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Three Arguables: Point Particle Singularity, Asymmetry in EM and Quantum Waves, and the Left Out Restricted Lorentz Gauge from U(1) 三个争论点点粒子奇异性、电磁波和量子波中的不对称性,以及来自 U(1) 的遗漏限制洛伦兹量规
IF 1.1 4区 物理与天体物理
Astronomy Reports Pub Date : 2024-02-25 DOI: 10.1134/S1063772923140196
Yousef Sobouti
{"title":"Three Arguables: Point Particle Singularity, Asymmetry in EM and Quantum Waves, and the Left Out Restricted Lorentz Gauge from U(1)","authors":"Yousef Sobouti","doi":"10.1134/S1063772923140196","DOIUrl":"10.1134/S1063772923140196","url":null,"abstract":"<p>We address three issues: (1) The point particle assumption inherent to non-quantum physics is singular and entails divergent fields and integrals. (2) In quantum physics electromagnetism (EM) plays an asymmetric roll. It acts on quantum wave functions (QW) but QW does not react back. We suggest to promote the one-sided action of EM on QW into a mutual action-reaction status. This enables QW to share its non-singular feature with EM and to remove the Coulomb singularity. (3) Quantum mechanics is U(1) symmetric. QW multiplied by an <i>arbitrary</i> phase factor and EM written in7 the same Lorentz gauge, leave both EM and QW invariant. The minimal coupling of QW to the EM 4-vector potential, <span>({{A}_{mu }})</span>, is a consequence of this arbitrary gauge. Symmetry under the restricted Lorentz gauge, is left out. We propose to enlarge U(1) to accommodate the restricted Lorentz gauge as well. This in turn invites in a coupling of QW to the derivatives of the vector potential, <span>({{partial }_{nu }}{{A}_{mu }})</span>, in addition to the minimal coupling. We find that (i) electron acquires a distributed charge, reminiscent of the QED-renormalized charge distributions; (ii) because of its spin, electron acquires a self induced magnetic moment with the same g-factor as in QED but without relying on QED.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":null,"pages":null},"PeriodicalIF":1.1,"publicationDate":"2024-02-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140884833","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
The Sun Made of Hot Gas 由高温气体组成的太阳
IF 1.1 4区 物理与天体物理
Astronomy Reports Pub Date : 2024-02-25 DOI: 10.1134/S1063772923130048
S. A. Yazev
{"title":"The Sun Made of Hot Gas","authors":"S. A. Yazev","doi":"10.1134/S1063772923130048","DOIUrl":"10.1134/S1063772923130048","url":null,"abstract":"<p>The paper presents an essay on the use of spectral analysis in the 19th–early 20th centuries to study the nature of the Sun.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":null,"pages":null},"PeriodicalIF":1.1,"publicationDate":"2024-02-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140884908","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
Simulations of Linear Polarization of Precessing AGN Jets at Parsec Scales 前冲 AGN 射流在等秒尺度上的线性极化模拟
IF 1.1 4区 物理与天体物理
Astronomy Reports Pub Date : 2024-02-25 DOI: 10.1134/S1063772923120119
R. V. Todorov, E. V. Kravchenko, I. N. Pashchenko, A. B. Pushkarev
{"title":"Simulations of Linear Polarization of Precessing AGN Jets at Parsec Scales","authors":"R. V. Todorov,&nbsp;E. V. Kravchenko,&nbsp;I. N. Pashchenko,&nbsp;A. B. Pushkarev","doi":"10.1134/S1063772923120119","DOIUrl":"10.1134/S1063772923120119","url":null,"abstract":"<p>The latest results of the most detailed analysis of multi-epoch polarization-sensitive observations of active galactic nuclei (AGN) jets at parsecs scales by very long baseline interferometry (VLBI) reveal several characteristic patterns of linear polarization distribution and its variability [1, 2]. Some of the observed profiles can be reproduced by a simple model of a jet threaded by a helical magnetic field. However, none of the models presented to date can explain the observed polarization profiles with an increase in its degree towards the edges of the jet, and accompanied by a “fountain” type electrical vector pattern and its high temporal variability in the center. Based on simulations of the VLBI observations of relativistic jets, we show here that the observed transverse linear polarization profiles can be naturally produced in a model of jets precessing on ten-years scales. In this scenario, due to the finite resolution of VLBI arrays, the initially strong polarization along the jet axis is blurred due to the superposition of regions whose polarization angle changes significantly when projected onto the sky plane. In our simulations, we qualitatively reproduce the distribution of the electric vector and its variability, though the polarization distribution images are characterized by a bright spine due to weak suppression of polarized emission, which is poorly consistent with observations of quasars. More effective depolarization can be obtained in models with the suppressed emission of the jet spine.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":null,"pages":null},"PeriodicalIF":1.1,"publicationDate":"2024-02-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140884918","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
Exploring Massive Neutron Stars Towards the Mass Gap: Constraining the High Density Nuclear Equation of State 探索大质量中子星的质量差距:约束高密度核状态方程
IF 1.1 4区 物理与天体物理
Astronomy Reports Pub Date : 2024-02-25 DOI: 10.1134/S1063772923140214
Zenia Zuraiq, Banibrata Mukhopadhyay, Fridolin Weber
{"title":"Exploring Massive Neutron Stars Towards the Mass Gap: Constraining the High Density Nuclear Equation of State","authors":"Zenia Zuraiq,&nbsp;Banibrata Mukhopadhyay,&nbsp;Fridolin Weber","doi":"10.1134/S1063772923140214","DOIUrl":"10.1134/S1063772923140214","url":null,"abstract":"<p>Due to the high-density nuclear matter equation of state (EOS) being as yet unknown, neutron stars (NSs) do not have a confirmed limiting “Chandrasekhar” type maximum mass. However, observations of NSs (PSR J1614-2230, PSR J0348+0432, PSR J0740+6620, PSR J0952–0607) indicate that the NS’s limiting mass, if there is any, could be well over <span>(2{{M}_{ odot }})</span>. On the other hand, there seems to be an observational mass gap (of around <span>(2.5{-} 5{{M}_{ odot }})</span>) between the lightest black hole and the heaviest NS. Therefore, the “massive NSs” are prime candidates to fill that gap. Several NS EOSs have been proposed using both microscopic and phenomenological approaches. In this project, we look at a class of phenomenological nuclear matter EOSs—relativistic mean field models—and see what kind of NS is formed from them. We compute the maximum mass supported by each model EOS to observe if the mass of the NS is indeed in the “massive” NS (<span>( &gt; {kern 1pt} 2{{M}_{ odot }})</span>) regime. We also observe the effects of including exotic particles (hyperons, Δ<i>s</i>) in the NS EOS and how that affects the NS mass. However, only by introducing the magnetic field, i.e. for magnetized anisotropic NSs, we find the mass exceeding <span>(2.5{{M}_{ odot }})</span>. Using tidal deformability constraints from gravitational wave observations, we place a further check on how physical the EOS and NSs are.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":null,"pages":null},"PeriodicalIF":1.1,"publicationDate":"2024-02-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140885115","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
The Sun: Methodology, Theory, Practice 太阳方法、理论、实践
IF 1.1 4区 物理与天体物理
Astronomy Reports Pub Date : 2024-02-25 DOI: 10.1134/S1063772923130073
S. A. Yazev
{"title":"The Sun: Methodology, Theory, Practice","authors":"S. A. Yazev","doi":"10.1134/S1063772923130073","DOIUrl":"10.1134/S1063772923130073","url":null,"abstract":"<p>The paper provides a general overview of the current state of solar research.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":null,"pages":null},"PeriodicalIF":1.1,"publicationDate":"2024-02-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139978693","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
The Sun: Dark and Cold 太阳黑暗与寒冷
IF 1.1 4区 物理与天体物理
Astronomy Reports Pub Date : 2024-02-25 DOI: 10.1134/S1063772923130036
S. A. Yazev
{"title":"The Sun: Dark and Cold","authors":"S. A. Yazev","doi":"10.1134/S1063772923130036","DOIUrl":"10.1134/S1063772923130036","url":null,"abstract":"<p>This paper makes an attempt to describe the ideas about the Sun that dominated Europe in the 17th–19th centuries.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":null,"pages":null},"PeriodicalIF":1.1,"publicationDate":"2024-02-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139978701","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
Plausible Detection of Rotating Magnetized Neutron Stars by Their Continious Gravitational Waves 通过连续引力波探测旋转磁化中子星的可能性
IF 1.1 4区 物理与天体物理
Astronomy Reports Pub Date : 2024-02-25 DOI: 10.1134/S1063772923140056
Mayusree Das, Banibrata Mukhopadhyay
{"title":"Plausible Detection of Rotating Magnetized Neutron Stars by Their Continious Gravitational Waves","authors":"Mayusree Das,&nbsp;Banibrata Mukhopadhyay","doi":"10.1134/S1063772923140056","DOIUrl":"10.1134/S1063772923140056","url":null,"abstract":"<p>In the past decades, several neutron stars (NSs), particularly pulsars, with mass <span>(M &gt; 2{{M}_{ odot }})</span>, have been observed. Hence, there is a generic question of the origin of massive compact objects. Here we explore the existence of massive, magnetized, rotating NSs by solving axisymmetric stationary stellar equilibria in general relativity using the Einstein equation solver for stellar structure <i>XNS</i> code. Such rotating NSs with magnetic field and rotation axes misaligned, hence with non-zero obliquity angle, can emit continuous gravitational waves (GW). We discuss the decay of the magnetic field due to Ohmic, Hall and Ambipolar diffusion, and the decay of angular velocity, and obliquity angle with time due to angular momentum extraction by GW and dipole radiation, which determine the timescales related to the GW emission. Further, in the Alfvén timescale, a differentially rotating, massive proto-NS rapidly settles into a uniformly rotating, less massive NS due to magnetic braking and viscosity. These explorations suggest that detecting massive NSs is challenging and sets a timescale for detection. We calculate the signal-to-noise ratio of GW emission, which confirms that any detector cannot detect them immediately, but detectable by Einstein Telescope and Cosmic Explorer over months of integration time, leading to direct detection of NSs.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":null,"pages":null},"PeriodicalIF":1.1,"publicationDate":"2024-02-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140884759","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
Magnetized Advective Accretion Disks and Jets: Harmpi Simulation 磁化对流吸积盘和喷流:Harmpi 仿真
IF 1.1 4区 物理与天体物理
Astronomy Reports Pub Date : 2024-02-25 DOI: 10.1134/S1063772923140172
Rohan Raha, Banibrata Mukhopadhyay, Koushik Chatterjee, S. M. Gopika
{"title":"Magnetized Advective Accretion Disks and Jets: Harmpi Simulation","authors":"Rohan Raha,&nbsp;Banibrata Mukhopadhyay,&nbsp;Koushik Chatterjee,&nbsp;S. M. Gopika","doi":"10.1134/S1063772923140172","DOIUrl":"10.1134/S1063772923140172","url":null,"abstract":"<p>An optically thin advective accretion disk appears to be indispensable to explain hard-state of black hole sources. Any transport of matter therein is assumed to be led by (modified) <span>(alpha )</span>-viscosity when the magnetic field is weak. We explore how large scale stronger magnetic field helps in transporting angular momentum in disk and outflow/jet, depending on the field geometry and plasma-<span>(beta )</span> parameter, basically by underlying magnetic shear over <span>(alpha )</span>-viscosity. Interestingly, while above a critical accretion rate the accretion disk turns out to be thermally unstable, in the presence of stronger magnetic fields the disk regains its stability. In the present work, we establish this by numerical simulation based on HARMPI, while the underlying theory was established by one of us earlier. This magnetically arrested advective accretion disk (MA-AAF) in the optically thin regime has far reaching implications including the explanation of ultra-luminous X-ray sources.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":null,"pages":null},"PeriodicalIF":1.1,"publicationDate":"2024-02-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140884997","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
Solar Cycle Structure and Structure of Activity Cycles at Late-Type Stars 太阳周期结构和晚型恒星活动周期结构
IF 1.1 4区 物理与天体物理
Astronomy Reports Pub Date : 2024-02-25 DOI: 10.1134/S1063772923120065
V. N. Obridko, D. D. Sokoloff, M. M. Katsova
{"title":"Solar Cycle Structure and Structure of Activity Cycles at Late-Type Stars","authors":"V. N. Obridko,&nbsp;D. D. Sokoloff,&nbsp;M. M. Katsova","doi":"10.1134/S1063772923120065","DOIUrl":"10.1134/S1063772923120065","url":null,"abstract":"<p>It is shown that a description of the solar cycle using the odd zonal harmonic of the solar magnetic field expands our capabilities in two important areas of solar research: first, in improving and expanding the forecast to the near future of evolution of the cyclic solar activity and, second, in developing a program for monitoring the spectrophotometric characteristics of radiation of solar-like stars, aimed at obtaining new information about their magnetic fields.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":null,"pages":null},"PeriodicalIF":1.1,"publicationDate":"2024-02-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139978386","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
Spectral Survey of the Star Formation Region DR21OH in the 4-mm Wavelength Range 4 毫米波长范围内恒星形成区 DR21OH 的光谱巡天
IF 1.1 4区 物理与天体物理
Astronomy Reports Pub Date : 2024-02-25 DOI: 10.1134/S106377292312003X
S. V. Kalenskii, E. A. Mikheeva
{"title":"Spectral Survey of the Star Formation Region DR21OH in the 4-mm Wavelength Range","authors":"S. V. Kalenskii,&nbsp;E. A. Mikheeva","doi":"10.1134/S106377292312003X","DOIUrl":"10.1134/S106377292312003X","url":null,"abstract":"<p>The results of a spectral survey of the region of massive star formation DR21OH in the 4-mm wavelength range are presented. Sixty-nine molecules and their isotopologues have been detected, ranging from simple diatomic or triatomic species such as SO, SiO and CCH, to complex organic molecules such as CH<sub>3</sub>OCHO or CH<sub>3</sub>OCH<sub>3</sub>. The obtained results qualitatively repeat the results of the survey of the same source at 3 mm. The inventories of molecules found at 3 and 4 mm overlap to a great extent. However, at 4 mm we found a number of species that have no allowed transitions in the 3-mm wavelength range, e.g., DCN, DNC, or SO<sup>+</sup>. The bulk of the molecules detected at 4 mm are those that are common for dense cores, e.g., HC<sub>3</sub>N or CH<sub>3</sub>CCH, but some of the detected species are typical for hot cores. The latter include complex organic molecules CH<sub>3</sub>OCHO, CH<sub>3</sub>CH<sub>2</sub>OH, CH<sub>3</sub>OCH<sub>3</sub>, etc. However, the detected emission of these molecules probably arises in a gas heated to 30 K only. Nine molecules, including complex species CH<sub>3</sub>C<sub>3</sub>N, CH<sub>3</sub>CH<sub>2</sub>CN, CH<sub>3</sub>COCH<sub>3</sub>, were found by spectral line stacking. This demonstrates the prospects of the method in the study of molecular clouds.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":null,"pages":null},"PeriodicalIF":1.1,"publicationDate":"2024-02-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139978671","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
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