Precise Masses, Ages, and Orbital Parameters of the Binary Systems HIP 11352, HIP 70973, and HIP 72479

Al-Tawalbeh, Y. M.; Hussein, Abdallah M.; Taani, Ali; Abushattal, A. A.; Yusuf, N.A.; Mardini, Mohammad K.; Suleiman, Firas Ahmad; Al-Naimiy, Hamid M. K.; Khasawneh, Awni; Al-Wardat, Mashhoor A.

doi:10.1134/s199034132101003x

Cited by 15 publications

(9 citation statements)

References 57 publications

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“…Atmospheric and fundamental parameters of the components of BMSs have been estimated using Al-Wardat's method Al-Wardat et al (2021a). The method was successfully used to accurately analyze several BMSs (see, e.g., Al-Wardat 2002, 2009a, 2009bAl-Wardat et al 2014a, 2014b, 2016Masda et al 2016;Al-Wardat et al 2017;Masda et al 2018Masda et al , 2019aMasda et al , 2019bAl-Tawalbeh et al 2021;Yousef et al 2021;Al-Wardat et al 2021b). It has been shown to be an effective tool for investigating the accuracy of the measured trigonometric parallaxes by the Hipparcos and Gaia astrometric missions.…”

Section: Methodsmentioning

confidence: 99%

Atmospheric and Fundamental Parameters of Eight Nearby Multiple Stars

Hussein

Al-Wardat

Abushattal

et al. 2022

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We present the complete set of atmospheric and fundamental parameters, in addition to the masses, for the individual components of eight stellar systems. The list of the systems, whose orbital solutions were published recently, includes seven binaries (HIP 14524, HIP 16025, HIP 46199, HIP 47791, HIP 60444, HIP 61100, HIP 73085) and one triple system (HIP 28671). The systems were analyzed using a spectrophotometric computational technique known as Al-Wardats method for analyzing binary and multiple stellar systems, which makes use of ATLAS9 line-blanketed plane-parallel model atmospheres. Using these estimated parameters, the positions of the components were located on the Hertzsprung–Russell diagram, evolutionary tracks and isochrones to estimate their ages, the range depending on the uncertainties in their metallicities. Five systems were found to be pre-main-sequence stars (HIP 14524, HIP 46199, HIP 60444, HIP 61100, HIP 73085), two were main-sequence stars (the zero-age HIP 28671 and the 6.3 Gyr HIP 16025), and one is a subgiant system (HIP 47791) with an age of 1.4 Gyr. Fragmentation is proposed as the most probable formation process for the eight systems. A comparison between the estimated masses and the dynamical ones lead to new dynamical parallaxes for four systems: (28.63 ± 0.56) mas for HIP 14524, (15.6 ± 0.63) mas for HIP 16025, (9.73 ± 0.26) mas for HIP 47791, and (16.53 ± 0.59) mas for HIP 73085. Hence, the orbital solutions were reclassified. We conclude that Gaia DR3 parallaxes are more precise than those given by Gaia DR2 and Hipparcos 2.

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Section: Methodsmentioning

confidence: 99%

Atmospheric and Fundamental Parameters of Eight Nearby Multiple Stars

Hussein

Al-Wardat

Abushattal

et al. 2022

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“…The latest visual orbit included in Orb6 is that from Docobo et al (2018a), but more recently Al-Tawalbeh et al (2021) has revised this solution, and obtained a system's mass of 1.61 ± 0.26 M , and an orbital parallax of 21.81 ± 0.8 mas. These results lie within 1σ of our derived values, albeit our combined solution yields much smaller formal uncertainties, due in part to our combined solution and also to the addition of three new HRCam+SOAR measurements in 2018.16, 2019.14, and 2019.54.…”

Section: Wds 14492+1013=a2983mentioning

confidence: 99%

Orbital elements and individual component masses from joint spectroscopic and astrometric data of double-line spectroscopic binaries

Anguita-Aguero,

Mendez,

Claveria

et al. 2022

Preprint

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We present orbital elements, orbital parallaxes and individual component masses, for fourteen spatially resolved double-line spectroscopic binaries derived doing a simultaneous fit of their visual orbit and radial velocity curve. This was done by means a Markov Chain Monte Carlo code developed by our group, which produces posterior distribution functions and error estimates for all the parameters. Of this sample, six systems had high quality previous studies and were included as benchmarks to test our procedures, but even in these cases we could improve the previous orbits by adding recent data from our survey of southern binaries being carried out with the HRCam and ZORRO speckle cameras at the SOAR 4.1m and Gemini South 8.1m telescopes, respectively. We also give results for eight objects that did not have a published combined orbital solution, one of which did not have a visual orbit either. We could determine mass ratios with a typical uncertainty of less than 1%, mass sums with uncertainties of about 1% and individual component masses with a formal uncertainty of 0.01M in the best cases. A comparison of our orbital parallaxes with available trigonometric parallaxes from Hipparcos and Gaia eDR3, shows a good correspondence; the mean value of the differences being consistent with zero within the errors of both catalogs. We also present observational HR diagrams for our sample of binaries, which in combination with isochrones from different sources allowed us to asses their evolutionary status of and also the quality of their photometry.

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“…Also available are luminosity, parallaxes, sizes, and orbital elements, which can be used to evaluate parameters of interests, and orbital elements. (Al-Tawalbeh et al, 2021, Docobo et al, 2018, Hussein et al, 2022.…”

Section: Introductionmentioning

confidence: 99%

The Precise Individual Masses and Theoretical Stability and Habitability of some Single-lined Spectroscopic Binaries

Algnamat¹,

Abushattal²,

Kraishan³

et al. 2022

ComBAO

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Over the past few decades, some Spectroscopic Binaries (SBs) have been resolved using high-resolution techniques. Astrophysics is interested in this subject because we can obtain the mass of each component. By combining a visual solution with a complimentary one, such as the spectroscopic orbit or Edward method, we can determine the individual masses, semimajor axes, magnitudes, spectral types, radii, and temperatures. These provide the most probable physical parameters for some single-lined spectroscopic binaries. Then We can use these parameters to calculate theoretical the stability and habitability of the system. Additionally, we assume the composite spectrum, the apparent global magnitude, and the parallax (generally the Hipparcos, and recently the Gaia ). The next step is to obtain the spectrum for each components. The Edwards method will be used in this case. As soon as we have two spectra foe two single-lined spectroscopic binaries (HIP 754 and HIP 3841), we can determine each mass based on the magnitude difference, ∆m. For selected samples, we calculate the rest of the physical parameters needed to calculate the theoretical stability and habitability.

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Precise Masses, Ages, and Orbital Parameters of the Binary Systems HIP 11352, HIP 70973, and HIP 72479

Cited by 15 publications

References 57 publications

Atmospheric and Fundamental Parameters of Eight Nearby Multiple Stars

Atmospheric and Fundamental Parameters of Eight Nearby Multiple Stars

Orbital elements and individual component masses from joint spectroscopic and astrometric data of double-line spectroscopic binaries

The Precise Individual Masses and Theoretical Stability and Habitability of some Single-lined Spectroscopic Binaries

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