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Quantum Locking and the Meissner Effect Lead to the Origin and Stability of the Saturn Rings System 量子锁定和迈斯纳效应导致土星环系统的起源和稳定性
International Journal of Astronomy and Astrophysics Pub Date : 2018-02-08 DOI: 10.4236/IJAA.2018.81008
V. Tchernyi, A. Y. Pospelov
{"title":"Quantum Locking and the Meissner Effect Lead to the Origin and Stability of the Saturn Rings System","authors":"V. Tchernyi, A. Y. Pospelov","doi":"10.4236/IJAA.2018.81008","DOIUrl":"https://doi.org/10.4236/IJAA.2018.81008","url":null,"abstract":"It is demonstrated how superconducting iced particles of the protoplanetary cloud of Saturn are coming to magnetic equator plane and create the stable enough rings disk. There are two steps. First, after appearance of the Saturn magnetic field due to Meissner phenomenon, all particles orbits are moving to the magnetic equator plane. Finally they become distributed as rings and gaps like iron particles around magnet on laboratory table. And they are separated from each other by the magnetic field expelled from them. It takes up to few tens of thousands years with ten meters rings disk thickness. Second, because of quantum locking all particles become to be locked within magnetic well at the magnetic equator plane due to Abrikosov vortex for superconductor. Finally each particle is locked within three-dimensional magnetic well. It works even when particles have small fraction of superconductor. During the rings evolution some contribution to the disk also could come from the collision-generated debris of the current moon, coming meteorites and from the geysers like it happened due to magnetic coupling of Saturn and Enceladus. The rings are relict of the early days of the magnetic field of Saturn system.","PeriodicalId":434427,"journal":{"name":"International Journal of Astronomy and Astrophysics","volume":"9 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2018-02-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"125390563","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 6
Compatibility of the Observed Rotation Parameters of Radio Pulsars on Long Time Scales 射电脉冲星观测旋转参数在长时间尺度上的相容性
International Journal of Astronomy and Astrophysics Pub Date : 2018-02-08 DOI: 10.4236/IJAA.2018.81003
A. Avramenko, Boris Yakovlevich Losovsky, V. D. Pugachev, T. V. Shabanova
{"title":"Compatibility of the Observed Rotation Parameters of Radio Pulsars on Long Time Scales","authors":"A. Avramenko, Boris Yakovlevich Losovsky, V. D. Pugachev, T. V. Shabanova","doi":"10.4236/IJAA.2018.81003","DOIUrl":"https://doi.org/10.4236/IJAA.2018.81003","url":null,"abstract":"We present the results of an analysis of the rotation regularities of pulsars from the current observations and retrospective data on the timing of pulsars at Pushchino Observatory, obtained since 1978 to 2017. Parametric approximation of numerical series of Times of Arrival (ToAs) the convergence polynomial series defined the combinations of numerical values, unique for each pulsar, identical in any reference system for coinciding epochs, irrespective of duration of observations that corresponds to the coherence of periodic radiation of pulsars. The braking index at all observed pulsars is n =−(0.9 ± 0.2) that corresponds monotony of slowing down of rotation (>0). The polynomial power series of the intervals calculated in observed parameters of rotation represent an analytical time scale on which variations of observed intervals, uncorrelated with rotation, are counted, as at pulsars B1919+21 and B0809+74, or the unpredictable variations of intervals defining the movement of a pulsar in the supernova remnants, as at PSR B0531+21 or at PSR B1822-09 which spontaneous movement also doesn’t exclude its belonging to the supernova remnants.","PeriodicalId":434427,"journal":{"name":"International Journal of Astronomy and Astrophysics","volume":"21 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2018-02-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"115558185","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 2
Mass Distribution in Space-Time and Conception about Space-Time-Mass Continuum 时空质量分布与时空质量连续体概念
International Journal of Astronomy and Astrophysics Pub Date : 2018-02-08 DOI: 10.4236/IJAA.2018.81007
Rahul K. Singh
{"title":"Mass Distribution in Space-Time and Conception about Space-Time-Mass Continuum","authors":"Rahul K. Singh","doi":"10.4236/IJAA.2018.81007","DOIUrl":"https://doi.org/10.4236/IJAA.2018.81007","url":null,"abstract":"There is a relation between space and time, which is called space-time continuum. With the help of some mathematical equations, we can establish an alternative relation between space-time and mass, treating mass as a fifth dimension. There is the concept about mass being a property of any inertial or gravitational object in space. Mass can create distortion in space. As a result of that, space-time curvature will be bent towards the massive object.","PeriodicalId":434427,"journal":{"name":"International Journal of Astronomy and Astrophysics","volume":"87 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2018-02-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"133198254","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
A Spherical Relativistic Anisotropic Compact Star Model 一个球面相对论各向异性致密星模型
International Journal of Astronomy and Astrophysics Pub Date : 2018-02-08 DOI: 10.4236/IJAA.2018.81004
Prakash Chandra Fulara, A. Sah
{"title":"A Spherical Relativistic Anisotropic Compact Star Model","authors":"Prakash Chandra Fulara, A. Sah","doi":"10.4236/IJAA.2018.81004","DOIUrl":"https://doi.org/10.4236/IJAA.2018.81004","url":null,"abstract":"We provide solutions to Einsteins field equations for a model of a spherically symmetric anisotropic fluid distribution, relevant to the description of compact stars. The central matter-energy density, radial and tangential pressures, red shift and speed of sound are positive definite and are decreasing monotonically with increasing radial distance from the center of matter distribution of astrophysical object. The causality condition is satisfied for complete fluid distribution. The central value of anisotropy is zero and is increasing monotonically with increasing radial distance from the center of the distribution. The adiabatic index is increasing with increasing radius of spherical fluid distribution. The stability conditions in relativistic compact star are also discussed in our investigation. The solution is representing the realistic objects such as SAXJ1808.4-3658, HerX-1, 4U1538-52, LMC X-4, CenX-3, VelaX-1, PSRJ1614-2230 and PSRJ0348+0432 with suitable conditions.","PeriodicalId":434427,"journal":{"name":"International Journal of Astronomy and Astrophysics","volume":"8 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2018-02-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"132043968","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 8
The Moon Meets All Requirements of the IAU Definition for “Planet” 月球符合国际天文学联合会对“行星”定义的所有要求
International Journal of Astronomy and Astrophysics Pub Date : 2017-12-18 DOI: 10.4236/IJAA.2017.74024
D. Russell
{"title":"The Moon Meets All Requirements of the IAU Definition for “Planet”","authors":"D. Russell","doi":"10.4236/IJAA.2017.74024","DOIUrl":"https://doi.org/10.4236/IJAA.2017.74024","url":null,"abstract":"The Earth-Moon system has often been characterized as having some characteristics of a “double planet” system. It is demonstrated that while the orbital barycenter of the Earth-Moon pair lies inside the radius of the Earth, the Moon does meet all three requirements of the IAU definition for “planet” and therefore the Moon can correctly be identified as the Solar System’s 9th planet. In order to avoid confusion by this development it is necessary to add definitions for “double planet”, “double dwarf planet”, “satellite planet”, and “satellite” to complement the International Astronomical Union definitions for “planet” and “dwarf planet”. The Earth-Moon system meets the requirements of a “double planet” system while the Pluto-Charon system meets the requirements of a “double dwarf planet” system. In order to extrapolate sub-stellar taxonomy to exoplanetary systems, general formation mechanisms (star-like gas collapse in molecular clouds vs. proto-planetary disk formation) should be included in the definitions for the various classes of sub-stellar mass bodies.","PeriodicalId":434427,"journal":{"name":"International Journal of Astronomy and Astrophysics","volume":"121 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2017-12-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"127342087","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 1
Constraints on Neutrino Masses from Baryon Acoustic Oscillation Measurements 重子声学振荡测量对中微子质量的约束
International Journal of Astronomy and Astrophysics Pub Date : 2017-12-10 DOI: 10.4236/ijaa.2018.81001
B. Hoeneisen
{"title":"Constraints on Neutrino Masses from Baryon Acoustic Oscillation Measurements","authors":"B. Hoeneisen","doi":"10.4236/ijaa.2018.81001","DOIUrl":"https://doi.org/10.4236/ijaa.2018.81001","url":null,"abstract":"From 21 independent Baryon Acoustic Oscillation (BAO) measurements we obtain the following sum of masses of active Dirac or Majorana neutrinos: , where and . This result may be combined with independent measurements that constrain the parameters Σmv, h, and Ωbh2 . For   and , we obtain at 95% confidence.","PeriodicalId":434427,"journal":{"name":"International Journal of Astronomy and Astrophysics","volume":"38 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2017-12-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"132611970","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 3
On the Artificial Equilibrium Points in the Circular Restricted Problem of 2 + 2 Bodies 2 + 2体圆形限制问题中的人工平衡点
International Journal of Astronomy and Astrophysics Pub Date : 2017-11-01 DOI: 10.4236/IJAA.2017.74020
Kumari Ranjana, Vijay Kumar
{"title":"On the Artificial Equilibrium Points in the Circular Restricted Problem of 2 + 2 Bodies","authors":"Kumari Ranjana, Vijay Kumar","doi":"10.4236/IJAA.2017.74020","DOIUrl":"https://doi.org/10.4236/IJAA.2017.74020","url":null,"abstract":"The present work studies the stability condition of central control artificial equilibrium points of the planar circular restricted problem of 2 + 2 bodies (PCRP2 + 2B) and also its variant when the shape of larger mass is taken to be an oblate spheroid. We find that the paper will be of great application in choosing an artificial equilibrium point (AEP) in the neighbourhood of numerous planets e.g. Jupiter or the bodies which provide a model of the problem studied. The minimum thrust will save a quantum of energy to be applied to have an arbitrary point as a chosen starter. For solar sailing and magnetic force this minimum thrust will be of great use.","PeriodicalId":434427,"journal":{"name":"International Journal of Astronomy and Astrophysics","volume":"26 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2017-11-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"125938981","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Is the Velocity Interpretation of the Redshift of Spectral Lines in Accordance with Astronomical Data 光谱线红移的速度解释与天文数据相符吗
International Journal of Astronomy and Astrophysics Pub Date : 2017-11-01 DOI: 10.4236/IJAA.2017.74021
L. Marosi
{"title":"Is the Velocity Interpretation of the Redshift of Spectral Lines in Accordance with Astronomical Data","authors":"L. Marosi","doi":"10.4236/IJAA.2017.74021","DOIUrl":"https://doi.org/10.4236/IJAA.2017.74021","url":null,"abstract":"Current progress in cosmic microwave background (CMB) anisotropy measurements opens up the possibility of determining Hubble’s constant (H0 = h × 100 km s−1 Mpc−1) from the CMB power spectrum radiation temperature anisotropy. The results show that, besides the Lambda cold dark matter (ΛCDM) model, much simpler Einstein-de Sitter (EdeS) models without the cosmological constant can fit the data as well, or even better, than the ΛCDM model. Calculations with EdeS models yield unexpectedly low values for Hubble’s constant of h = 0.30 and 0.46, respectively. These values are completely inconsistent with the direct determination of h ~ 0.70 from the redshift (RS) of spectral lines. In the present paper I consider whether the gap between h = 0.3 and h = 0.7 could be explained using conventional physics without introducing further hypotheses, or whether the RS of starlight and the RS of the CMB could stem from different physical origins.","PeriodicalId":434427,"journal":{"name":"International Journal of Astronomy and Astrophysics","volume":"1 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2017-11-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"128274954","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 2
Membership Determination of van den Bergh Open Clusters vdB92, vdB146 (NGC 7129) and vdB150 van den Bergh疏散星团vdB92、vdB146 (NGC 7129)和vdB150的隶属度测定
International Journal of Astronomy and Astrophysics Pub Date : 2017-11-01 DOI: 10.4236/IJAA.2017.74023
R. B. Orellana, M. Biasi, L. G. Paiz
{"title":"Membership Determination of van den Bergh Open Clusters vdB92, vdB146 (NGC 7129) and vdB150","authors":"R. B. Orellana, M. Biasi, L. G. Paiz","doi":"10.4236/IJAA.2017.74023","DOIUrl":"https://doi.org/10.4236/IJAA.2017.74023","url":null,"abstract":"In this paper we study some van den Bergh open clusters combining photometry and astrometry. A model which analyses the proper motion distribution and the stellar density is applied to find the kinematic parameters and stellar membership in the region of the open clusters vdB92, vdB146 (NGC 7129) and vdB150. The astrometric data are obtained from UCAC4 catalogue. The centre coordinates, the components of mean proper motion, the angular diameter and the astrometric members are reported, taking the following values: for vdB92: α=105.97281°±0.13113°, δ=−11.57814°±0.10575°, μαcosδ=−3.46±0.19mas/yr,μδ=1.27±0.19mas/yr, 34', 60 members; for vdB146: α=325.78423°±0.15297°, δ=66.13575°±0.02907°, μαcosδ=−2.71±0.25mas/yr, μδ=−3.32±0.25mas/yr, 9', 5 members; and for vdB150: α=332.22519°±0.06074°, δ=73.40232°±0.0.07789°, μαcosδ=3.07±0.90mas/yr, μδ=4.65±0.90mas/yr, 15', 7 members. The incidence of the proper motion errors in the determination of the cluster parameters and of the stellar membership is analysed and it is found that they do not significantly change. We finally compare the astrometric members with the photometric ones given in the literature.","PeriodicalId":434427,"journal":{"name":"International Journal of Astronomy and Astrophysics","volume":"53 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2017-11-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"122719601","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Short-Period and Long-Period Effects of Weak Gravitational Waves 弱引力波的短周期和长周期效应
International Journal of Astronomy and Astrophysics Pub Date : 2017-07-19 DOI: 10.4236/IJAA.2017.73019
M. H. Youssef
{"title":"Short-Period and Long-Period Effects of Weak Gravitational Waves","authors":"M. H. Youssef","doi":"10.4236/IJAA.2017.73019","DOIUrl":"https://doi.org/10.4236/IJAA.2017.73019","url":null,"abstract":"We compute the long-term orbital variation of a test particle orbiting a central body acted upon by normal incident of plane gravitational wave. We use the tools of celestial mechanics to give the first order solution of canonical equations of long-period and short-period terms of the perturbed Hamiltonian of gravitational waves. We consider normal incident of plane gravitational wave and characteristic size of bound—two body system (earth’s satellite or planet) is much smaller than the wavelength of the wave and the wave’s frequency nw is much smaller than the particle’s orbital np. We construct the Hamiltonian of the gravitational waves in terms of the canonical variables (l,g,h,L,G,H) and we solve the canonical equations numerically using Runge-Kutta fourth order method using language MATHEMATICA V10. Taking Jupiter as practical example we found that there are long period perturbations on ω,Ω and i and not changing with revolution and the short period perturbations on a, e and M changing with revolution during the interval of time (t−t0 ) which is changing from 0→4π.","PeriodicalId":434427,"journal":{"name":"International Journal of Astronomy and Astrophysics","volume":"7 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2017-07-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"114586607","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 2
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