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Coordinates: Sky map 21h 00m 06.1969s, −05° 05′ 40.0370″
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NameExoWorlds
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| epoch = J2000
| epoch = J2000
| constell = [[Aquarius (constellation)|Aquarius]]
| constell = [[Aquarius (constellation)|Aquarius]]
| ra = {{RA|21|00|06.1969}}<ref name=SIMBAD/>
| ra = {{RA|21|00|06.19682}}<ref name=GaiaDR3/>
| dec = {{DEC|-05|05|40.0370}}<ref name=SIMBAD/>
| dec = {{DEC|-05|05|40.0349}}<ref name=GaiaDR3/>
| appmag_v = 9.87{{±|0.03}}<ref name=Anderson2013/>
| appmag_v = 9.87{{±|0.03}}<ref name=Anderson2013/>
}}
}}
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}}
}}
{{Starbox astrometry
{{Starbox astrometry
| radial_v = −9.372<ref name=EDR3>{{cite Gaia EDR3|6910753016653587840}}</ref>
| radial_v = {{val|−9.83|0.13}}<ref name=GaiaDR3/>
| prop_mo_ra = 33.778<ref name=EDR3/>
| prop_mo_ra = 33.778
| prop_mo_dec = −93.581<ref name=EDR3/>
| prop_mo_dec = −93.581
| pm_footnote = <ref name=GaiaDR3/>
| parallax = 19.8858
| parallax = 19.8858
| p_error = 0.0170
| p_error = 0.0170
| parallax_footnote = <ref name=EDR3/>
| parallax_footnote = <ref name=GaiaDR3/>
}}
}}
{{Starbox detail
{{Starbox detail
| mass = 0.826{{±|0.029}}<ref name=Anderson2013/>
| mass = 0.826{{±|0.029}}<ref name=Anderson2013/>
| radius = 0.813<ref name=Anderson2013/>
| radius = 0.813<ref name=Anderson2013/>
| temperature = 4782{{±|15}}<ref name=Gill2018/>
⚫
| temperature = 4782{{±|15}}<ref name=Gill2018>{{citation|arxiv=1801.06106|title=The atmospheric parameters of FGK stars using wavelet analysis of CORALIE spectra|year=2018|doi=10.1051/0004-6361/201731954|last1=Gill|first1=S.|last2=Maxted|first2=P. F. L.|last3=Smalley|first3=B.|journal=Astronomy & Astrophysics|volume=612|pages=A111|bibcode=2018A&A...612A.111G|s2cid=119331772}}</ref>
| luminosity =
| luminosity =
| gravity = 4.59{{±|0.02}}<ref name=Gill2018/>
| gravity = 4.59{{±|0.02}}<ref name=Gill2018/>
Line 34: Line 35:
}}
}}
{{Starbox catalog
{{Starbox catalog
| names = {{odlist|BD=−05 5432|2MASS = J21000618-0505398|GSC=05200-01560|TYC=5200-1560-1}}<ref name=SIMBAD>{{cite simbad|title=BD-05 5432|access-date=2021-01-08}}</ref>
| names = {{odlist | name = Wouri | BD=−05 5432 | 2MASS = J21000618-0505398 | GSC=05200-01560 | TYC=5200-1560-1 | WASP = 69}}<ref name=SIMBAD/>
}}
}}
{{Starbox reference
{{Starbox reference
Line 41: Line 42:
{{Starbox end}}
{{Starbox end}}


'''WASP-69''' is a [[K-type main-sequence star]]. Its surface temperature is 4782{{±|15}} [[Kelvin|K]]. WASP-69 is slightly enriched in heavy elements compared to the [[Sun]], with a [[metallicity]] Fe/H index of 0.10{{±|0.01}},<ref name=Gill2018/> and is much younger than the Sun at 2 billion years. The data regarding [[starspot]] activity of WASP-69 are inconclusive, but spot coverage of the [[photosphere]] may be very high.<ref name=Murgas2020/>
'''WASP-69''' is a [[K-type main-sequence star]] {{convert|164|ly|pc|lk=on|abbr=off}} away. Its surface temperature is 4782{{±|15}} [[Kelvin|K]]. WASP-69 is slightly enriched in heavy elements compared to the [[Sun]], with a [[metallicity]] Fe/H index of 0.10{{±|0.01}},<ref name=Gill2018/> and is much younger than the Sun at 2 billion years. The data regarding [[starspot]] activity of WASP-69 are inconclusive, but spot coverage of the [[photosphere]] may be very high.<ref name=Murgas2020/>


Multiplicity surveys did not detect any stellar companions to WASP-69 as of 2020.<ref>{{citation|arxiv=2001.08224|year=2020|title=A multiplicity study of transiting exoplanet host stars. I. High-contrast imaging with VLT/SPHERE|doi=10.1051/0004-6361/201937127|last1=Bohn|first1=A. J.|last2=Southworth|first2=J.|last3=Ginski|first3=C.|last4=Kenworthy|first4=M. A.|last5=Maxted|first5=P. F. L.|last6=Evans|first6=D. F.|journal=Astronomy & Astrophysics|volume=635|pages=A73|bibcode=2020A&A...635A..73B|s2cid=210861118}}</ref>
Multiplicity surveys did not detect any stellar companions to WASP-69 as of 2020.<ref>{{citation|arxiv=2001.08224|year=2020|title=A multiplicity study of transiting exoplanet host stars. I. High-contrast imaging with VLT/SPHERE|doi=10.1051/0004-6361/201937127|last1=Bohn|first1=A. J.|last2=Southworth|first2=J.|last3=Ginski|first3=C.|last4=Kenworthy|first4=M. A.|last5=Maxted|first5=P. F. L.|last6=Evans|first6=D. F.|journal=Astronomy & Astrophysics|volume=635|pages=A73|bibcode=2020A&A...635A..73B|s2cid=210861118}}</ref>

==Nomenclature==
The designation ''WASP-69'' indicates that this was the 69th star found to have a planet by the [[Wide Angle Search for Planets]].

⚫
In August 2022, this planetary system was included among 20 systems to be named by the third [[NameExoWorlds]] project.<ref>{{cite web |url=https://www.nameexoworlds.iau.org/2022exoworlds |title=List of ExoWorlds 2022 |date=8 August 2022 |website=nameexoworlds.iau.org |publisher=[[International Astronomical Union|IAU]] |access-date=27 August 2022}}</ref> The approved names, proposed by a team from [[Cameroon]], were announced in June 2023. WASP-69 is named '''Wouri''' and its planet is named '''Makombé''', after the [[Wouri River|Wouri]] and [[Makombé River|Makombé]] rivers.<ref name="NEW2022"/>


==Planetary system==
==Planetary system==
In 2013, one planet, named [[WASP-69b]], was discovered on a tight, circular orbit.<ref name=Anderson2013>{{citation|arxiv=1310.5654|title=Three sub-Jupiter-mass planets: WASP-69b & WASP-84b transit active K dwarfs and WASP-70Ab transits the evolved primary of a G4+K3 binary|year=2013|doi=10.1093/mnras/stu1737|last1=Anderson|first1=D. R.|last2=Collier Cameron|first2=A.|last3=Delrez|first3=L.|last4=Doyle|first4=A. P.|last5=Faedi|first5=F.|last6=Fumel|first6=A.|last7=Gillon|first7=M.|last8=Gómez Maqueo Chew|first8=Y.|last9=Hellier|first9=C.|last10=Jehin|first10=E.|last11=Lendl|first11=M.|last12=Maxted|first12=P. F. L.|last13=Pepe|first13=F.|last14=Pollacco|first14=D.|last15=Queloz|first15=D.|last16=Ségransan|first16=D.|last17=Skillen|first17=I.|last18=Smalley|first18=B.|last19=Smith|first19=A. M. S.|last20=Southworth|first20=J.|last21=Triaud|first21=A. H. M. J.|last22=Turner|first22=O. D.|last23=Udry|first23=S.|last24=West|first24=R. G.|s2cid=54750890}}</ref> Its equilibrium temperature is 886 [[Kelvin|K]],<ref name=Wang2021>{{citation|arxiv=2101.00042|year=2021|title=Metastable Helium Absorptions with 3D Hydrodynamics and Self-consistent Photochemistry. I. WASP-69b, Dimensionality, X-Ray and UV Flux Level, Spectral Types, and Flares|last1=Wang|first1=Lile|last2=Dai|first2=Fei|journal=The Astrophysical Journal|volume=914|issue=2|page=98|doi=10.3847/1538-4357/abf1ee|bibcode=2021ApJ...914...98W |s2cid=230433986}}</ref> but the measured terminator temperature is significantly higher by at least 200 [[Kelvin|K]].<ref name=Murgas2020/>The planet is losing mass at a moderate rate of 0.5 {{Earth_mass}} per billion years, not producing a visible cometary tail.<ref name=Wang2021/>
In 2013, one planet, named [[WASP-69b]], was discovered on a tight, circular orbit.<ref name=Anderson2013/> Its equilibrium temperature is 886 [[Kelvin|K]],<ref name=Wang2021/> but the measured terminator temperature is significantly higher by at least 200 [[Kelvin|K]].<ref name=Murgas2020/> The planet is losing mass at a moderate rate of 0.5 {{Earth_mass}} per billion years, not producing a visible cometary tail.<ref name=Wang2021/>


The planetary atmosphere is extremely hazy and contains a partial cloud deck with cloud tops rising to a pressure of 100 [[Pascal (unit)|Pa]]. Its composition is mostly hydrogen and helium, and sodium was also detected in low concentration.<ref name=Murgas2020/><ref>{{citation|arxiv=1710.06479|year=2017|title=Detection of sodium in the atmosphere of WASP-69b|doi=10.1051/0004-6361/201731956|last1=Casasayas-Barris|first1=N.|last2=Palle|first2=E.|last3=Nowak|first3=G.|last4=Yan|first4=F.|last5=Nortmann|first5=L.|last6=Murgas|first6=F.|journal=Astronomy & Astrophysics|volume=608|pages=A135|bibcode=2017A&A...608A.135C|s2cid=67777582}}</ref> The sodium may originate from volcanic moons, not from the planet itself.<ref>{{citation|arxiv=1908.10732|year=2019|title=Sodium and Potassium Signatures of Volcanic Satellites Orbiting Close-in Gas Giant Exoplanets|doi=10.3847/1538-4357/ab40cc|last1=Oza|first1=Apurva V.|last2=Johnson|first2=Robert E.|last3=Lellouch|first3=Emmanuel|last4=Schmidt|first4=Carl|last5=Schneider|first5=Nick|last6=Huang|first6=Chenliang|last7=Gamborino|first7=Diana|last8=Gebek|first8=Andrea|last9=Wyttenbach|first9=Aurelien|last10=Demory|first10=Brice-Olivier|last11=Mordasini|first11=Christoph|last12=Saxena|first12=Prabal|last13=Dubois|first13=David|last14=Moullet|first14=Arielle|last15=Thomas|first15=Nicolas|journal=The Astrophysical Journal|volume=885|issue=2|page=168|bibcode=2019ApJ...885..168O|s2cid=201651224}}</ref>
The planetary atmosphere is extremely hazy and contains a partial cloud deck with cloud tops rising to a pressure of 100 [[Pascal (unit)|Pa]]. Its composition is mostly hydrogen and helium, and sodium was also detected in low concentration.<ref name=Murgas2020/><ref>{{citation|arxiv=1710.06479|year=2017|title=Detection of sodium in the atmosphere of WASP-69b|doi=10.1051/0004-6361/201731956|last1=Casasayas-Barris|first1=N.|last2=Palle|first2=E.|last3=Nowak|first3=G.|last4=Yan|first4=F.|last5=Nortmann|first5=L.|last6=Murgas|first6=F.|journal=Astronomy & Astrophysics|volume=608|pages=A135|bibcode=2017A&A...608A.135C|s2cid=67777582}}</ref> The sodium may originate from volcanic moons, not from the planet itself.<ref>{{citation|arxiv=1908.10732|year=2019|title=Sodium and Potassium Signatures of Volcanic Satellites Orbiting Close-in Gas Giant Exoplanets|doi=10.3847/1538-4357/ab40cc|last1=Oza|first1=Apurva V.|last2=Johnson|first2=Robert E.|last3=Lellouch|first3=Emmanuel|last4=Schmidt|first4=Carl|last5=Schneider|first5=Nick|last6=Huang|first6=Chenliang|last7=Gamborino|first7=Diana|last8=Gebek|first8=Andrea|last9=Wyttenbach|first9=Aurelien|last10=Demory|first10=Brice-Olivier|last11=Mordasini|first11=Christoph|last12=Saxena|first12=Prabal|last13=Dubois|first13=David|last14=Moullet|first14=Arielle|last15=Thomas|first15=Nicolas|journal=The Astrophysical Journal|volume=885|issue=2|page=168|bibcode=2019ApJ...885..168O|s2cid=201651224}}</ref>


By 2021, the presence of hazes in atmosphere of WASP-69b was confirmed, along with the solar or super-solar water abundance.<ref>{{citation|arxiv=2109.06335|year=2021|title=Probing the atmosphere of WASP-69 b with low- and high-resolution transmission spectroscopy|doi=10.1051/0004-6361/202141191 |last1=Khalafinejad |first1=S. |last2=Molaverdikhani |first2=K. |last3=Blecic |first3=J. |last4=Mallonn |first4=M. |last5=Nortmann |first5=L. |last6=Caballero |first6=J. A. |last7=Rahmati |first7=H. |last8=Kaminski |first8=A. |last9=Sadegi |first9=S. |last10=Nagel |first10=E. |last11=Carone |first11=L. |last12=Amado |first12=P. J. |last13=Azzaro |first13=M. |last14=Bauer |first14=F. F. |last15=Casasayas-Barris |first15=N. |last16=Czesla |first16=S. |last17=von Essen |first17=C. |last18=Fossati |first18=L. |last19=Güdel |first19=M. |last20=Henning |first20=Th. |last21=López-Puertas |first21=M. |last22=Lendl |first22=M. |last23=Lüftinger |first23=T. |last24=Montes |first24=D. |last25=Oshagh |first25=M. |last26=Pallé |first26=E. |last27=Quirrenbach |first27=A. |last28=Reffert |first28=S. |last29=Reiners |first29=A. |last30=Ribas |first30=I. |journal=Astronomy & Astrophysics |volume=656 |pages=A142 |bibcode=2021A&A...656A.142K |s2cid=237503489 |display-authors=1 }}</ref>
By 2021, the presence of hazes in atmosphere of WASP-69b was confirmed, along with a solar or super-solar water abundance.<ref>{{citation|arxiv=2109.06335|year=2021|title=Probing the atmosphere of WASP-69 b with low- and high-resolution transmission spectroscopy|doi=10.1051/0004-6361/202141191 |last1=Khalafinejad |first1=S. |last2=Molaverdikhani |first2=K. |last3=Blecic |first3=J. |last4=Mallonn |first4=M. |last5=Nortmann |first5=L. |last6=Caballero |first6=J. A. |last7=Rahmati |first7=H. |last8=Kaminski |first8=A. |last9=Sadegi |first9=S. |last10=Nagel |first10=E. |last11=Carone |first11=L. |last12=Amado |first12=P. J. |last13=Azzaro |first13=M. |last14=Bauer |first14=F. F. |last15=Casasayas-Barris |first15=N. |last16=Czesla |first16=S. |last17=von Essen |first17=C. |last18=Fossati |first18=L. |last19=Güdel |first19=M. |last20=Henning |first20=Th. |last21=López-Puertas |first21=M. |last22=Lendl |first22=M. |last23=Lüftinger |first23=T. |last24=Montes |first24=D. |last25=Oshagh |first25=M. |last26=Pallé |first26=E. |last27=Quirrenbach |first27=A. |last28=Reffert |first28=S. |last29=Reiners |first29=A. |last30=Ribas |first30=I. |journal=Astronomy & Astrophysics |volume=656 |pages=A142 |bibcode=2021A&A...656A.142K |s2cid=237503489 |display-authors=1 }}</ref>

⚫
In August 2022, this planetary system was included among 20 systems to be named by the third [[NameExoWorlds]] project.<ref>{{cite web |url=https://www.nameexoworlds.iau.org/2022exoworlds |title=List of ExoWorlds 2022 |date=8 August 2022 |website=nameexoworlds.iau.org |publisher=[[International Astronomical Union|IAU]] |access-date=27 August 2022}}</ref>


{{OrbitboxPlanet begin
{{OrbitboxPlanet begin
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| exoplanet = [[WASP-69b|b]]
| exoplanet = [[WASP-69b|b]]
| mass = {{val|0.260|0.017}}
| mass = {{val|0.260|0.017}}
| radius = {{val|0.945|0.007|0.017}}<ref name=Murgas2020/>
⚫
| radius = {{val|0.945|0.007|0.017}}<ref name=Murgas2020>{{citation|arxiv=2007.02741|year=2020|title=The GTC exoplanet transit spectroscopy survey XI. Possible detection of Rayleigh scattering in the atmosphere of the Saturn-mass planet WASP-69b|doi=10.1051/0004-6361/202038161|last1=Murgas|first1=F.|last2=Chen|first2=G.|last3=Nortmann|first3=L.|last4=Pallé|first4=E.|last5=Nowak|first5=G.|journal=Astronomy & Astrophysics|volume=A158|page=641|bibcode=2020A&A...641A.158M|s2cid=220363912}}</ref>
| semimajor = {{val|0.04525|0.00053}}
| semimajor = {{val|0.04525|0.00053}}
| period = {{val|3.8681382|0.0000017}}
| period = {{val|3.8681382|0.0000017}}
Line 70: Line 74:


==References==
==References==
{{Reflist}}
{{Reflist|refs=

<ref name=SIMBAD>{{cite simbad|title=BD-05 5432|access-date=2021-01-08}}</ref>

<ref name=GaiaDR3>{{Cite Gaia DR3|6910753016653587840}}</ref>

<ref name=Anderson2013>{{citation|arxiv=1310.5654|title=Three sub-Jupiter-mass planets: WASP-69b & WASP-84b transit active K dwarfs and WASP-70Ab transits the evolved primary of a G4+K3 binary|year=2013|doi=10.1093/mnras/stu1737|last1=Anderson|first1=D. R.|last2=Collier Cameron|first2=A.|last3=Delrez|first3=L.|last4=Doyle|first4=A. P.|last5=Faedi|first5=F.|last6=Fumel|first6=A.|last7=Gillon|first7=M.|last8=Gómez Maqueo Chew|first8=Y.|last9=Hellier|first9=C.|last10=Jehin|first10=E.|last11=Lendl|first11=M.|last12=Maxted|first12=P. F. L.|last13=Pepe|first13=F.|last14=Pollacco|first14=D.|last15=Queloz|first15=D.|last16=Ségransan|first16=D.|last17=Skillen|first17=I.|last18=Smalley|first18=B.|last19=Smith|first19=A. M. S.|last20=Southworth|first20=J.|last21=Triaud|first21=A. H. M. J.|last22=Turner|first22=O. D.|last23=Udry|first23=S.|last24=West|first24=R. G.|s2cid=54750890}}</ref>

⚫
<ref name=Gill2018>{{citation|arxiv=1801.06106|title=The atmospheric parameters of FGK stars using wavelet analysis of CORALIE spectra|year=2018|doi=10.1051/0004-6361/201731954|last1=Gill|first1=S.|last2=Maxted|first2=P. F. L.|last3=Smalley|first3=B.|journal=Astronomy & Astrophysics|volume=612|pages=A111|bibcode=2018A&A...612A.111G|s2cid=119331772}}</ref>

⚫
<ref name=Murgas2020>{{citation|arxiv=2007.02741|year=2020|title=The GTC exoplanet transit spectroscopy survey XI. Possible detection of Rayleigh scattering in the atmosphere of the Saturn-mass planet WASP-69b|doi=10.1051/0004-6361/202038161|last1=Murgas|first1=F.|last2=Chen|first2=G.|last3=Nortmann|first3=L.|last4=Pallé|first4=E.|last5=Nowak|first5=G.|journal=Astronomy & Astrophysics|volume=A158|page=641|bibcode=2020A&A...641A.158M|s2cid=220363912}}</ref>

<ref name=Wang2021>{{citation|arxiv=2101.00042|year=2021|title=Metastable Helium Absorptions with 3D Hydrodynamics and Self-consistent Photochemistry. I. WASP-69b, Dimensionality, X-Ray and UV Flux Level, Spectral Types, and Flares|last1=Wang|first1=Lile|last2=Dai|first2=Fei|journal=The Astrophysical Journal|volume=914|issue=2|page=98|doi=10.3847/1538-4357/abf1ee|bibcode=2021ApJ...914...98W |s2cid=230433986}}</ref>

<ref name="NEW2022">{{cite web |url=https://www.nameexoworlds.iau.org/2022approved-names |title=2022 Approved Names |website=nameexoworlds.iau.org |publisher=[[International Astronomical Union|IAU]] |access-date=7 June 2023}}</ref>

}}


{{Sky|21|00|06.1969|-|05|05|40.0370}}
{{Sky|21|00|06.1969|-|05|05|40.0370}}
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[[Category:Planetary systems with one confirmed planet]]
[[Category:Planetary systems with one confirmed planet]]
[[Category:2MASS objects|J21000618-0505398]]
[[Category:2MASS objects|J21000618-0505398]]
[[Category:Durchmusterung objects|-05 5432]]
[[Category:Durchmusterung objects|BD-05 5432]]
[[Category:Wide Angle Search for Planets|069]]
[[Category:Stars with proper names|Wouri]]

Revision as of 21:59, 8 June 2023

WASP-69
Observation data
Epoch J2000      Equinox J2000
Constellation Aquarius
Right ascension 21h 00m 06.19682s[1]
Declination −05° 05′ 40.0349″[1]
Apparent magnitude (V) 9.87±0.03[2]
Characteristics
Evolutionary stage main-sequence star
Spectral type K5V[3]
Astrometry
Radial velocity (Rv)−9.83±0.13[1] km/s
Proper motion (μ) RA: 33.778 mas/yr[1]
Dec.: −93.581 mas/yr[1]
Parallax (π)19.8858 ± 0.0170 mas[1]
Distance164.0 ± 0.1 ly
(50.29 ± 0.04 pc)
Details
Mass0.826±0.029[2] M☉
Radius0.813[2] R☉
Surface gravity (log g)4.59±0.02[4] cgs
Temperature4782±15[4] K
Metallicity [Fe/H]0.10±0.01[4] dex
Rotation23.07 d[2]
Rotational velocity (v sin i)1.27±0.22[4] km/s
Age2[2] Gyr
Other designations
Wouri, BD−05 5432, WASP-69, TYC 5200-1560-1, GSC 05200-01560, 2MASS J21000618-0505398[5]
Database references
SIMBADdata

WASP-69 is a K-type main-sequence star 164 light-years (50 parsecs) away. Its surface temperature is 4782±15 K. WASP-69 is slightly enriched in heavy elements compared to the Sun, with a metallicity Fe/H index of 0.10±0.01,[4] and is much younger than the Sun at 2 billion years. The data regarding starspot activity of WASP-69 are inconclusive, but spot coverage of the photosphere may be very high.[6]

Multiplicity surveys did not detect any stellar companions to WASP-69 as of 2020.[7]

Nomenclature

The designation WASP-69 indicates that this was the 69th star found to have a planet by the Wide Angle Search for Planets.

In August 2022, this planetary system was included among 20 systems to be named by the third NameExoWorlds project.[8] The approved names, proposed by a team from Cameroon, were announced in June 2023. WASP-69 is named Wouri and its planet is named Makombé, after the Wouri and Makombé rivers.[9]

Planetary system

In 2013, one planet, named WASP-69b, was discovered on a tight, circular orbit.[2] Its equilibrium temperature is 886 K,[10] but the measured terminator temperature is significantly higher by at least 200 K.[6] The planet is losing mass at a moderate rate of 0.5 ME per billion years, not producing a visible cometary tail.[10]

The planetary atmosphere is extremely hazy and contains a partial cloud deck with cloud tops rising to a pressure of 100 Pa. Its composition is mostly hydrogen and helium, and sodium was also detected in low concentration.[6][11] The sodium may originate from volcanic moons, not from the planet itself.[12]

By 2021, the presence of hazes in atmosphere of WASP-69b was confirmed, along with a solar or super-solar water abundance.[13]

The WASP-69 planetary system[2]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b 0.260±0.017 MJ 0.04525±0.00053 3.8681382±0.0000017 0 86.71±0.20° 0.945+0.007
−0.017[6] RJ

References

  1. ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  2. ^ a b c d e f g Anderson, D. R.; Collier Cameron, A.; Delrez, L.; Doyle, A. P.; Faedi, F.; Fumel, A.; Gillon, M.; Gómez Maqueo Chew, Y.; Hellier, C.; Jehin, E.; Lendl, M.; Maxted, P. F. L.; Pepe, F.; Pollacco, D.; Queloz, D.; Ségransan, D.; Skillen, I.; Smalley, B.; Smith, A. M. S.; Southworth, J.; Triaud, A. H. M. J.; Turner, O. D.; Udry, S.; West, R. G. (2013), Three sub-Jupiter-mass planets: WASP-69b & WASP-84b transit active K dwarfs and WASP-70Ab transits the evolved primary of a G4+K3 binary, arXiv:1310.5654, doi:10.1093/mnras/stu1737, S2CID 54750890{{citation}}: CS1 maint: unflagged free DOI (link)
  3. ^ France, Kevin; Arulanantham, Nicole; Fossati, Luca; Lanza, Antonino F.; Loyd, R. O. Parke; Redfield, Seth; Schneider, P. Christian (2018), "Far-ultraviolet Activity Levels of F, G, K, and M Dwarf Exoplanet Host Stars", The Astrophysical Journal Supplement Series, 239 (1): 16, arXiv:1809.07342, Bibcode:2018ApJS..239...16F, doi:10.3847/1538-4365/aae1a3, S2CID 119368148{{citation}}: CS1 maint: unflagged free DOI (link)
  4. ^ a b c d e Gill, S.; Maxted, P. F. L.; Smalley, B. (2018), "The atmospheric parameters of FGK stars using wavelet analysis of CORALIE spectra", Astronomy & Astrophysics, 612: A111, arXiv:1801.06106, Bibcode:2018A&A...612A.111G, doi:10.1051/0004-6361/201731954, S2CID 119331772
  5. ^ "BD-05 5432". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-01-08.
  6. ^ a b c d Murgas, F.; Chen, G.; Nortmann, L.; Pallé, E.; Nowak, G. (2020), "The GTC exoplanet transit spectroscopy survey XI. Possible detection of Rayleigh scattering in the atmosphere of the Saturn-mass planet WASP-69b", Astronomy & Astrophysics, A158: 641, arXiv:2007.02741, Bibcode:2020A&A...641A.158M, doi:10.1051/0004-6361/202038161, S2CID 220363912
  7. ^ Bohn, A. J.; Southworth, J.; Ginski, C.; Kenworthy, M. A.; Maxted, P. F. L.; Evans, D. F. (2020), "A multiplicity study of transiting exoplanet host stars. I. High-contrast imaging with VLT/SPHERE", Astronomy & Astrophysics, 635: A73, arXiv:2001.08224, Bibcode:2020A&A...635A..73B, doi:10.1051/0004-6361/201937127, S2CID 210861118
  8. ^ "List of ExoWorlds 2022". nameexoworlds.iau.org. IAU. 8 August 2022. Retrieved 27 August 2022.
  9. ^ "2022 Approved Names". nameexoworlds.iau.org. IAU. Retrieved 7 June 2023.
  10. ^ a b Wang, Lile; Dai, Fei (2021), "Metastable Helium Absorptions with 3D Hydrodynamics and Self-consistent Photochemistry. I. WASP-69b, Dimensionality, X-Ray and UV Flux Level, Spectral Types, and Flares", The Astrophysical Journal, 914 (2): 98, arXiv:2101.00042, Bibcode:2021ApJ...914...98W, doi:10.3847/1538-4357/abf1ee, S2CID 230433986{{citation}}: CS1 maint: unflagged free DOI (link)
  11. ^ Casasayas-Barris, N.; Palle, E.; Nowak, G.; Yan, F.; Nortmann, L.; Murgas, F. (2017), "Detection of sodium in the atmosphere of WASP-69b", Astronomy & Astrophysics, 608: A135, arXiv:1710.06479, Bibcode:2017A&A...608A.135C, doi:10.1051/0004-6361/201731956, S2CID 67777582
  12. ^ Oza, Apurva V.; Johnson, Robert E.; Lellouch, Emmanuel; Schmidt, Carl; Schneider, Nick; Huang, Chenliang; Gamborino, Diana; Gebek, Andrea; Wyttenbach, Aurelien; Demory, Brice-Olivier; Mordasini, Christoph; Saxena, Prabal; Dubois, David; Moullet, Arielle; Thomas, Nicolas (2019), "Sodium and Potassium Signatures of Volcanic Satellites Orbiting Close-in Gas Giant Exoplanets", The Astrophysical Journal, 885 (2): 168, arXiv:1908.10732, Bibcode:2019ApJ...885..168O, doi:10.3847/1538-4357/ab40cc, S2CID 201651224{{citation}}: CS1 maint: unflagged free DOI (link)
  13. ^ Khalafinejad, S.; et al. (2021), "Probing the atmosphere of WASP-69 b with low- and high-resolution transmission spectroscopy", Astronomy & Astrophysics, 656: A142, arXiv:2109.06335, Bibcode:2021A&A...656A.142K, doi:10.1051/0004-6361/202141191, S2CID 237503489


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