Physical and geometrical parameters of the binary system gliese 150.2

Al-Wardat, Mashhoor A.; Balega, Yu. Yu.; Леушин, В. В.; Zuchkov, R. Ya.; Abujbha, R. M.; Al-Waqfi, Khaled; Masda, Suhail G.

doi:10.1134/s1990341314020072

Cited by 21 publications

(17 citation statements)

References 22 publications

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“…Hence, it affects the calculated mass sums strongly. Both the mass sum given by Al-Wardat et al (2014c) as 2.6 M and the photometric mass sum given by Malkov et al (2012a) as 2.67 M coincide with the dynamical mass calculated based on Hip 2007 parallax measurement. However, when we recalculate the dynamical mass based on Gaia 2018 parallax measurement, we obtain a value of 4.29 M !.…”

Section: Notes On Specific Systemssupporting

confidence: 83%

“…The rich data of Gaia DR2 are already being implemented in solving orbits and masses of binary and multiple systems, see for example Tokovinin's work (Tokovinin 2018a(Tokovinin ,b, 2019aTokovinin et al 2019;Tokovinin 2019c). It is also very useful in determining the physical and geometrical parameters of BSs, using Al-Wardat's method, which has been used to analyse several solar-type binary and triple systems (Al-Wardat 2009;Al-Wardat & Widyan 2009;Al-Wardat 2012;Al-Wardat et al 2014cMasda et al 2016;Al-Wardat et al 2017;Masda et al 2019b), and was successfully applied to subgiant BSs like HD 25811, HD 375, HD 6009 (Al-Wardat et al 2014a,b;Al-Wardat 2014) and Hip 68170 in this work.…”

Section: Discussionmentioning

confidence: 99%

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Comparison of Gaia and Hipparcos parallaxes of close visual binary stars and the impact on determinations of their masses

Al-Wardat

Hussein

Al-Naimiy

et al. 2021

Publ. Astron. Soc. Aust.

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Precise measurement of the fundamental parameters of stellar systems, including mass and radius, depends critically on how well the stellar distances are known. Astrometry from space provides parallax measurements of unprecented accuracy, from which distances can be derived, initially from the Hipparcos mission, with a further refinement of that analysis provided by van Leeuwen in 2007. The publication of the Gaia DR2 catalogue promises a dramatic improvement in the available data. We have recalculated the dynamical masses of a sample of 1 700 close visual binary stars using Gaia DR2 and compared the results with masses derived from both the original and enhanced Hipparcos data. We show the van Leeuwen analysis yields results close to those of Gaia DR2, but the latter are significantly more accurate. We consider the impact of the Gaia DR2 parallaxes on our understanding of the sample of visual binaries.

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Section: Notes On Specific Systemssupporting

confidence: 83%

Section: Discussionmentioning

confidence: 99%

Comparison of Gaia and Hipparcos parallaxes of close visual binary stars and the impact on determinations of their masses

Al-Wardat

Hussein

Al-Naimiy

et al. 2021

Publ. Astron. Soc. Aust.

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“…(13) We improve the orbit of DM91. (14) First SB orbit; the star was already a VB with known orbital elements (Al-Wardat et al 2014). (15) Orbit derived taking into account 15 Elodie measurements found in the Elodie Archive; the offset of the Elodie RVs is −0.193 km s −1 .…”

Section: Appendix A: Tables Of Mean Rvs and Of Orbital Elementsmentioning

confidence: 99%

Multiplicity among solar-type stars

Halbwachs

Mayor

Udry

2018

A&A

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Context. The statistical properties of binary stars are clues for understanding their formation process. A radial velocity survey was carried on amongst nearby G-type stars and the results were published in 1991. Aims. The survey of radial velocity measurements was extended towards K-type stars. Methods. A sample of 261 K-type stars was observed with the spectrovelocimeter CORAVEL (COrrelation RAdial VELocities). Those stars with a variable radial velocity were detected on the basis of the P( χ 2 ) test. The orbital elements of the spectroscopic binaries were then derived. Results. The statistical properties of binary stars were derived from these observations and published in 2003. We present the catalogue of the radial velocity measurements obtained with CORAVEL for all the K stars of the survey and the orbital elements derived for 34 spectroscopic systems. In addition, the catalogue contains eight G-type spectroscopic binaries that have received additional measurements since 1991 and for which the orbital elements are revised or derived for the first time.

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“…The method was firstly introduced by Al-Wardat (2002a, 2007)(henceforth paper I and paper II in this series respectively), where it was applied to the analysis of the quadruple hierarchical system ADS11061 and the two binary systems COU1289 and COU1291 . Later on, the method was successfully applied to several solar-type and subgiant binary systems: Hip11352, Hip11253 and Hip689 Al-Wardat (2009);Al-Wardat & Widyan (2009); Al-Wardat (2012) (henceforth papers III, IV and V in this series respectively).…”

Section: Introductionmentioning

confidence: 99%

Physical and geometrical parameters of CVBS X: the spectroscopic binary Gliese 762.1

Masda¹,

Al-Wardat

Neuhäuser³

et al. 2016

Res. Astron. Astrophys.

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We present the physical and geometrical parameters of the individual components of the close visual double-lined spectroscopic binary system Gliese 762.1, which were estimated using Al-Wardat's complex method for analyzing close visual binary systems. The estimated parameters of the individual components of the system are as follows: radius R A = 0.845 ± 0.09R ⊙ , R B = 0.795 ± 0.10R ⊙ , effective temperature T A eff = 5300 ± 50 K, T B eff = 5150 ± 50 K, surface gravity log g A = 4.52 ± 0.10, log g B = 4.54 ± 0.15 and luminosity L A = 0.51 ± 0.08L ⊙ , L B = 0.40 ± 0.07L ⊙ . New orbital elements are presented with a semi-major axis of 0.0865 ± 0.010 arcsec using the Hippracos parallax π = 58.96 ± 0.65 mas, and an accurate total mass and individual masses of the system are determined as M = 1.72 ± 0.60M ⊙ , M A = 0.89 ± 0.08M ⊙ and M B = 0.83 ± 0.07M ⊙ . Finally, the spectral types and luminosity classes of both components are assigned as K0V and K1.5V for the primary and secondary components respectively, and their positions on the H-R diagram and evolutionary tracks are given.

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Physical and geometrical parameters of the binary system gliese 150.2

Cited by 21 publications

References 22 publications

Comparison of Gaia and Hipparcos parallaxes of close visual binary stars and the impact on determinations of their masses

Comparison of Gaia and Hipparcos parallaxes of close visual binary stars and the impact on determinations of their masses

Multiplicity among solar-type stars

Physical and geometrical parameters of CVBS X: the spectroscopic binary Gliese 762.1

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