14 Andromedae b
{{Short description|Extrasolar planet in Andromeda constellation}}
{{Infobox planet
| 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.
| 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
| apsis = astron
| semimajor = {{convert|0.775|AU|km|abbr=on}}
| eccentricity = 0.0094
| period = {{val|186.76|0.11|0.12|ul=d}}
| time_periastron = {{val|2452853.0|2.1}}
| semi-amplitude = {{val|86.08|2.76|2.95|ul=m/s}}
| star = 14 Andromedae
| mean_radius = 1.16 times jupiters
| mass = {{val|3.559|0.114|0.122|p=≥|ul=Jupiter mass}}
| density = 0.7217 g/cm^3
}}
14 Andromedae b (abbreviated 14 And b), formally named Spe {{IPAc-en|'|s|p|iː}}, 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 4.8 times the mass of Jupiter. And a estimated radius of 1.16 times Jupiter{{Cite web |date=2019-04-22 |title=14 Andromedae b - NASA Science |url=https://science.nasa.gov/exoplanet-catalog/14-andromedae-b/ |access-date=2025-04-11 |language=en-US}}. 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.[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 The process involved public nomination and voting for the new names.{{Cite web |url=http://nameexoworlds.iau.org/process |title=NameExoWorlds The Process |access-date=2015-09-05 |archive-date=2015-08-15 |archive-url=https://web.archive.org/web/20150815025117/http://www.nameexoworlds.iau.org/process |url-status=dead }} In December 2015, the IAU announced the name Spe for this planet.[http://www.iau.org/news/pressreleases/detail/iau1514/ Final Results of NameExoWorlds Public Vote Released], International Astronomical Union, 15 December 2015. The winning name was based on that submitted by the Thunder Bay Centre of the Royal Astronomical Society of Canada[http://www.tbrasc.org/centre-news/ Thunder Bay Amateur Astronomers Name a Planet]); 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.{{Cite web |url=http://nameexoworlds.iau.org/names |title=NameExoWorlds The Approved Names |access-date=2015-12-17 |archive-date=2018-02-01 |archive-url=https://web.archive.org/web/20180201043609/http://nameexoworlds.iau.org/names |url-status=dead }}
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).
See also
References
{{Reflist|refs=
{{cite journal |last1=Teng |first1=Huan-Yu |last2=Sato |first2=Bun'ei |display-authors=etal |date=August 2023 |title=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 |journal=Publications of the Astronomical Society of Japan |volume=75 |issue=6 |pages=1030–1071 |doi=10.1093/pasj/psad056 |arxiv=2308.05343 |bibcode=2023PASJ...75.1030T}}
{{cite journal |last1=Spaeth |first1=Dane |last2=Reffert |first2=Sabine |display-authors=etal |date=September 2024 |title=Non-radial oscillations mimicking a brown dwarf orbiting the cluster giant NGC 4349 No. 127 |journal=Astronomy & Astrophysics |volume=689 |issue= |pages=A91 |doi=10.1051/0004-6361/202450163 |arxiv=2407.21583 |bibcode=2024A&A...689A..91S}}
}}
External links
- {{cite web | url=http://media4.obspm.fr/exoplanets/base/etoile.php?nom=14+And | title=14 Andromedae | work=Exoplanets | access-date=2008-08-06 | archive-url=https://web.archive.org/web/20091125004955/http://media4.obspm.fr/exoplanets/base/etoile.php?nom=14+And | archive-date=2009-11-25 | url-status=dead }}
- {{cite web |url=https://exoplanet.eu/catalog/14_and_b--489/ |title=Notes for Planet 14 And b |author=Jean Schneider |year=2011 |work=Extrasolar Planets Encyclopaedia |access-date=30 September 2011}}
{{Andromeda (constellation)}}
Category:Andromeda (constellation)
Category:Exoplanets discovered in 2008