ORBITS FOR EIGHTHIPPARCOSDOUBLE STARS

Abstract

In this paper, we analyze new orbital elements and the quantities that follow from them for eight binaries: WDS 00101+3825 = HDS 23Da,Db, WDS 00321−1218 = HDS 71, WDS 04287+2613 = HDS 576, WDS 04389−1207 = HDS 599, WDS 16206+4535 = HDS 2309, WDS 17155+1052 = HDS 2440, WDS 22161−0705 = HDS 3158, and WDS 23167+3441 = HDS 3315. For seven of them, the orbital elements are calculated for the first time. Binaries, denoted as HDS, were discovered during the Hipparcos mission, and their first observational epoch is 1991.25, the same as the mean epoch of the Hipparcos catalog. We found all other measurements of these binaries in databases. They were obtained in the last 15 yr using the speckle interferometric technique. All studied pairs are close, and all measured separations are less than 0. 4. The resulting orbital periods fall within 26 and 80 yr. In addition to the orbital elements, we also give (O − C) residuals in θ and ρ, masses, dynamical parallaxes, absolute magnitudes, spectral types, and ephemerides for the next 5 yr.

ARMADA. II. Further Detections of Inner Companions to Intermediate-mass Binaries with Microarcsecond Astrometry at CHARA and VLTI

“…HD 29573 (HIP 21644) is a bright A-type star that was discovered to be a binary by the Hipparcos mission (van Leeuwen 2007). Cvetković et al (2014) characterized its binary orbit further with newly obtained speckle data. Despite the low number of data points on the 40 yr period, they were able to compute a dynamical mass of 4.99 ± 0.73 M e , which was somewhat consistent within error bars with the photometric mass obtained from the spectral types of the two stars in the system-spectral types A1 and F2 (corresponding to a photometric system mass of 3.84 M e ).…”

Spectroscopic Orbits of Subsystems in Multiple Stars. III.

“…This is a slightly metal-deficient G5V star with a fast PM, G27-21. The binary system A,B was discovered by Hipparcos (HDS 3158), and its first visual orbit with P = 80.6 year was computed by Cvetkovic et al (2014). Latham et al (2002) found that the RV is changing slowly, presumably owing to the motion in the visual orbit.…”

Orbits and masses of binaries from Speckle Interferometry at SOAR

“…HDS2440=WDS17155+1052: Nice orbit and good phase coverage. Our observations led to a small change of the orbital elements compared to Cvetković et al (2014). Could be promoted to grade 2.…”