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14 Andromedae b

Extrasolar planet in Andromeda constellation

Field	Value
name	14 Andromedae b / Spe
image	14 And b rv.pdf
caption	Radial velocity changes over time of 14 Andromedae caused by the orbit of 14 Andromedae b.
discovery_ref
discoverer	Sato et al.
discovery_site	Okayama Planet
Search Program
discovered	July 2, 2008
discovery_method	Doppler Spectroscopy
extrasolarplanet	yes
named_after	"spe" from latin "spes" meaning hope
alt_names	Spe
orbit_ref
apsis	astron
semimajor	0.775 AU
eccentricity	0.0094
period
time_periastron
semi-amplitude
star	[14 Andromedae](14-andromedae)
physical_ref
mass

Search Program](okayama-planet-search-program) | semi-amplitude =

14 Andromedae b (abbreviated 14 And b), formally named Spe , is a candidate exoplanet approximately 248 light-years away in the constellation of Andromeda.

The 186-day period planet orbits about 83% the Earth-Sun distance from the giant star 14 Andromedae. It has a minimum mass of 3.559 times the mass of Jupiter. The planet orbits with an eccentricity of 0.0094, which means the orbital distance over the course of its revolution varies by only 0.02 AU.

Nomenclature

In July 2014 the International Astronomical Union launched NameExoWorlds, a process for giving proper names to certain exoplanets and their host stars. The process involved public nomination and voting for the new names. In December 2015, the IAU announced the name Spe for this planet. The winning name was based on that submitted by the Thunder Bay Centre of the Royal Astronomical Society of Canada); namely 'Spes', Latin for 'hope'. (Spes was also the Roman goddess of hope.) The IAU substituted the ablative form 'Spe', which means 'where there is hope', to match that given to the host star at the same time.

Discovery

The preprint announcing 14 Andromedae b was submitted to the arXiv electronic repository on July 2, 2008, by Bun'ei Sato and collaborators, who discovered it using the Doppler Spectroscopy method, during the Okayama Planet Search radial velocity survey of G and K giants at Okayama Astrophysical Observatory.

Planet challenged

A 2023 study of planets around evolved stars, while presenting updated parameters for this planet, found that the radial velocity variations are correlated with stellar activity signals, casting doubt on the planet's existence. Based on this, a 2024 study listed it as one of several doubtful planets around giant stars (along with the other named planets 41 Lyncis b and 42 Draconis b).

References

[http://www.iau.org/news/pressreleases/detail/iau1404/ NameExoWorlds: An IAU Worldwide Contest to Name Exoplanets and their Host Stars]. IAU.org. 9 July 2014
"NameExoWorlds The Process".
[http://www.iau.org/news/pressreleases/detail/iau1514/ Final Results of NameExoWorlds Public Vote Released], International Astronomical Union, 15 December 2015.
[http://www.tbrasc.org/centre-news/ Thunder Bay Amateur Astronomers Name a Planet]
"NameExoWorlds The Approved Names".
(2008). "Planetary Companions to Evolved Intermediate-Mass Stars: 14 Andromedae, 81 Ceti, 6 Lyncis, and HD167042". Publications of the Astronomical Society of Japan.
(August 2023). "Revisiting planetary systems in the Okayama Planet Search Program: A new long-period planet, RV astrometry joint analysis, and a multiplicity-metallicity trend around evolved stars". [[Publications of the Astronomical Society of Japan]].
(September 2024). "Non-radial oscillations mimicking a brown dwarf orbiting the cluster giant NGC 4349 No. 127". [[Astronomy & Astrophysics]].

Info: Wikipedia Source

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