J. F. Ling

ICCD SPECKLE OBSERVATIONS OF BINARY STARS. XXIII. MEASUREMENTS DURING 1982¨1997 FROM SIX TELESCOPES, WITH 14 NEW ORBITS

We present 2017 observations of 1286 binary stars, observed by means of speckle interferometry using six telescopes over a 15 year period from 1982 April to 1997 June. These measurements constitute the 23d installment in CHARAs speckle program at 2 to 4 m class telescopes and include the second major collection of measurements from the Mount Wilson 100 inch (2.5 m) Hooker Telescope. Orbital elements are also presented for 14 systems, seven of which have had no previously published orbital analyses.

Orbits and System Masses of 14 Visual Double Stars with Early-Type Components

This paper presents revised orbits and system masses of 14 visual double stars, in all of which at least one component is of early spectral type: WDS 00546+1911 (STT 20 AB), WDS 01040+3528 (HO 213), WDS 02039+4220 (STT 38 BC), WDS 03503+2535 (STT 65), WDS 06393+4200 (STT 150), WDS 08285-0231 (A551 AB), WDS 15088-4517 (SEE 219 AB), WDS 15416+1940 (HU 580 AB), WDS 16514+0113 (STT 315), WDS 17104-1544 (BU 1118 AB), WDS 19172-6640 (GLE 3), WDS 19411+1349 (KUI 93), WDS 22241-0450 (BU 172 AB), and WDS 23382+5514 (A1493). Star masses were calculated from Hipparcos parallax data whenever the precision was good enough (10 cases); otherwise, dynamical parallaxes were used, except in one case involving component multiplicity. Other physical and orbital properties of these stars are also discussed.

Orbits and masses of twenty double stars discovered by Paul Couteau

In this article we present the orbits and masses of 20 double stars discovered by P. Couteau at the Nice Observatory (France), namely WDS 01450+2703 (COU 750), 03321+4340 (1688), 03423+3141 (691), 06503+2409 (768), 12409+2708 (596), 14138+3059 (606), 15390+2545 (612), 16584+3943 (1289), 17075+3810 (1291), 17221+2310 (415), 18035+ 4032 (1785), 18043+4206 (1786), 19089+3404 (1462), 19180+2012 (321), 20151+3742 (2416), 20216+1930 (327 AB), 21593+4606 (2138), 22077+2622 (537), 22307+1758 (234) and 23199+2844 (439). For two of these stars, COU 750 and COU 1289, these are the first orbits to be published other than IAU Circulars; for the others, previously published orbits are improved on by those presented here. Star masses were in fifteen cases calculated from Hipparcos parallax data, and in the other five from dynamical parallaxes; in all cases, the error is estimated. Some of the other physical and orbital properties of these stars are also discussed.

Orbits of Five Visual Double Stars

This paper revises and discusses the orbits and other parameters of the double stars WDS 01497-1414, WDS 05413+1632, WDS 11136+5525, WDS 20311+3333, and WDS 20494+1124.

Preliminary Orbits for Eight Visual Binaries

This paper reports orbits and masses calculated for the visual binary stars WDS 00427-6537 (I440), WDS 01084-5515 (RST 1205 AB), WDS 01343-0827 (A314), WDS 03590+0947 (HU 27), WDS 10287+4558 (A1993), WDS 12429+0516 (A1602), WDS 20157+4339 (A2095 AB), and WDS 22180-6249 (I20). All the orbits have previously been announced in IAU Commission 26 Information Circulars; for all except WDS 20157+4339, they are the first orbits to have been published. They are accompanied by ephemerides, residuals with respect to observations, and figures of the apparent orbits. Masses (calculated using both Hipparcos and dynamic parallax data, except for WDS 20157+4339, for which no Hipparcos data are available) are accompanied by estimates of uncertainty. Features of the orbits and physical properties are discussed.

Orbits of Visual Binaries WDS 13320+3109, 14310−0548, 14492+1013, and 16384+3514

Revised orbits and dynamical data of visual binaries WDS 13320+3109, 14310-0548, 14492+1013, and 16384+3514 are presented. For all systems but WDS 16384+3514, the total mass is derived. Some astrophysical properties of the stars are discussed as well.

FIRST ORBIT SOLUTIONS AND CALCULATED MASSES OF 10 VISUAL BINARIES

This paper presents the first reported orbits and masses of 10 visual double stars, all of which have described arcs of less than 180° since the first observation: WDS 00209+1059 (BU 1093), WDS 02405 – 2408 (SEE 19), WDS 05289 – 0318 (DA 6), WDS 07347+3852 (HU 842 AB), WDS 07546 – 0248 (STF 1157), WDS 08127+2613 (A 2471), WDS 08456+8442 (A 1078), WDS 23072+6050 (BU 180 AB), WDS 23103+3229 (BU 385), and WDS 23175+1652 (HU 497 BC). Masses were calculated from updated Hipparcos parallax data when available and sufficiently precise, and from dynamical parallaxes otherwise. Other physical and orbital properties are also discussed.

Binary Star Speckle Interferometry: Measurements and Orbits

Results of our second observational run of binary star interferometric measurements with an ICCD speckle camera attached to the 1.52 m telescope of the Observatorio Astronomico Nacional at Calar Alto (Almeria, Spain) in 2000 June–July are presented. The measured angular separations range from 0096 to 6558. With the use of the new speckle data, the orbits of the visual binaries WDS 14369+4813 and WDS 21597+4908 are improved.

The Influence of Mass Loss on The Eccentricity of Double Star Orbits

In this comunication we study the behaviour of the eccentricity of double star orbits (visual and wide spectroscopic binaries) according to simplified laws of mass loss. Applications to the systems WDS 05245S0224 - HD 35411, WDS 05387S0236 - HD 37468 and WDS 06154S0902 - HD 43362 are included.

Binary stars with late‐type components: 6 orbits and system masses

Revised orbits and system masses are presented for the following 6 visual double stars: WDS 01259‐4754 (RST 33), WDS 16057‐3252 (SEE 264), WDS 17575+1058 (BU 1299 AB), WDS 19471‐0809 (A 108), WDS 21000+4004 (KUI 103), and WDS 22329+5348 (KUI 112 Aa). In all of these systems, at least one component is of the late‐type and the latest observations were made using speckle or CCD techniques. Total system masses were calculated in each case from the orbital period and semiaxis major together with the updated Hipparcos parallax, except in the cases for which there were no Hipparcos data or when these values were not precise.