Talk:HD 43587
 | This article is rated Start-class on Wikipedia's content assessment scale. It is of interest to the following WikiProjects: | |||||||||||||
| ||||||||||||||
.jpg){kind=small}
INFO DUMP
[edit]As referenced for over a decade in literature, HD 43587 (A) was a CoRoT main-sequence astroseismology target. A relevant paper appeared recently, though there are many more.
The system is quadruple, though apparently most literature didn't pick up on the fourth component.
- Component A (F9V) is a spectroscopic binary, detected by Vogt et al. 2002 in the Keck planet search. Adaptive optics and speckle interferometry has resolved the components, finding that Ab is a late K- or early M-dwarf.
- Four companions are listed in the WDS. Companion A has been observed 11 times and is very slowly moving, while B and C have only been observed once in 1911, making A unphysical and BC unlikely to be bound or real. Companion E (NLTT 16333, 2MASS J06171064+0507024), however, has very similar proper motions to A, and is therefore bound. This component is referred to by various designations, mostly Gliese 231.1 B, though HD 43587 B should be valid (because The primary binary is Aab).
- Component B is an M-dwarf. Well, not quite, because it's a binary consisting of two late M-dwarfs. Confusingly, SIMBAD has adopted Gliese 231.1 BC as different to NLT 16333 because of the number of decimal points used in that paper, but they are referring to the same object.
Kozai oscillations could be responsible for Ab's eccentricity, but this is tentative because the distribution of stellar eccentricities can typically go upwards of 0.9 without peturbation.
Hoy. It's no Sigma Coronae Borealis, but this system took several hours for me to figure out.