SPECKLE INTERFEROMETRY AND ORBITS OF “FAST” VISUAL BINARIES

By A. Tokovinin. 2012

228 citations recorded by the source corpus.

Results of speckle observations at the 4.1 m SOAR telescope in 2012 (158 measures of 121 systems, 27 non-resolutions) are reported. The aim is to follow fast orbital motion of recently discovered or neglected close binaries and sub-systems. Here, eight previously known orbits are defined better, two more are completely revised, and five orbits are computed for the first time. Using differential photometry from Hipparcos or speckle and the standard relation between mass and absolute magnitude, the component's masses and dynamical parallaxes are estimated for all 15 systems with new or updated orbits. Two astrometric binaries HIP 54214 and 56245 are resolved here for the first time, another eight are measured. We highlight several unresolved pairs that may actually be single despite multiple historic measures, such as 104 Tau and f Pup AB. Continued monitoring is needed to understand those enigmatic cases.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/b12df15ceb850933ec1a774ea2dccd41647a8fc8

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Citations in the corpus

Speckle Interferometry at SOAR in 2016 and 2017 (2014, background): “This paper continues the series published by Tokovinin, Mason, & Hartkopf (2010a, hereafter TMH10), Tokovinin et al. (2010b), Hartkopf et al. (2012), Tokovinin (2012), Tokovinin et al. (2014), Tokovinin et al. (2015, hereafter SOAR14), and Tokovinin et al. (2016a).”
SPECTROSCOPIC ORBITS FOR 15 LATE-TYPE STARS (2016, methodology): “In agreement with the magnitude difference D =y 3.5 mag from Tokovinin (2012), these values of M1 and M2 indicate that the secondary would be about 3.4 mag fainter than the primary.”
Multiplicity among Solar-type Stars (2017, methodology): “For this astrometric, spectroscopic, and visual binary with a 10.5 year period (Abt &Willmarth 2006; Tokovinin 2012; Jenkins et al. 2015; Willmarth et al. 2016), spectroscopically resolved observations are only possible for a small part of its eccentric orbit, the next window being around the year…”