View source for WASP-121b

{{Short description|Hot Jupiter exoplanet orbiting WASP-121}}
{{use dmy dates|date=August 2017}}
{{Infobox planet
| name = WASP-121b / Tylos
| image = WASP-121b 01.jpg
| caption = Artist's impression of WASP-121b and its host star
<!-- DISCOVERY           -->
| discovery_ref = <ref name="Delrez2015"/>
| discoverer = L. Delrez ''et al.''
| discovered = 2015
| discovery_method = [[Methods of detecting exoplanets#Transit photometry|Transit]]
<!-- DESIGNATIONS        -->
| alt_names = Tylos<ref name="NEW2022"/>
<!-- ORBITAL             -->
| orbit_ref = <ref name="Bourrier2020"/>
| apsis = astron
| semimajor = {{val|0.02596|0.00043|0.00063|ul=AU}}
| eccentricity = <0.0032
| period = {{val|1.27492504|(15)|ul=d}}
| inclination = {{val|88.49|0.16|u=deg}}
| arg_peri = {{val|10|10|u=deg}}
| star = [[WASP-121]]
<!-- PHYS CHARS          -->
| physical_ref = <ref name="Bourrier2020"/>
| mean_radius = {{val|1.753|0.036|ul=Jupiter radius}}
| mass = {{val|1.157|0.070|ul=Jupiter mass}}
| density = {{val|0.266|0.024|0.022|ul=g/cm3}}
| surface_grav = {{val|9.33|0.71|0.67|ul=m/s2}} (0.95 [[g-force|g]])
| single_temperature = {{val|2602|53|ul=K}} ({{convert|2602|K|C F|disp=out}})<ref name="Changeat2022"/>
<!-- ATMOSPHERE          --> 
<!-- NOTES               -->
}}

'''WASP-121b''', formally named '''Tylos''',<ref name="NEW2022"/> is an [[exoplanet]] orbiting the [[star]] [[WASP-121]].<ref name="NASA-20170802"/><ref name="NAT-20170802"/> WASP-121b is the first exoplanet found to contain [[water]] in an extrasolar planetary [[stratosphere]] (i.e., an [[atmosphere|atmospheric layer]] in which temperatures increase as the altitude increases).<ref name="NASA-20170802" /><ref name="NAT-20170802" /> WASP-121b is in the constellation [[Puppis]],<ref name="Constellation">{{cite web |author=Staff |title=Finding the constellation which contains given sky coordinates |url=http://djm.cc/constellation.html |work=djm.cc |access-date=3 August 2017 }}</ref> and is about 858 [[light-year]]s from Earth.<ref name="GaiaDR3"/><ref name="NASA-20170802" /><ref>{{Cite news|url=https://www.nasa.gov/feature/jpl/water-is-destroyed-then-reborn-in-ultrahot-jupiters|title=Water Is Destroyed, Then Reborn in Ultrahot Jupiters|last=Greicius|first=Tony|date=2018-08-07|work=NASA|access-date=2018-11-15|language=en}}</ref>

==Nomenclature==
In August 2022, this planet and its host star were 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 [[Bahrain]], were announced in June 2023. WASP-121b is named '''Tylos''' after the [[Tylos|ancient Greek name]] for Bahrain, and its host star is named '''[[WASP-121|Dilmun]]''' after the [[Dilmun|ancient civilization]].<ref name="NEW2022"/>

==Characteristics==
[[File:PIA22565-Exoplanet-WASP121b-ComputerSimViews-20180809.jpg|thumb|center|400px|{{center|WASP-121b - computer simulated views (August 2018)}}]]

WASP-121b is an [[ultra-hot Jupiter]] [[exoplanet]] with a mass about 1.16 times that of [[Jupiter]] and a radius about 1.75 times that of Jupiter. The exoplanet orbits [[WASP-121]], its host star, every 1.27 days.<ref name="Bourrier2020"/>

In 2019 a work by Hellard ''et al.'' discussed the possibility of measuring the [[Love number]] of transiting hot Jupiters using HST ([[Hubble Space Telescope]])/[[Space Telescope Imaging Spectrograph|STIS]]. A tentative measurement of <math>h_2=1.4\pm0.8</math> for WASP-121b was published in the same work.<ref>{{cite journal|last1=Hellard|first1=Hugo|last2=Csizmadia|first2=Szilárd|last3=Padovan|first3=Sebastiano|last4=Sohl|first4=Frank|last5=Rauer|first5=Heike|s2cid=209324250|title=HST/STIS capability for Love number measurement of WASP-121b|journal=The Astrophysical Journal|year=2020|volume=889|issue=1|page=66|doi=10.3847/1538-4357/ab616e|arxiv=1912.05889|bibcode=2020ApJ...889...66H |doi-access=free }}</ref><ref>{{Cite web|url=https://wasp-planets.net/2019/12/19/the-tidal-shape-of-the-exoplanet-wasp-121b/|title=The tidal shape of the exoplanet WASP-121b|last=waspplanets|date=2019-12-19|website=WASP Planets|language=en|access-date=2020-01-20}}</ref>

The planetary orbit is inclined to the equatorial plane of the star by 8.1°.<ref name=Borsa2020/>

===Atmospheric composition===
A spectral survey in 2015 attributed {{convert|2500|C|F|abbr=on}}, hot<ref name="NASA-20170802" /> [[stratosphere]] absorption bands to [[Water|water molecules]], [[titanium(II) oxide]] (TiO) and [[vanadium(II) oxide]] (VO).<ref name="EP-2015"/> Neutral iron was also detected in the stratosphere of WASP-121b in 2020,<ref>{{cite journal|arxiv=2001.06430|last1=Gibson|first1=Neale P.|title=Detection of Fe I in the atmosphere of the ultra-hot Jupiter WASP-121b, and a new likelihood-based approach for Doppler-resolved spectroscopy|last2=Merritt|first2=Stephanie|last3=Nugroho|first3=Stevanus K.|last4=Cubillos|first4=Patricio E.|last5=de Mooij|first5=Ernst J. W.|last6=Mikal-Evans|first6=Thomas|last7=Fossati|first7=Luca|last8=Lothringer|first8=Joshua|last9=Nikolov|first9=Nikolay|last10=Sing|first10=David K.|last11=Spake|first11=Jessica J.|last12=Watson|first12=Chris A.|last13=Wilson|first13=Jamie|s2cid=210714233|journal=Monthly Notices of the Royal Astronomical Society|year=2020|volume=493|issue=2|page=2215|doi=10.1093/mnras/staa228|doi-access=free |bibcode=2020MNRAS.493.2215G}}</ref><ref>{{cite journal|arxiv=2001.07196|last1=Cabot|first1=Samuel H. C.|title=Detection of neutral atomic species in the ultra-hot jupiter WASP-121b|last2=Madhusudhan|first2=Nikku|last3=Welbanks|first3=Luis|last4=Piette|first4=Anjali|last5=Gandhi|first5=Siddharth|s2cid=210838889|journal=Monthly Notices of the Royal Astronomical Society|year=2020|volume=494|issue=1|pages=363–377|doi=10.1093/mnras/staa748|doi-access=free |bibcode=2020MNRAS.494..363C}}</ref> along with neutral [[chromium]] and [[vanadium]].<ref>{{cite journal|arxiv=2006.05995|doi=10.3847/2041-8213/ab94aa|title=Neutral Cr and V in the Atmosphere of Ultra-hot Jupiter WASP-121 B|year=2020|last1=Ben-Yami|first1=Maya|last2=Madhusudhan|first2=Nikku|last3=Cabot|first3=Samuel H. C.|last4=Constantinou|first4=Savvas|last5=Piette|first5=Anjali|last6=Gandhi|first6=Siddharth|last7=Welbanks|first7=Luis|s2cid=219573825|journal=The Astrophysical Journal|volume=897|issue=1|pages=L5|bibcode=2020ApJ...897L...5B |doi-access=free }}</ref> A number of other studies, however, failed to detect TiO and VO.<ref name="NAT-20170802"/><ref name="Mikal-Evans2019"/><ref>{{Cite journal |last1=Merritt |first1=S. R. |last2=Gibson |first2=N. P. |last3=Nugroho |first3=S. K. |last4=Mooij |first4=E. J. W. de |last5=Hooton |first5=M. J. |last6=Matthews |first6=S. M. |last7=McKemmish |first7=L. K. |last8=Mikal-Evans |first8=T. |last9=Nikolov |first9=N. |last10=Sing |first10=D. K. |last11=Spake |first11=J. J. |date=2020-04-01 |title=Non-detection of TiO and VO in the atmosphere of WASP-121b using high-resolution spectroscopy |url=https://www.aanda.org/articles/aa/abs/2020/04/aa37409-19/aa37409-19.html |journal=Astronomy & Astrophysics |language=en |volume=636 |pages=A117 |doi=10.1051/0004-6361/201937409 |arxiv=2002.02795 |bibcode=2020A&A...636A.117M |issn=0004-6361|doi-access=free}}</ref><ref>{{cite journal|arxiv=2005.09631|last1=Mikal-Evans|first1=Thomas|last2=Sing|first2=David K.|last3=Kataria|first3=Tiffany|last4=Wakeford|first4=Hannah R.|last5=Mayne|first5=Nathan J.|last6=Lewis|first6=Nikole K.|last7=Barstow|first7=Joanna K.|last8=Spake|first8=Jessica J.|s2cid=218684532|title=Confirmation of water emission in the dayside spectrum of the ultrahot Jupiter WASP-121b|journal=Monthly Notices of the Royal Astronomical Society|year=2020|volume=496|issue=2|pages=1638–1644|doi=10.1093/mnras/staa1628|doi-access=free |bibcode=2020MNRAS.496.1638M}}</ref>

Reanalysis of collected spectral data was published in June 2020. Neutral [[magnesium]], [[calcium]], vanadium, chromium, iron, and [[nickel]], along with ionized [[sodium|sodium atoms]], were detected. However the low quality of available data precluded a positive identification of any molecular species, including water. The atmosphere appears to be significantly out of [[chemical equilibrium]] and possibly escaping.<ref name="Hoeijmakers2020"/> The strong atmospheric flows beyond the [[Roche lobe]], indicating ongoing atmosphere loss, were confirmed in late 2020.<ref name=Borsa2020/>

In 2021, the planetary atmosphere was revealed to be slightly more blue and less absorbing, which may be an indication of planetary weather patterns.<ref>{{citation|arxiv=2103.05698|year=2021|title=Gemini/GMOS optical transmission spectroscopy of WASP-121b: Signs of variability in an ultra-hot Jupiter?|doi=10.1093/mnras/stab797 |last1=Wilson |first1=Jamie |last2=Gibson |first2=Neale P. |last3=Lothringer |first3=Joshua D. |last4=Sing |first4=David K. |last5=Mikal-Evans |first5=Thomas |last6=De Mooij |first6=Ernst J W. |last7=Nikolov |first7=Nikolay |last8=Watson |first8=Chris A. |journal=Monthly Notices of the Royal Astronomical Society |volume=503 |issue=4 |pages=4787–4801 |doi-access=free }}</ref> By mid-2021, the presence of ions of [[iron]], chromium, vanadium and calcium in the planetary atmosphere was confirmed.<ref>{{citation|arxiv=2106.15394|year=2021|title=An inventory of atomic species in the atmosphere of WASP-121b using UVES high-resolution spectroscopy|doi=10.1093/mnras/stab1878 |last1=Merritt |first1=Stephanie R. |last2=Gibson |first2=Neale P. |last3=Nugroho |first3=Stevanus K. |last4=De Mooij |first4=Ernst J W. |last5=Hooton |first5=Matthew J. |last6=Lothringer |first6=Joshua D. |last7=Matthews |first7=Shannon M. |last8=Mikal-Evans |first8=Thomas |last9=Nikolov |first9=Nikolay |last10=Sing |first10=David K. |last11=Watson |first11=Chris A. |journal=Monthly Notices of the Royal Astronomical Society |volume=506 |issue=3 |pages=3853–3871 |doi-access=free }}</ref> In 2022, ionized barium was also detected.<ref>{{citation|arxiv=2210.06892|year=2022|title=Detection of barium in the atmospheres of the ultra-hot gas giants WASP-76b and WASP-121b|doi=10.1051/0004-6361/202244489 |last1=Azevedo Silva |first1=T. |last2=Demangeon |first2=O. D. S. |last3=Santos |first3=N. C. |last4=Allart |first4=R. |last5=Borsa |first5=F. |last6=Cristo |first6=E. |last7=Esparza-Borges |first7=E. |last8=Seidel |first8=J. V. |last9=Palle |first9=E. |last10=Sousa |first10=S. G. |last11=Tabernero |first11=H. M. |last12=Zapatero Osorio |first12=M. R. |last13=Cristiani |first13=S. |last14=Pepe |first14=F. |last15=Rebolo |first15=R. |last16=Adibekyan |first16=V. |last17=Alibert |first17=Y. |last18=Barros |first18=S. C. C. |last19=Bouchy |first19=F. |last20=Bourrier |first20=V. |last21=Lo Curto |first21=G. |last22=Di Marcantonio |first22=P. |last23=d'Odorico |first23=V. |last24=Ehrenreich |first24=D. |last25=Figueira |first25=P. |last26=González Hernández |first26=J. I. |last27=Lovis |first27=C. |last28=Martins |first28=C. J. A. P. |last29=Mehner |first29=A. |last30=Micela |first30=G. |journal=Astronomy & Astrophysics |volume=666 |pages=L10 |s2cid=252873126 |display-authors=1 }}</ref> By 2022, an absence of titanium in the planetary atmosphere was confirmed and attributed to the nightside condensation of highly refractory [[titanium dioxide]].<ref>{{citation|arxiv=2210.12847|year=2022|title=The Mantis Network III: A titanium cold-trap on the ultra-hot Jupiter WASP-121 b.|last1=Hoeijmakers |first1=H. J. |last2=Kitzmann |first2=D. |last3=Morris |first3=B. M. |last4=Prinoth |first4=B. |last5=Borsato |first5=N. |last6=Pino |first6=L. |last7=Lee |first7=E. K. H. |last8=Akın |first8=C. |last9=Heng |first9=K. |journal=Astronomy and Astrophysics |volume=685 |doi=10.1051/0004-6361/202244968 |bibcode=2024A&A...685A.139H}}</ref> Observations by HST from 2016-2019, published in 2024, confirmed variability in the atmosphere of WASP-121b.<ref name="heic2401"/><ref name="Changeat2024"/>

A 2025 study revealed the first 3D structure of its atmosphere, showing it to be formed of at least three layers. The upper layer consists of hydrogen gas, the  middle layer contains sodium and the lower layer iron. A super-rotational sodium-containing jet stream moves material around the equator while the layer below moves the gas from the hot side of the planet to the cooler side.<ref>{{cite journal |journal=Nature |author=Julia V. Seidel, Bibiana Prinoth, Lorenzo Pino, Leonardo A. dos Santos, Hritam Chakraborty, Vivien Parmentier, Elyar Sedaghati, Joost P. Wardenier, Casper Farret Jentink, Maria Rosa Zapatero Osorio, Romain Allart, David Ehrenreich, Monika Lendl, Giulia Roccetti, Yuri Damasceno, Vincent Bourrier, Jorge Lillo-Box, H. Jens Hoeijmakers, Enric Pallé, Nuno Santos, Alejandro Suárez Mascareño, Sergio G. Sousa, Hugo M. Tabernero & Francesco A. Pepe |title=Vertical structure of an exoplanet’s atmospheric jet stream|date=2025|doi=10.1038/s41586-025-08664-1 |arxiv=2502.12261 }}</ref> Titanium is detected at a lower latitude below the equatorial jet stream.<ref>{{cite journal |journal= Astronomy & Astrophysics |title=Titanium chemistry of WASP-121 b with ESPRESSO in 4-UT mode |volume =694|date= February 2025 |doi=10.1051/0004-6361/202452405 |author=B. Prinoth, J.V. Seidel, H.J. Hoeijmakers, B.M. Morris, M. Baratella, N.W. Borsato, Y.C. Damasceno, V. Parmentier, D. Kitzmann, E. Sedaghati, L. Pino, F. Borsa, R. Allart, N. Santos, M. Steiner, A. Suárez Mascareño, H. Tabernero, M.R. Zapatero Osorio |arxiv=2502.12262 }}</ref>

==Possible exomoon==
The sodium detected via [[absorption spectroscopy]] around WASP-121b<ref name="Hoeijmakers2020"/> is consistent with an extrasolar [[gas torus]], possibly fueled by an [[Io (moon)|Io]]-like [[exomoon]].<ref name="Gebek2020"/>

==See also==
{{Commons category}}
* [[List of exoplanet firsts]]
* [[List of exoplanets discovered in 2015]], including WASP-121b
* [[SuperWASP]]
* [[WASP-33b]], another ultra-hot Jupiter

==References==
{{Reflist|refs=

<ref name="GaiaDR3">{{Cite Gaia DR3|5565050255701441664}}</ref>

<ref name="Delrez2015">{{citation|arxiv=1506.02471|year=2015|title=WASP-121 b: A hot Jupiter close to tidal disruption transiting an active F star|doi=10.1093/mnras/stw522|last1=Delrez|first1=L.|last2=Santerne|first2=A.|last3=Almenara|first3=J.-M.|last4=Anderson|first4=D. R.|last5=Collier-Cameron|first5=A.|last6=Díaz|first6=R. F.|last7=Gillon|first7=M.|last8=Hellier|first8=C.|last9=Jehin|first9=E.|last10=Lendl|first10=M.|last11=Maxted|first11=P. F. L.|last12=Neveu-Vanmalle|first12=M.|last13=Pepe|first13=F.|last14=Pollacco|first14=D.|last15=Queloz|first15=D.|last16=Ségransan|first16=D.|last17=Smalley|first17=B.|last18=Smith|first18=A. M. S.|last19=Triaud|first19=A. H. M. J.|last20=Udry|first20=S.|last21=Van Grootel|first21=V.|last22=West|first22=R. G.|journal=Monthly Notices of the Royal Astronomical Society|volume=458|issue=4|pages=4025–4043 |doi-access=free |bibcode=2016MNRAS.458.4025D}}</ref>

<ref name="EP-2015">{{cite encyclopedia |author=Staff |title=Planet WASP-121 b |url=https://exoplanet.eu/catalog/wasp_121_b--2410/ |date=2015 |encyclopedia=[[Extrasolar Planets Encyclopaedia]] |access-date=3 August 2017 }}</ref>

<ref name="NASA-20170802">{{cite web |last1=Landau |first1=Elizabeth |last2=Villard |first2=Ray |title=Hubble Detects Exoplanet with Glowing Water Atmosphere |url=https://www.jpl.nasa.gov/news/news.php?feature=6909 |date=2 August 2017 |work=[[NASA]] |access-date=2 August 2017 }}</ref>

<ref name="NAT-20170802">{{cite journal |last1=Evans |first1=Thomas M. |last2=Sing |first2=David K. |last3=Kataria |first3=Tiffany |last4=Goyal |first4=Jayesh |last5=Nikolov |first5=Nikolay |last6=Wakeford |first6=Hannah R. |last7=Deming |first7=Drake |last8=Marley |first8=Mark S. |last9=Amundsen |first9=David S. |last10=Ballester |first10=Gilda E. |last11=Barstow |first11=Joanna K. |s2cid=205258293 |display-authors=2 |title=An ultrahot gas-giant exoplanet with a stratosphere |date=2 August 2017 |journal=[[Nature (journal)|Nature]] |volume=548 |issue=7665 |pages=58–61 |doi=10.1038/nature23266 |pmid=28770846 |arxiv = 1708.01076 |bibcode = 2017Natur.548...58E |language=en |issn=1476-4687}}</ref>

<ref name="Mikal-Evans2019">{{Cite journal |last=Mikal-Evans |first=Thomas |date=27 June 2019 |title=An emission spectrum for WASP-121b measured across the 0.8–1.1 μm wavelength range using the Hubble Space Telescope |journal=Monthly Notices of the Royal Astronomical Society |volume=488 |issue=2 |pages=2222–2234 |doi=10.1093/mnras/stz1753 |doi-access=free |hdl=10150/634587 |hdl-access=free |arxiv=1906.06326 |bibcode=2019MNRAS.488.2222M}}</ref>

<ref name="Bourrier2020">{{cite journal |last1=Bourrier |first1=V. |last2=Ehrenreich |first2=D. |display-authors=etal |date=March 2020 |title=Hot Exoplanet Atmospheres Resolved with Transit Spectroscopy (HEARTS). III. Atmospheric structure of the misaligned ultra-hot Jupiter WASP-121b |journal=[[Astronomy & Astrophysics]] |volume=635 |issue= |pages=A205 |doi=10.1051/0004-6361/201936640 |arxiv=2001.06836 |bibcode=2020A&A...635A.205B}}</ref>

<ref name="Gebek2020">{{cite journal |last1=Gebek |first1=Andrea |last2=Oza |first2=Apurva |title=Alkaline exospheres of exoplanet systems: evaporative transmission spectra |journal=Monthly Notices of the Royal Astronomical Society |date=29 July 2020 |volume=497 |issue=4 |pages=5271–5291 |doi=10.1093/mnras/staa2193 |doi-access=free |arxiv=2005.02536 |bibcode=2020MNRAS.497.5271G |s2cid=218516741 |url=https://academic.oup.com/mnras/article-abstract/497/4/5271/5877918?redirectedFrom=fulltext |access-date=8 December 2020}}</ref>

<ref name="Hoeijmakers2020">{{cite journal |last1=Hoeijmakers |first1=H.J. |last2=Seidel |first2=J.V. |last3=Pino |first3=L. |last4=Kitzmann |first4=D. |last5=Sindel |first5=J.P. |last6=Ehrenreich |first6=D. |last7=Oza |first7=A.V. |last8=Bourrier |first8=V. |last9=Allart |first9=R. |last10=Gebek |first10=A. |last11=Lovis |first11=C. |last12=Yurchenko |first12=S.N. |last13=Astudillo-Defru |first13=N. |last14=Bayliss |first14=D. |last15=Cegla |first15=H. |last16=Lavie |first16=B. |last17=Lendl |first17=M. |last18=Melo |first18=C. |last19=Murgas |first19=F. |last20=Nascimbeni |first20=V. |last21=Pepe |first21=F. |last22=Segransan |first22=D. |last23=Udry |first23=S. |last24=Wyttenbach |first24=A. |last25=Heng |first25=K. |title=Hot Exoplanet Atmospheres Resolved with Transit Spectroscopy (HEARTS) - IV. A spectral inventory of atoms and molecules in the high-resolution transmission spectrum of WASP-121 b |journal=Astronomy & Astrophysics |date=18 September 2020 |volume=641 |page=A123 |doi=10.1051/0004-6361/202038365|arxiv=2006.11308 |bibcode=2020A&A...641A.123H |s2cid=219966241 }}</ref>

<ref name=Borsa2020>{{citation|arxiv=2011.01245|title=Atmospheric Rossiter–Mc ''Laughlin'' effect and transmission spectroscopy of WASP-121b with ESPRESSO|year=2021|doi=10.1051/0004-6361/202039344 |last1=Borsa |first1=F. |last2=Allart |first2=R. |last3=Casasayas-Barris |first3=N. |last4=Tabernero |first4=H. |last5=Zapatero Osorio |first5=M. R. |last6=Cristiani |first6=S. |last7=Pepe |first7=F. |last8=Rebolo |first8=R. |last9=Santos |first9=N. C. |last10=Adibekyan |first10=V. |last11=Bourrier |first11=V. |last12=Demangeon |first12=O. D. S. |last13=Ehrenreich |first13=D. |last14=Pallé |first14=E. |last15=Sousa |first15=S. |last16=Lillo-Box |first16=J. |last17=Lovis |first17=C. |last18=Micela |first18=G. |last19=Oshagh |first19=M. |last20=Poretti |first20=E. |last21=Sozzetti |first21=A. |last22=Allende Prieto |first22=C. |last23=Alibert |first23=Y. |last24=Amate |first24=M. |last25=Benz |first25=W. |last26=Bouchy |first26=F. |last27=Cabral |first27=A. |last28=Dekker |first28=H. |last29=d'Odorico |first29=V. |last30=Di Marcantonio |first30=P. |journal=Astronomy & Astrophysics |volume=645 |pages=A24 |bibcode=2021A&A...645A..24B |s2cid=226237425 |display-authors=1 }}</ref>

<ref name="Changeat2022">{{cite journal |last1=Changeat |first1=Q. |last2=Edwards |first2=B. |display-authors=etal |date=May 2022 |title=Five Key Exoplanet Questions Answered via the Analysis of 25 Hot-Jupiter Atmospheres in Eclipse |journal=[[The Astrophysical Journal Supplement Series]] |volume=260 |issue=1 |pages=3 |doi=10.3847/1538-4365/ac5cc2 |doi-access=free |arxiv=2204.11729 |bibcode=2022ApJS..260....3C}}</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>

<ref name="heic2401">{{cite web |url=https://esahubble.org/news/heic2401/ |title=Hubble observes a changing exoplanet atmosphere |website=esahubble.org |publisher=[[European Space Agency|ESA]] |date=4 January 2024 |access-date=4 January 2024}}</ref>

<ref name="Changeat2024">{{cite journal |last1=Changeat |first1=Quentin |last2=Skinner |first2=Jack W. |display-authors=etal |date=January 2024 |title=Is the atmosphere of the ultra-hot Jupiter WASP-121b variable? |journal=[[The Astrophysical Journal Supplement Series]] |volume= 270|issue= 2|page=34 |doi= 10.3847/1538-4365/ad1191|doi-access=free |arxiv=2401.01465|bibcode=2024ApJS..270...34C }}</ref>

}}

==External links==
* [http://wasp-planets.net/wasp-planets/ SuperWASP Wide Angle Search for Planets: The Planets], [[SuperWASP]].
* {{cite web |last=Pultarova |first=Tereza |title=Hubble Telescope Detects Stratosphere on Huge Alien Planet |url=https://www.space.com/37705-exoplanet-stratosphere-detected-wasp-121b.html |date=3 August 2017 |work=[[space.com]] |access-date=3 August 2017 }}

{{Sky|07|10|24.0|-|39|05|51|900}}
{{2015 in space}}
{{Puppis}}
{{Authority control}}
{{portal bar|Astronomy|Space}}

[[Category:Exoplanets discovered by WASP]]
[[Category:Exoplanets discovered in 2015]]
[[Category:Puppis]]
[[Category:Hot Jupiters]]
[[Category:Exoplanets with proper names]]