In this paper, the integrated continuum radio spectrum of supernova remnant (SNR) W44 was analyzed up to 70 GHz, testing the different emission models that can be responsible for its particular shape. The observations by the Planck space telescope made it possible to analyze the high frequency part of radio emission from SNRs. Although the quality of radio continuum spectrum (a high scatter of data points at same frequencies) prevents us to make definite conclusions, the possibility of spinning dust emission detection towards this remnant is emphasized. In addition, a concave-down feature, due to synchrotron losses, can not be definitely dismissed by the present knowledge of the integrated radio continuum spectrum of this SNR. [Projekat Ministarstva nauke Republike Srbije, br. 176005: Emission Nebulae: Structure and Evolution]
{"title":"On the Integrated Continuum Radio Spectrum of Supernova Remnant W44 (G34.7-0.4): New Insights From Planck","authors":"D. Onić","doi":"10.2298/SAJ150715004O","DOIUrl":"https://doi.org/10.2298/SAJ150715004O","url":null,"abstract":"In this paper, the integrated continuum radio spectrum of supernova remnant \u0000 (SNR) W44 was analyzed up to 70 GHz, testing the different emission models \u0000 that can be responsible for its particular shape. The observations by the \u0000 Planck space telescope made it possible to analyze the high frequency part of \u0000 radio emission from SNRs. Although the quality of radio continuum spectrum (a \u0000 high scatter of data points at same frequencies) prevents us to make definite \u0000 conclusions, the possibility of spinning dust emission detection towards this \u0000 remnant is emphasized. In addition, a concave-down feature, due to \u0000 synchrotron losses, can not be definitely dismissed by the present knowledge \u0000 of the integrated radio continuum spectrum of this SNR. [Projekat \u0000 Ministarstva nauke Republike Srbije, br. 176005: Emission Nebulae: Structure \u0000 and Evolution]","PeriodicalId":48878,"journal":{"name":"Serbian Astronomical Journal","volume":"191 1","pages":"29-37"},"PeriodicalIF":0.5,"publicationDate":"2015-05-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"68672696","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}
G. Apostolovska, Z. Donchev, A. Kostov, V. Ivanova, G. Borisov, B. Bilkina
An analysis of photometric observations of Mars crosser asteroid 1011 Laodamia conducted at Bulgarian National Astronomical Observatory Rozhen over a twelve year interval (2002, 2003, 2004, 2006, 2007, 2008, 2011, 2012 and 2013) is made. Based on the obtained lightcurves the spin vector, sense of rotation, and preliminary shape model of (1011) Laodamia have been determined using the lightcurve inversion method. The aim of this investigation is to increase the set of asteroids with known spin and shape parameters and to contribute in improving the model in combination with other techniques and sparse data produced by photometric asteroid surveys such as Pan-STARRS or GAIA.
{"title":"Photometry and shape modeling of Mars crosser asteroid (1011) Laodamia","authors":"G. Apostolovska, Z. Donchev, A. Kostov, V. Ivanova, G. Borisov, B. Bilkina","doi":"10.2298/SAJ1489079A","DOIUrl":"https://doi.org/10.2298/SAJ1489079A","url":null,"abstract":"An analysis of photometric observations of Mars crosser asteroid 1011 \u0000 Laodamia conducted at Bulgarian National Astronomical Observatory Rozhen over \u0000 a twelve year interval (2002, 2003, 2004, 2006, 2007, 2008, 2011, 2012 and \u0000 2013) is made. Based on the obtained lightcurves the spin vector, sense of \u0000 rotation, and preliminary shape model of (1011) Laodamia have been determined \u0000 using the lightcurve inversion method. The aim of this investigation is to \u0000 increase the set of asteroids with known spin and shape parameters and to \u0000 contribute in improving the model in combination with other techniques and \u0000 sparse data produced by photometric asteroid surveys such as Pan-STARRS or \u0000 GAIA.","PeriodicalId":48878,"journal":{"name":"Serbian Astronomical Journal","volume":"189 1","pages":"79-85"},"PeriodicalIF":0.5,"publicationDate":"2014-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"68672574","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}
SUMMARY: In this paper we generalized the fast convergent Forth-and-Back Implicit Lambda Iteration (FBILI) method to the solution of the two-level atom line transfer problems in media with low velocity fields using the observer’s reference frame. In order to test the accuracy and the convergence properties of the method we solved several astrophysically important benchmark problems of the NLTE line formation: in a plan-parallel differentially expanding medium of finite thickness, and in spherically symmetric stellar atmospheres, both static and expanding. We compared our solutions with those obtained by other authors using different numerical methods.
{"title":"FBILI METHOD FOR THE TWO-LEVEL ATOM LINE FORMATION IN MEDIA WITH LOW VELOCITY FIELDS","authors":"I. Pirkovic, O. Atanacković","doi":"10.2298/SAJ1489053P","DOIUrl":"https://doi.org/10.2298/SAJ1489053P","url":null,"abstract":"SUMMARY: In this paper we generalized the fast convergent Forth-and-Back Implicit Lambda Iteration (FBILI) method to the solution of the two-level atom line transfer problems in media with low velocity fields using the observer’s reference frame. In order to test the accuracy and the convergence properties of the method we solved several astrophysically important benchmark problems of the NLTE line formation: in a plan-parallel differentially expanding medium of finite thickness, and in spherically symmetric stellar atmospheres, both static and expanding. We compared our solutions with those obtained by other authors using different numerical methods.","PeriodicalId":48878,"journal":{"name":"Serbian Astronomical Journal","volume":"189 1","pages":"53-67"},"PeriodicalIF":0.5,"publicationDate":"2014-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"68672452","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}
SUMMARY: In the present paper, a universal symbolic expression for radial distance of conic motion in recursive power series form is developed. The importance of this analytical power series representation is that it is invariant under many operations because the result of addition, multiplication, exponentiation, integration, differentiation, etc. of a power series is also a power series. This is the fact that provides excellent flexibility in dealing with analytical, as well as computational developments of problems related to radial distance. For computational developments, a full recursive algorithm is developed for the series coefficients. An efficient method using the continued fraction theory is provided for series evolution, and two devices are proposed to secure the convergence when the time interval (t − t0) is large. In addition, the algorithm does not need the solution of Kepler’s equation and its variants for parabolic and hyperbolic orbits. Numerical applications of the algorithm are given for three orbits of different eccentricities; the results showed that it is accurate for any conic motion.
{"title":"Universal symbolic expression for radial distance of conic motion","authors":"M. Sharaf, A. S. Saad, A. Alshaery","doi":"10.2298/SAJ1489087S","DOIUrl":"https://doi.org/10.2298/SAJ1489087S","url":null,"abstract":"SUMMARY: In the present paper, a universal symbolic expression for radial distance of conic motion in recursive power series form is developed. The importance of this analytical power series representation is that it is invariant under many operations because the result of addition, multiplication, exponentiation, integration, differentiation, etc. of a power series is also a power series. This is the fact that provides excellent flexibility in dealing with analytical, as well as computational developments of problems related to radial distance. For computational developments, a full recursive algorithm is developed for the series coefficients. An efficient method using the continued fraction theory is provided for series evolution, and two devices are proposed to secure the convergence when the time interval (t − t0) is large. In addition, the algorithm does not need the solution of Kepler’s equation and its variants for parabolic and hyperbolic orbits. Numerical applications of the algorithm are given for three orbits of different eccentricities; the results showed that it is accurate for any conic motion.","PeriodicalId":48878,"journal":{"name":"Serbian Astronomical Journal","volume":"189 1","pages":"87-92"},"PeriodicalIF":0.5,"publicationDate":"2014-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"68672641","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}
Landing on Mars is extremely challenging task due to the fact that the Martian atmosphere is the most hostile environment in the Solar system to perform the entry, descent and landing (EDL) process, because it is thick enough to create substantial heating of the entry vehicle but not thick enough to reduce its velocity to the one necessary for safe landing. Beside this, the atmosphere is very dynamic mainly due to high eccentricity of the Martian orbit, obliquity of the orbital to the equatorial plane and close alignment of the winter solstice and the orbital perihelion. Although seasonal variations of atmospheric parameters are significantly larger than the diurnal, it is very important to analyze diurnal cycles as they can significantly change vertical and horizontal atmospheric profiles in very short time intervals. This can present a serious threat to missions which have very precise timings and specific requirements such as the requirement for the daytime landing to enable ground images acquisition during the descent and landing phase. A 3-degrees-of-freedom trajectory integration routine was combined with the Mars Global Reference Atmospheric Model (Mars-GRAM) to identify the dependence of the EDL profiles on the diurnal cycles of atmospheric parameters throughout the Martian year. The obtained results show that the influence of the diurnal cycles is the largest at the equator and decreases relatively symmetrically towards the poles with a slightly stronger influence in the northern hemisphere. Also, there is a significant influence of the orbital position of Mars on the effect of diurnal atmospheric variations which causes that, around the orbital perihelion and winter solstice, there is some kind of inversion of the dependance of optimal entry timing on latitude of the landing site comparing to the rest of the Martian year. [Projekat Ministarstva nauke Republike Srbije, br. 176002]
{"title":"The Effects of the Diurnal Atmospheric Variability on Entry, Descent and Landing on Mars","authors":"D. Marčeta","doi":"10.2298/SAJ1489069M","DOIUrl":"https://doi.org/10.2298/SAJ1489069M","url":null,"abstract":"Landing on Mars is extremely challenging task due to the fact that the \u0000 Martian atmosphere is the most hostile environment in the Solar system to \u0000 perform the entry, descent and landing (EDL) process, because it is thick \u0000 enough to create substantial heating of the entry vehicle but not thick \u0000 enough to reduce its velocity to the one necessary for safe landing. Beside \u0000 this, the atmosphere is very dynamic mainly due to high eccentricity of the \u0000 Martian orbit, obliquity of the orbital to the equatorial plane and close \u0000 alignment of the winter solstice and the orbital perihelion. Although \u0000 seasonal variations of atmospheric parameters are significantly larger than \u0000 the diurnal, it is very important to analyze diurnal cycles as they can \u0000 significantly change vertical and horizontal atmospheric profiles in very \u0000 short time intervals. This can present a serious threat to missions which \u0000 have very precise timings and specific requirements such as the requirement \u0000 for the daytime landing to enable ground images acquisition during the \u0000 descent and landing phase. A 3-degrees-of-freedom trajectory integration \u0000 routine was combined with the Mars Global Reference Atmospheric Model \u0000 (Mars-GRAM) to identify the dependence of the EDL profiles on the diurnal \u0000 cycles of atmospheric parameters throughout the Martian year. The obtained \u0000 results show that the influence of the diurnal cycles is the largest at the \u0000 equator and decreases relatively symmetrically towards the poles with a \u0000 slightly stronger influence in the northern hemisphere. Also, there is a \u0000 significant influence of the orbital position of Mars on the effect of \u0000 diurnal atmospheric variations which causes that, around the orbital \u0000 perihelion and winter solstice, there is some kind of inversion of the \u0000 dependance of optimal entry timing on latitude of the landing site comparing \u0000 to the rest of the Martian year. [Projekat Ministarstva nauke Republike \u0000 Srbije, br. 176002]","PeriodicalId":48878,"journal":{"name":"Serbian Astronomical Journal","volume":"189 1","pages":"69-77"},"PeriodicalIF":0.5,"publicationDate":"2014-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"68672519","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}
M. Pavlović, A. Dobardžić, B. Vukoti'c, D. Urošević
In this paper we present the updated empirical radio surface- brightness-to-diameter (?-D) relation for Galactic supernova remnants (SNRs) calibrated using 110 SNRs with reliable distances. We apply orthogonal fitting procedure and kernel density smoothing in the ? ? D plane and compare the results with the latest theoretical ? - D relations derived from simulations of radio evolution of SNRs. We argue that the best agreement between the empirical and simulated ? ? D relations is achieved if the mixed-morphology SNRs and SNRs of both, low brightness and small diameter, are filtered out from the calibration sample. The distances to 5 newly discovered remnants and 27 new candidates for shell SNRs are estimated from our full and filtered calibration samples.
{"title":"Updated radio Σ - D relation for galactic supernova remnants - II","authors":"M. Pavlović, A. Dobardžić, B. Vukoti'c, D. Urošević","doi":"10.2298/SAJ1489025P","DOIUrl":"https://doi.org/10.2298/SAJ1489025P","url":null,"abstract":"In this paper we present the updated empirical radio surface-\u0000 brightness-to-diameter (?-D) relation for Galactic supernova remnants (SNRs)\u0000 calibrated using 110 SNRs with reliable distances. We apply orthogonal\u0000 fitting procedure and kernel density smoothing in the ? ? D plane and compare\u0000 the results with the latest theoretical ? - D relations derived from\u0000 simulations of radio evolution of SNRs. We argue that the best agreement\u0000 between the empirical and simulated ? ? D relations is achieved if the\u0000 mixed-morphology SNRs and SNRs of both, low brightness and small diameter,\u0000 are filtered out from the calibration sample. The distances to 5 newly\u0000 discovered remnants and 27 new candidates for shell SNRs are estimated from\u0000 our full and filtered calibration samples.","PeriodicalId":48878,"journal":{"name":"Serbian Astronomical Journal","volume":"52 1","pages":""},"PeriodicalIF":0.5,"publicationDate":"2014-11-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"68672442","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}
At the beginning of 2013, we have a team of scientists at the Astronomical Observatory of Belgrade, focusing on observations and research of blazars. At the same time, we established a cooperation with the Astronomical Observatory of Torino (Osservatorio Astrofisico di Torino), center for the Whole Earth Blazar Telescope (WEBT) international collaboration. In this paper, we describe the WEBT project, present our equipment as well as some preliminary results. We also point to some issues that we have encountered during the one year experience and found important from the observational point of view. [Projekat Ministarstva nauke Republike Srbije, br. 176011: Dynamics and Kinematics of Celestial Bodies and Systems, br. 176021: Visible and Invisible Matter in Nearby Galaxies: Theory and Observations i br. 176004: Stellar Physics]
2013年初，我们在贝尔格莱德天文台(Astronomical Observatory of Belgrade)组建了一支科学家团队，专注于对耀变体的观测和研究。同时，我们还与都灵天文台(Osservatorio Astrofisico di Torino)、全球Blazar望远镜(WEBT)国际合作中心建立了合作关系。本文介绍了WEBT项目，介绍了我们的设备和一些初步成果。我们还指出了我们在一年的经验中遇到的一些问题，从观察的角度来看，这些问题很重要。[南斯拉夫]塞族共和国部长项目;176011:天体动力学与运动学，[j]。176021:邻近星系中可见与不可见物质:理论与观测[j]。[176004:恒星物理]
{"title":"Research of blazars at the Astronomical observatory of Belgrade","authors":"O. Vince, G. Damljanovic","doi":"10.2298/SAJ1488067V","DOIUrl":"https://doi.org/10.2298/SAJ1488067V","url":null,"abstract":"At the beginning of 2013, we have a team of scientists at the Astronomical \u0000 Observatory of Belgrade, focusing on observations and research of blazars. At \u0000 the same time, we established a cooperation with the Astronomical Observatory \u0000 of Torino (Osservatorio Astrofisico di Torino), center for the Whole Earth \u0000 Blazar Telescope (WEBT) international collaboration. In this paper, we \u0000 describe the WEBT project, present our equipment as well as some preliminary \u0000 results. We also point to some issues that we have encountered during the one \u0000 year experience and found important from the observational point of view. \u0000 [Projekat Ministarstva nauke Republike Srbije, br. 176011: Dynamics and \u0000 Kinematics of Celestial Bodies and Systems, br. 176021: Visible and Invisible \u0000 Matter in Nearby Galaxies: Theory and Observations i br. 176004: Stellar \u0000 Physics]","PeriodicalId":48878,"journal":{"name":"Serbian Astronomical Journal","volume":"188 1","pages":"67-74"},"PeriodicalIF":0.5,"publicationDate":"2014-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://sci-hub-pdf.com/10.2298/SAJ1488067V","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"68672361","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}
S. Samurović, A. Vudragovic, M. Jovanović, M. Ćirković
In this paper we analyze the kinematics and dynamics of the nearby early-type galaxy NGC 821 based on its globular clusters (GCs) and planetary nebulae (PNe). We use PNe and GCs to extract the kinematics of NGC 821 which is then used for the dynamical modelling based on the Jeans equation. We apply the Jeans equation using the Newtonian mass-follows-light approach assuming constant mass-to-light ratio and find that using such an approach we can successfully fit the kinematic data. The inferred constant mass-to-light ratio, 4:2 < M=LB < 12:4 present throughout the whole galaxy, implies the lack of significant amount of dark matter. We also used three different MOND approaches and found that we can fit the kinematic data without the need for additional, dark, component. [Projekat Ministarstva nauke Republike Srbije, br. 176021: Visible and invisible matter in nearby galaxies: theory and observations]
{"title":"LOW DARK MATTER CONTENT OF THE NEARBY EARLY-TYPE GALAXY NGC 821","authors":"S. Samurović, A. Vudragovic, M. Jovanović, M. Ćirković","doi":"10.2298/SAJ1488029S","DOIUrl":"https://doi.org/10.2298/SAJ1488029S","url":null,"abstract":"In this paper we analyze the kinematics and dynamics of the nearby early-type \u0000 galaxy NGC 821 based on its globular clusters (GCs) and planetary nebulae \u0000 (PNe). We use PNe and GCs to extract the kinematics of NGC 821 which is then \u0000 used for the dynamical modelling based on the Jeans equation. We apply the \u0000 Jeans equation using the Newtonian mass-follows-light approach assuming \u0000 constant mass-to-light ratio and find that using such an approach we can \u0000 successfully fit the kinematic data. The inferred constant mass-to-light \u0000 ratio, 4:2 < M=LB < 12:4 present throughout the whole galaxy, implies the \u0000 lack of significant amount of dark matter. We also used three different MOND \u0000 approaches and found that we can fit the kinematic data without the need for \u0000 additional, dark, component. [Projekat Ministarstva nauke Republike Srbije, \u0000 br. 176021: Visible and invisible matter in nearby galaxies: theory and \u0000 observations]","PeriodicalId":48878,"journal":{"name":"Serbian Astronomical Journal","volume":"11 1","pages":"29-36"},"PeriodicalIF":0.5,"publicationDate":"2014-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://sci-hub-pdf.com/10.2298/SAJ1488029S","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"68672185","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}
We made an attempt to remedy recent confusing treatments of some basic relativistic concepts and results. Following the argument presented in an earlier paper (Redžic 2008b), we discussed the misconceptions that are recurrent points in the literature devoted to teaching relativity such as: there is no change in the object in Special Relativity, illusory character of relativistic length contraction, stresses and strains induced by Lorentz contraction, and related issues. We gave several examples of the traps of everyday language that lurk in Special Relativity. To remove a possible conceptual and terminological muddle, we made a distinction between the relativistic length reduction and relativistic FitzGerald-Lorentz contraction, corresponding to a passive and an active aspect of length contraction, respectively; we pointed out that both aspects have fundamental dynamical contents. As an illustration of our considerations, we discussed briefly the Dewan-Beran-Bell spaceship paradox and the ‘pole in a barn’ paradox. [Projekat Ministarstva nauke Republike Srbije, br. 171028]
{"title":"Relativistic Length Agony Continued","authors":"D. Redžić","doi":"10.2298/SAJ1488055R","DOIUrl":"https://doi.org/10.2298/SAJ1488055R","url":null,"abstract":"We made an attempt to remedy recent confusing treatments of some basic \u0000 relativistic concepts and results. Following the argument presented in an \u0000 earlier paper (Redžic 2008b), we discussed the misconceptions that are \u0000 recurrent points in the literature devoted to teaching relativity such as: \u0000 there is no change in the object in Special Relativity, illusory character of \u0000 relativistic length contraction, stresses and strains induced by Lorentz \u0000 contraction, and related issues. We gave several examples of the traps of \u0000 everyday language that lurk in Special Relativity. To remove a possible \u0000 conceptual and terminological muddle, we made a distinction between the \u0000 relativistic length reduction and relativistic FitzGerald-Lorentz \u0000 contraction, corresponding to a passive and an active aspect of length \u0000 contraction, respectively; we pointed out that both aspects have fundamental \u0000 dynamical contents. As an illustration of our considerations, we discussed \u0000 briefly the Dewan-Beran-Bell spaceship paradox and the ‘pole in a barn’ \u0000 paradox. [Projekat Ministarstva nauke Republike Srbije, br. 171028]","PeriodicalId":48878,"journal":{"name":"Serbian Astronomical Journal","volume":"188 1","pages":"55-65"},"PeriodicalIF":0.5,"publicationDate":"2014-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://sci-hub-pdf.com/10.2298/SAJ1488055R","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"68672353","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}
The past several decades have seen accelerating progress in improving binary stars fundamental parameters determinations, as new observational techniques have produced visual orbits of many spectroscopic binaries with a milli arcsecond precision. Modern astrometry is rapidly approaching the goal of sub-milli arcsecond precision, and although presently this precision has been achieved only for a limited number of binary stars, in the near future this will become a standard for very large number of objects. In this paper we review the representative results of techniques which have already allowed the sub-milli arcsecond precision like the optical long baseline interferometry, as well as the precursor techniques such as speckle interferometry, adaptive optics and aperture masking. These techniques provide a step forward from milli to sub-milli arcsecond precision, allowing even short period binaries to be resolved, and often resulting in orbits allowing precisions in stellar dynamical masses better than 1%. We point out that such unprecedented precisions should allow for a significant improvement of our comprehension of stellar physics and other related astrophysical topics.
{"title":"Binary star astrometry with milli and sub-milli arcsecond precision","authors":"S. Jankov, Z. Cvetkovic, R. Pavlović","doi":"10.2298/SAJ1488001J","DOIUrl":"https://doi.org/10.2298/SAJ1488001J","url":null,"abstract":"The past several decades have seen accelerating progress in improving binary \u0000 stars fundamental parameters determinations, as new observational techniques \u0000 have produced visual orbits of many spectroscopic binaries with a milli \u0000 arcsecond precision. Modern astrometry is rapidly approaching the goal of \u0000 sub-milli arcsecond precision, and although presently this precision has been \u0000 achieved only for a limited number of binary stars, in the near future this \u0000 will become a standard for very large number of objects. In this paper we \u0000 review the representative results of techniques which have already allowed \u0000 the sub-milli arcsecond precision like the optical long baseline \u0000 interferometry, as well as the precursor techniques such as speckle \u0000 interferometry, adaptive optics and aperture masking. These techniques \u0000 provide a step forward from milli to sub-milli arcsecond precision, allowing \u0000 even short period binaries to be resolved, and often resulting in orbits \u0000 allowing precisions in stellar dynamical masses better than 1%. We point out \u0000 that such unprecedented precisions should allow for a significant improvement \u0000 of our comprehension of stellar physics and other related astrophysical \u0000 topics.","PeriodicalId":48878,"journal":{"name":"Serbian Astronomical Journal","volume":"188 1","pages":"1-21"},"PeriodicalIF":0.5,"publicationDate":"2014-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://sci-hub-pdf.com/10.2298/SAJ1488001J","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"68672127","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}
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