/s10509-024-04386-4

Shivani Sharma, Pratik V. Lepse, Mehul Raj Sharma

引用次数: 0

Micro-Raman and FTIR spectroscopic characterization of the first Turkish lunar regolith simulant 第一个土耳其月球风化模拟物的微拉曼和傅里叶红外光谱表征

IF 1.8 4区物理与天体物理

Astrophysics and Space Science Pub Date : 2024-12-06 DOI: 10.1007/s10509-024-04383-7

Ozan Unsalan, Y. Cengiz Toklu, Cisem Altunayar-Unsalan, Nurcan Calis Acikbas, Gokhan Acikbas, Ali Erdem Cercevik

{"title":"Micro-Raman and FTIR spectroscopic characterization of the first Turkish lunar regolith simulant","authors":"Ozan Unsalan, Y. Cengiz Toklu, Cisem Altunayar-Unsalan, Nurcan Calis Acikbas, Gokhan Acikbas, Ali Erdem Cercevik","doi":"10.1007/s10509-024-04383-7","DOIUrl":"10.1007/s10509-024-04383-7","url":null,"abstract":"<div><p>In this work, Infrared and Raman spectroscopic investigations on a new Turkish lunar regolith simulant (TBG-1), Chinese (own product), and Japanese simulants are presented for the first time. Our Raman spectroscopic investigation on TBG-1 simulant implies that it is mainly forsteritic olivine. Moreover, the Chinese sample produced by our group in Türkiye showed carbonate peaks at 712 cm<sup>−1</sup> and 878 cm<sup>−1</sup> in the IR spectra, which were attributed as calcium or sodium carbonates which could be a result of terrestrial weathering. Here, we propose that TBG-1 is close to the composition of lunar highland impact glass in terms of its (Mg, Ca)/Al<sub>2</sub>O<sub>3</sub> ratios. Our effort suggested that our recently produced Turkish simulant is similar to the Apollo 11 lunar soil sample in terms of its Al<sub>2</sub>O<sub>3</sub> and TiO<sub>2</sub> composition. Some of the samples we collected to simulate lunar regolith also show similarities to the Apollo 14 samples and JSC-1A simulant produced by NASA.</p></div>","PeriodicalId":8644,"journal":{"name":"Astrophysics and Space Science","volume":"369 12","pages":""},"PeriodicalIF":1.8,"publicationDate":"2024-12-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142789299","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

Determination of the porosity of Didim H3-5 meteorite using pycnometry and three-dimensional laser scanning Didim H3-5陨石孔隙度的三维激光扫描测定

IF 1.8 4区物理与天体物理

Astrophysics and Space Science Pub Date : 2024-12-03 DOI: 10.1007/s10509-024-04384-6

Cisem Altunayar-Unsalan, Ozan Unsalan

{"title":"Determination of the porosity of Didim H3-5 meteorite using pycnometry and three-dimensional laser scanning","authors":"Cisem Altunayar-Unsalan, Ozan Unsalan","doi":"10.1007/s10509-024-04384-6","DOIUrl":"10.1007/s10509-024-04384-6","url":null,"abstract":"<div><p>This study focuses on the porosity of the Didim H3−5 chondrite, providing insights into its physical and structural properties. Using the 3D laser scanning, we determined, that the bulk volume and the bulk density of Didim are 17.15 cm<sup>3</sup> and 3.16 g/cm<sup>3</sup>, respectively. Through helium pycnometry, we found thatthe grain volume and the grain density of Didim chondrite are 1.41 cm<sup>3</sup> and 3.64±0.001 g/cm<sup>3</sup>. We calculated that Didim has a porosity of 13.28±0.024%, which is consistent with similar chondrites, such as Fermo, but higher than Acfer 166 and Oum Dreyga. To establish robust links between meteorites and their possible parent bodies, further systematic and multi-analytical efforts, such as those used in this study, are requiredto accurately characterize meteorites’ porosities. Among the primary minerals in H3−5 chondrites, iron-nickel metals and iron-sulfides are also distributed heterogeneously in these ordinary chondrites. Using a combined approach of pycnometry and 3D laser scanning, we can further interpret shock processes from impacts on the parent body and weathering on Earth can be further interpreted in terms of their geologic history and the environmental conditions experienced by these chondrites both in parent bodies and after landing on Earth.</p></div>","PeriodicalId":8644,"journal":{"name":"Astrophysics and Space Science","volume":"369 12","pages":""},"PeriodicalIF":1.8,"publicationDate":"2024-12-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142761926","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

“Entangled” pairs of stars disrupted by the tidal action of Super Massive Black Hole 被超大质量黑洞潮汐作用扰乱的 "纠缠 "恒星对

IF 1.8 4区物理与天体物理

Astrophysics and Space Science Pub Date : 2024-11-28 DOI: 10.1007/s10509-024-04381-9

Galina N. Dryomova, Vladimir V. Dryomov, Alexander V. Tutukov

{"title":"“Entangled” pairs of stars disrupted by the tidal action of Super Massive Black Hole","authors":"Galina N. Dryomova, Vladimir V. Dryomov, Alexander V. Tutukov","doi":"10.1007/s10509-024-04381-9","DOIUrl":"10.1007/s10509-024-04381-9","url":null,"abstract":"<div><p>Based on modern observations on central S-stars by Gillessen et al. and hypervelocity stars (HVS) by Brown et al. the question is raised whether it is possible to establish the genetic duality of these stars? Could they belong in the past to a common parent binary star until it was captured and then gravitationally ruptured by a supermassive black hole (SMBH) within the Hills scenario? A cross-analysis of these observational data is carried out to obtain reliable evidence for the possible quantitative relationship of the stars under consideration. Three key issues are considered: 1. reconstruction of the trajectory of HVS ejection from the SMBH neighborhood by the method of backward integration in the Galaxy potential; 2. estimation of the dynamical stability of the S-star orbits by the <span>(N)</span>-body method — direct integration of their motion in the central field of the SMBH, taking into account the perturbing potential created by the S-cloud members; 3. checking of the coplanarity of orbits of a central S-star and an HVS; For nine HVSs it is possible to reconstruct the central trajectory of the ejection (at a distance less than a parsec from the SMBH) within the uncertainty of the observational proper motion values. For S2 star the timescale of the dynamical stability of its spatial orbital configuration in the S-cloud is evaluated as ∼ 100,000 years. This requires an additional comment on the criterion of the coplanarity of the orbits of paired S-HVS. The problem of identifying tidally decoupled components (S-HVS pairs) by the SMBH field poses a challenge to modern astrometric observations, and not only. This problem may provide an independent test of our knowledge of the distribution of baryon and dark matter, as well as the Galactic gravitational potential constructed on their basis, which is important in cosmological and evolutionary interpretations.</p></div>","PeriodicalId":8644,"journal":{"name":"Astrophysics and Space Science","volume":"369 11","pages":""},"PeriodicalIF":1.8,"publicationDate":"2024-11-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142736861","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

Analysis of anisotropic quark stellar objects in modified gravity 各向异性夸克恒星物体在修正引力下的分析

IF 1.8 4区物理与天体物理

Astrophysics and Space Science Pub Date : 2024-11-27 DOI: 10.1007/s10509-024-04379-3

M. Sharif, K. Hassan

引用次数: 0

Turbulence and chaotic structure generated by nonlinear kinetic Alfvén waves near magnetic null points in solar corona 日冕磁零点附近的非线性动能阿尔弗文波产生的湍流和混沌结构

IF 1.8 4区物理与天体物理

Astrophysics and Space Science Pub Date : 2024-11-21 DOI: 10.1007/s10509-024-04380-w

Garima Patel, R. Uma, R. P. Sharma

{"title":"Turbulence and chaotic structure generated by nonlinear kinetic Alfvén waves near magnetic null points in solar corona","authors":"Garima Patel, R. Uma, R. P. Sharma","doi":"10.1007/s10509-024-04380-w","DOIUrl":"10.1007/s10509-024-04380-w","url":null,"abstract":"<div><p>In the dynamic and complex environment of the solar corona, the interaction between kinetic Alfvén waves (KAWs) and magnetic null points might play a significant role in understanding various plasma processes. Recognizing the potential role of reconnection in coronal heating, our study aims to delve into how different types of null points affect KAW dynamics and ultimately contribute to heating. We investigate the behavior of nonlinear KAWs near the more frequently occurring components-null point with a mean magnetic field in the solar corona. The nonlinearity is attributed to the ponderomotive effects due to density perturbations. We used a three-dimensional model equation that describes the dynamics of KAWs in the presence of components-null point. Numerical methods are employed to solve the model equation for solar coronal parameters. Our simulations reveal that the nonlinear interaction between KAWs and magnetic null points can lead to the generation and amplification of turbulent and chaotic structures. This formation of localized structures, progressively exhibit more chaotic behavior over time, which may efficiently contribute to energy transfer. The power spectrum analysis of these turbulent structures shows a steeper spectrum with a pronounced cascade. Turbulence implies the presence of localized plasma heating, particle acceleration, and magnetic reconnection. These phenomena have significant implications for understanding the energy transport, particle dynamics, and magnetic topology in the solar corona. We also address nonlinearity’s role in promoting turbulence. This research offers insights into the dynamics of nonlinear KAWs near null points in the solar corona, suggesting their potential role in energy transfer and current sheet formation.</p></div>","PeriodicalId":8644,"journal":{"name":"Astrophysics and Space Science","volume":"369 11","pages":""},"PeriodicalIF":1.8,"publicationDate":"2024-11-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142679803","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

Images in axially symmetric gravitational lenses from elliptical sources: the elimination method 椭圆源轴对称引力透镜中的图像：消除法

IF 1.8 4区物理与天体物理

Astrophysics and Space Science Pub Date : 2024-11-19 DOI: 10.1007/s10509-024-04378-4

Albert Kotvytskiy, Štefan Parimucha

引用次数: 0

Following the tidal trail: a history of modeling the Magellanic Stream 追寻潮汐踪迹：麦哲伦海流建模史

IF 1.8 4区物理与天体物理

Astrophysics and Space Science Pub Date : 2024-11-18 DOI: 10.1007/s10509-024-04377-5

Scott Lucchini

引用次数: 0

Investigation of non-substorm Pi2 magnetic pulsation during solar flare event 太阳耀斑事件期间非次级风暴 Pi2 磁脉冲研究

IF 1.8 4区物理与天体物理

Astrophysics and Space Science Pub Date : 2024-11-18 DOI: 10.1007/s10509-024-04375-7

Islam Hawash, Essam Ghamry, Susan W. Samwel, Muhamed Yousef Omar, Hala El-Desoky

引用次数: 0

Resolved stellar populations as a key to unlocking the formation and evolution of galaxies 解析恒星群是开启星系形成和演化之门的钥匙

IF 1.8 4区物理与天体物理

Astrophysics and Space Science Pub Date : 2024-11-11 DOI: 10.1007/s10509-024-04376-6

Ata Sarajedini

引用次数: 0