Communications of the Byurakan Astrophysical Observatory最新文献

{"title":"Inertia II: The local induced inertia effects","authors":"G. Ter-Kazarian","doi":"10.52526/25792776-23.70.2-212","DOIUrl":"https://doi.org/10.52526/25792776-23.70.2-212","url":null,"abstract":"Inthe frameworkof localMSp-SUSYtheory,which is extensionof global, socalled,master space (MSp)-SUSYtheory(Ter-Kazarian, 2023, 2024),weaddress theacceleratedmotionand inertiaeffects. The superspace isadirect sumof curvedbackgrounddouble spacesM4⊕MSp,withan inclusionof additional fermioniccoordinates(Θ, ¯ Θ) inducedbythespinors(θ,¯ θ),whichrefertoMSp.Wetakethe Lorentzgroupasour structuregroupinorder torecover rigidsuperspaceasa limitingsolutiontoour dynamicaltheory.ThelocalMSp-SUSYisconceivedasaquantumfieldtheorywhoseactionincludesthe fictitiousgravitationfieldterm,wherethegravitoncoexistswithafermionicfieldof, so-called,gravitino (sparticle) describedby theRarita-Scwinger kinetic term. Asignificant differencebetween standard theoriesof supergravityandthelocalMSp-SUSYtheoryisthatacouplingof supergravitywithmatter superfields no longer holds. We argue that adeformation/(distortionof local internal properties) of MSp, istheoriginof theabsoluteacceleration(aabs=0)andinertiaeffects(fictitiousgraviton). These gravitational fieldshadnosourcesandweregeneratedbycoordinate transformations. Acurvatureof MSparisesentirelyduetotheinertialpropertiesoftheLorentz-rotatedframeof interest.Thisrefersto theparticleof interestitself,withoutrelationtoothermatterfields,sothatthiscanbegloballyremoved byappropriatecoordinatetransformations. ThesupervielbeinEA(z),beinganalogueofCartan’s local frame, isthedynamicalvariableof superspaceformulation,whichidentifiesthetetradfielde ˆ a ˆ m(X)and theRarita-Schwingerfields. Theconnectionis theseconddynamicalvariable inthis theory. Thefield e ˆ a ˆ m(X)plays the roleof agaugefieldassociatedwith local transformations (fictitious graviton). The fictitiousgravitinoisthegaugefieldrelatedtolocalsupersymmetry.Thetwofieldsdifferintheirspin: 2 forthegraviton,3/2forthegravitino.Thesetwoparticlesarethetwobosonicandfermionicstatesofa gaugeparticleinthecurvedbackgroundspacesM4andMSp,respectively,orviceversa.Following(TerKazarian, 2012), inthe frameworkof classical physics,wediscuss the inertiaeffectsbygoingbeyond thehypothesisof locality, andderive theexplicit formof thevierbiene ˆ a ˆ m( )≡(ea m( ),e a m( )). This theoryfurnishesjustificationfortheintroductionoftheweakprincipleofequivalence(WPE).Wederive ageneralexpressionoftherelativisticinertial forceexertedontheextendedspinningbodymovinginthe Rieman-Cartanspace.","PeriodicalId":412578,"journal":{"name":"Communications of the Byurakan Astrophysical Observatory","volume":"38 49","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-01-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139442826","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}

{"title":"Unraveling the Origins and Development of the Galactic Disk through Metal-Poor Stars","authors":"Maria Rah, Yatman Manolya, Ali Taani, A. Abushattal, K. M. Mohammad","doi":"10.52526/25792776-23.70.2-306","DOIUrl":"https://doi.org/10.52526/25792776-23.70.2-306","url":null,"abstract":"The Milky Way is a spiral galaxy comprising three main components: the Bulge, the Disk, and the Halo. Of particular interest is the Galactic disk, which holds a significant portion of the baryonic matter angular momentum and harbors at least two primary stellar populations: the thin and thick disks. Understanding the formation and evolution of the Galactic disk is crucial for comprehending the origins and development of our Galaxy. Stellar archaeology offers a means to probe the disk’s evolution by listening to the cosmological narratives of its oldest and most pristine stars, specifically the metal-poor stars. In this study, we employed accurate photometric metallicity estimates and Gaia Early Data Release 3 astrometry to curate a pure sample of the oldest Galactic stars. This proceeding presents a summary of our primary findings.","PeriodicalId":412578,"journal":{"name":"Communications of the Byurakan Astrophysical Observatory","volume":"12 16","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-01-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139443382","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}

{"title":"Role of galactic disc thickness in magnetic field generation","authors":"E. Mikhailov, M. V. Frolova","doi":"10.52526/25792776-23.70.2-282","DOIUrl":"https://doi.org/10.52526/25792776-23.70.2-282","url":null,"abstract":"A large variety of galaxies have magnetic structures of lengthscales comparable with their radius. Theoretically, their existence is based on the dynamo mechanism. It is based on alpha-effect characterizing helicity of the turbulent motions and differential rotation which is connected with changing angular velocity. The field can be destroyed by turbulent diffusion, so the mechanism is threshold and can be realized only for the case when first and second effect are more intensive than the third one. Equations of magnetohydrodynamics that are used to describe the dynamo mechanism, are too difficult to be solved. So, usually different approximation taking into account details of astrophysical objects are used. As for galaxies, a thin disc approximation has been developed. It works properly for galactic objects with small half-thickness. However, as for thick discs we should take a model which uses more complicated structure of the field. Here we find the threshold for the field generation for thick astrophysical discs.","PeriodicalId":412578,"journal":{"name":"Communications of the Byurakan Astrophysical Observatory","volume":"11 16","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-01-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139443451","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}

{"title":"Reflection of Radiation from a Plane-Parallel Half-Space in the Case of Redistribution of Radiation by Frequencies and Directions","authors":"H. V. Pikichyan","doi":"10.52526/25792776-23.70.2-235","DOIUrl":"https://doi.org/10.52526/25792776-23.70.2-235","url":null,"abstract":"Themethod introduced intheauthor’s twopreviousworks isusedtosolve theproblemofdiffuse reflectionfromasemi-infiniteplane-parallel scattering-absorbingmediuminthegeneralcaseof redistributionofradiationbyfrequenciesanddirectionsinanelementaryactofscattering.Asystemoffunctional equationswasobtainedtodeterminetheunknowneigenfunctionsandeigenvalues.Theinitialproblemof thesixexplanatoryvariablesisexplicitlyexpressedintermsoftheseeigenfunctionsthatdependonlyon threeindependentvariables(dimensionlessfrequency,zenithangle,andazimuth).","PeriodicalId":412578,"journal":{"name":"Communications of the Byurakan Astrophysical Observatory","volume":"27 6","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-01-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139443465","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}

{"title":"Morphological Study of Active Galaxies based on SDSS Images. Preliminary Results","authors":"V. K. Mkrtchyan, A.M. Mickaelian †, H.V. Abrahamyan ‡, G.A. Mikayelyan §, G. Paronyan, RA Nas, V. A. Byurakan, Astrophysical Observatory","doi":"10.52526/25792776-23.70.2-358","DOIUrl":"https://doi.org/10.52526/25792776-23.70.2-358","url":null,"abstract":"Activity in galaxies has mainly two major forms: Active Galactic Nuclei (AGN) and Starburst (SB). Moreover, different types of AGN have different morphology. However, this question has not yet been properly investigated and due to old low-quality images, the morphology of many galaxies is not well described. SDSS images give a good possibility to homogeneously classify galaxies and investigate differences by the activity types. The concentration of the central part and the ratio between the central bulge and the total flux is a subject for detailed study. We use SDSS images to classify different types of active galaxies (both AGN and Starburst) and understand differences between QSOs, Seyferts 1 and 2, LINERS and Composites, as well as Starburst galaxies. The best expectation from our study will be the preliminary classification of active galaxies into activity types based on the images and before having their spectral types.","PeriodicalId":412578,"journal":{"name":"Communications of the Byurakan Astrophysical Observatory","volume":"18 3","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-01-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139443505","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}

{"title":"Infrared surveys to search for high proper motion stars","authors":"E. D. Malik, O. Y. Malkov","doi":"10.52526/25792776-23.70.2-297","DOIUrl":"https://doi.org/10.52526/25792776-23.70.2-297","url":null,"abstract":"There are restrictions on the nature and characteristics of nearby brown dwarfs (including hypothetical component of the Sun), imposed by the current results of the work of the Gaia space observatory. In particular, even close brown dwarfs of spectral type Y3 and colder will go unnoticed by the Gaia observatory, although they may well be already included in infrared survey catalogues. Here we present information on modern infrared surveys, which can be used for a search for such objects.","PeriodicalId":412578,"journal":{"name":"Communications of the Byurakan Astrophysical Observatory","volume":"38 48","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-01-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139442827","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}

{"title":"The Pleiades flare stars in the Gaia era","authors":"V. Hambaryan, S. Ghazaryan, L. Hambardzumyan, R. Neuhaeuser, A. Mirzoyan, K. P. Tsvetkova","doi":"10.52526/25792776-23.70.2-242","DOIUrl":"https://doi.org/10.52526/25792776-23.70.2-242","url":null,"abstract":"We study the six-dimensional arrangement of flare stars in the Pleiades cluster region using the third release of the Gaia–mission (Gaia DR3) and we provide preliminary, a new, original view of the spatial configuration of the flare “star-members” of the cluster.","PeriodicalId":412578,"journal":{"name":"Communications of the Byurakan Astrophysical Observatory","volume":"9 8","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-01-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139441737","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}

{"title":"The influence of environmental effects on Type Ia Supernovae Standardization","authors":"A. Y. Baluta, M. Pruzhinskaya, P. Rosnet, N. Pauna","doi":"10.52526/25792776-23.70.2-316","DOIUrl":"https://doi.org/10.52526/25792776-23.70.2-316","url":null,"abstract":"Type Ia Supernovae (SNe Ia) are used as reliable cosmic distance indicators and their standardization is necessary for a more accurate measurement of the cosmological parameters of the Universe using the Hubble diagram. However, the Hubble diagram still shows intrinsic dispersion, potentially influenced by the supernova’s environment. In this study, we reproduce Hubble fit diagrams for the Pantheon supernovae data, and also investigate the possibility of introducing various standardization equations for supernovae that exploded in early- and late-type galaxies. We analyze 330 SNe Ia from the Pantheon cosmological sample to study how host galaxy morphology affects SN Ia standardization. We find that SNe Ia hosted by early-type galaxies have different standardization parameters compared to those hosted by late-type galaxies. We conclude that correcting for host galaxy morphology significantly impacts the accuracy of the Hubble diagram fit.","PeriodicalId":412578,"journal":{"name":"Communications of the Byurakan Astrophysical Observatory","volume":"44 22","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-01-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139442472","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}

{"title":"Building the Largest Sample of IR Galaxies. Preliminary Results","authors":"G. Mikayelyan, A. Mickaelian, H. Abrahamyan, G. Paronyan","doi":"10.52526/25792776-23.70.2-321","DOIUrl":"https://doi.org/10.52526/25792776-23.70.2-321","url":null,"abstract":"To build the IRAS full extragalactic sample (including both point-like sources - QSOs, and extended ones - galaxies), we have applied several approaches. Cross-correlation of IRAS PSC/FSC Combined Catalogue with optical catalogues of already known galaxies, quasars and blazars such as The NGC 2000.0 Catalog, Third Reference Catalogue of Bright Galaxies, The Roma BZCAT, Astrometric Catalogue 5 and many others. Cross-correlation of IRAS PSC/FSC Combined Catalogue with optical catalogues giving data, which can be used to determine galaxy candidates, for example Sloan Digital Sky Survey (SDSS, contains data about point like and extended objects), The APM North Catalogue (contains data about ellipticity of objects), etc. Cross-correlation of IRAS PSC/FSC Combined Catalogue with GAIA DR3, which gives data about proper motions of objects (we can consider the objects having real proper motions as stars and exclude them from the sample). If all data show the same type of object, then we give it as a genuine one, and if there is an ambiguity, we give the most probable type with a flag. All this will lead to construction of a confident sample of optical counterparts of extragalactic objects of IRAS PSC/FSC: galaxies and quasars. We also will study IR/opt flux ratios, which may serve as one more characteristic to reveal galaxies with very high SFR. We will carry out calculation of IR luminosities for all IR galaxies. We expect revelation of many new ULIRGs and HLIRGs and building their largest samples.","PeriodicalId":412578,"journal":{"name":"Communications of the Byurakan Astrophysical Observatory","volume":"118 15","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-01-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139444615","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}

{"title":"Inertia I: The global MSp-SUSY induced uniform motion","authors":"G. Ter-Kazarian","doi":"10.52526/25792776-23.70.2-170","DOIUrl":"https://doi.org/10.52526/25792776-23.70.2-170","url":null,"abstract":"In this communication our main emphasis is on the review of the foundations of standard Lorentz code\u0000(SLC) of a particle motion. To this aim, we develop the theory of global, so-called, `double space´- or\u0000master space (MSp)-supersymmetry, subject to certain rules, wherein the superspace is a 14D-extension\u0000of a direct sum of background spaces M4⊕ MSp by the inclusion of additional 8D fermionic coordinates.\u0000The latter is induced by the spinors θ and ¯θ referred to MSp. While all the particles are living on\u0000M4, their superpartners can be viewed as living on MSp. This is a main ground for introducing MSp,\u0000which is unmanifested individual companion to the particle of interest. Supersymmetry transformation is\u0000defined as a translation in superspace, specified by the group element with corresponding anticommuting\u0000parameters. The multiplication of two successive transformations induce the motion. As a corollary, we\u0000derive SLC in a new perspective of global double MSp-SUSY transformations in terms of Lorentz spinors\u0000(θ,\u0000¯θ). This calls for a complete reconsideration of our ideas of Lorentz motion code, to be now referred\u0000to as the individual code of a particle, defined as its intrinsic property. In MSp-SUSY theory, obviously as\u0000in standard unbroken SUSY theory, the vacuum zero point energy problem, standing before any quantum\u0000field theory in M4, is solved. The particles in M4 themselves can be considered as excited states above the\u0000underlying quantum vacuum of background double spaces M4⊕ MSp, where the zero point cancellation\u0000occurs at ground-state energy, provided that the natural frequencies are set equal (q\u00002\u00000 ≡ νb = νf ), because\u0000the fermion field has a negative zero point energy while the boson field has a positive zero point energy.\u0000On these premises, we derive the two postulates on which the Special Relativity (SR) is based.","PeriodicalId":412578,"journal":{"name":"Communications of the Byurakan Astrophysical Observatory","volume":"27 4","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-01-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139441709","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}