Talk:44 Boötis
 | This article is rated Start-class on Wikipedia's content assessment scale. It is of interest to the following WikiProjects: | |||||||||||||
| ||||||||||||||
.jpg){kind=small}
Excised section about possible companion[edit]
I have excised the below section from the article as it gives undue weight to a single conference poster [1] that has never subsequently been referred to in the literature (ADS shows 0 citations [2]). Especially given the apparent instability of the orbit which casts doubt on the reality of the object, this claim is neither notable nor plausible. 77.57.25.250 (talk) 10:11, 1 May 2014 (UTC)
- Probably for the best. Praemonitus (talk) 05:04, 13 May 2019 (UTC)
A substellar companion?[edit]
Recent analysis in timing variations for 44 Bootis B would suggest the presence of a third body orbiting the W Ursae Majoris-type eclipsing binary with likely substellar mass.[1] Its minimum mass is estimated at 48 times that of Jupiter and the orbital separation at 10.73 AUs (a bit farther away than Saturn in the Solar System). So far unconfirmed, such an object seems unstable considering the system's architecture, with 44 Bootis B-C getting as close as 26.6 AUs to 44 Bootis A,[2] unless it is locked in some kind of peculiar configuration and inclination.
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (years) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b (unconfirmed) | ≥47.5 MJ | 10.73 | ≈35 | ? | — | — |
References
- ^ a b Byrd-Fisher; et al. (2008). "Patterns in the Long Term Behavior of Eclipsing Binary Star System 44i-Bootis". American Physical Society, 10th Annual Meeting of the Northwest Section of APS, May 15–17, 2008. Bibcode:2008APS..NWS.C1013B.
{{cite journal}}: Explicit use of et al. in:|author=(help) - ^ Heintz (1997). "Orbits of 40 Visual Binaries". Astrophysical Journal Supplement. 111: 1–4. Bibcode:1997ApJS..111..335H. doi:10.1086/313011.