WASP-79b
{{Short description|Exoplanet}}
{{Infobox planet
| name = WASP-79b / Pollera
| discovery_method = Transit method
| apsis = astron
| semimajor = {{val|0.05014|0.00034|0.00035|ul=AU}}
| period = {{val|3.66239094|(60)}} days
| inclination = {{val|85.52|0.1|ul=deg}}
| star = WASP-79
| mean_radius = {{val|1.5795|0.0048|ul=Jupiter radius}}
| mass = {{val|0.835|0.077|ul=Jupiter mass}}
| single_temperature = {{val|1747|27|ul=K}}
}}
WASP-79b, also known as Pollera, is an extrasolar planet orbiting the star WASP-79 (Montuno). This planet is in the constellation Eridanus, and is about 810 light-years from Earth.
The name, Pollera, was selected in the NameExoWorlds campaign by Panama, during the 100th anniversary of the IAU. A pollera is the traditional costume the woman wears in the El Punto, a Panamanian dance.{{Cite web|url=http://www.nameexoworlds.iau.org/final-results|title=Approved names|website=NameExoworlds|language=en|access-date=2020-01-02}}{{Cite web|url=https://www.iau.org/news/pressreleases/detail/iau1912/|title=International Astronomical Union {{!}} IAU|website=www.iau.org|access-date=2020-01-02}}
Host star
WASP-79, or CD-30 1812, is a F-type dwarf star located at 240 parsecs (810 light years) away from Earth. With {{solar mass|1.38|link=y}} and {{solar radius|1.53|link=y}}, it is both larger and more massive than the Sun. Its effective temperature is 6,600 K, making it hotter than the Sun.
The star WASP-79 is named Montuno. Montuno is the traditional costume the man wears in the “El Punto”, a Panamanian dance.
Characteristics
WASP-79b is a very large hot jupiter that is among the largest exoplanets discovered although its size is uncertain. The discovery paper estimated it to be {{jupiter radius|2.09 ± 0.14|link=y}} (approximately 300,000 kilometers across) with a temperature of 1,900 ± 50 K,{{cite journal|bibcode=2012A&A...547A..61S|title=WASP-78b and WASP-79b: Two highly-bloated hot Jupiter-mass exoplanets orbiting F-type stars in Eridanus|journal=Astronomy & Astrophysics|volume=547|pages=A61|last1=Smalley|first1=B|last2=Anderson|first2=D. R|last3=Collier-Cameron|first3=A|last4=Doyle|first4=A. P|last5=Fumel|first5=A|last6=Gillon|first6=M|last7=Hellier|first7=C|last8=Jehin|first8=E|last9=Lendl|first9=M|last10=Maxted|first10=P. F. L|last11=Pepe|first11=F|last12=Pollacco|first12=D|last13=Queloz|first13=D|last14=Ségransan|first14=D|last15=Smith|first15=A. M. S|last16=Southworth|first16=J|last17=Triaud|first17=A. H. M. J|last18=Udry|first18=S|last19=West|first19=R. G|year=2012|doi=10.1051/0004-6361/201219731|arxiv=1206.1177|s2cid=119233646 }} but modern studies suggest a lower radius of {{val|1.5795|0.0048|u=Jupiter radius}} and a temperature of {{val|1747|27|ul=K}}.
The planet is orbiting the host star at nearly-polar orbit with respect to star's equatorial plane, inclination being equal to −95.2{{±|0.9|1.0}}°.{{citation|arxiv=1610.00600|title=Rossiter–Mc Laughlin models and their effect on estimates of stellar rotation, illustrated using six WASP systems|year=2016|doi=10.1093/mnras/stw2316 |last1=Brown |first1=D. J. A. |last2=Triaud |first2=A. H. M. J. |last3=Doyle |first3=A. P. |last4=Gillon |first4=M. |last5=Lendl |first5=M. |last6=Anderson |first6=D. R. |last7=Collier Cameron |first7=A. |last8=Hébrard |first8=G. |last9=Hellier |first9=C. |last10=Lovis |first10=C. |last11=Maxted |first11=P. F. L. |last12=Pepe |first12=F. |last13=Pollacco |first13=D. |last14=Queloz |first14=D. |last15=Smalley |first15=B. |journal=Monthly Notices of the Royal Astronomical Society |volume=464 |pages=810–839 |doi-access=free }}
In 2019 and 2020, the transmission spectra of WASP-79b were taken utilizing HST and Spitzer Space Telescope, with best fit being the hazy atmosphere containing about 1% water{{citation|arxiv=2104.10688|year=2021|title=HST PanCET Program: A Complete Near-UV to Infrared Transmission Spectrum for the Hot Jupiter WASP-79b|doi=10.3847/1538-3881/ac0e99 |last1=Rathcke |first1=Alexander D. |last2=MacDonald |first2=Ryan J. |last3=Barstow |first3=Joanna K. |last4=Goyal |first4=Jayesh M. |last5=Lopez-Morales |first5=Mercedes |last6=Mendonça |first6=João M. |last7=Sanz-Forcada |first7=Jorge |last8=Henry |first8=Gregory W. |last9=Sing |first9=David K. |last10=Alam |first10=Munazza K. |last11=Lewis |first11=Nikole K. |last12=Chubb |first12=Katy L. |last13=Taylor |first13=Jake |last14=Nikolov |first14=Nikolay |last15=Buchhave |first15=Lars A. |journal=The Astronomical Journal |volume=162 |issue=4 |page=138 |bibcode=2021AJ....162..138R |s2cid=233347193 |doi-access=free }} and traces of Iron(I) hydride.{{cite journal|arxiv=1911.02051|last1=Smalley|first1=B.|title=Transmission Spectroscopy of WASP-79b from 0.6 to 5.0 μm|last2=Anderson|first2=D. R.|last3=Collier-Cameron|first3=A.|last4=Doyle|first4=A. P.|last5=Fumel|first5=A.|last6=Gillon|first6=M.|last7=Hellier|first7=C.|last8=Jehin|first8=E.|last9=Lendl|first9=M.|last10=Maxted|first10=P. F. L.|last11=Pepe|first11=F.|last12=Pollacco|first12=D.|last13=Queloz|first13=D.|last14=Segransan|first14=D.|last15=Smith|first15=A. M. S.|last16=Southworth|first16=J.|last17=Triaud|first17=A. H. M. J.|last18=Udry|first18=S.|last19=West|first19=R. G.|last20=Rathcke|first20=Alexander D.|last21=Sanz-Forcada|first21=Jorge|journal=The Astronomical Journal|year=2019|volume=159|page=5|doi=10.3847/1538-3881/ab5442|s2cid=207880528 |doi-access=free }}{{cite journal|arxiv=2005.09615|last1=Skaf|first1=Nour|author2=Michelle Fabienne Bieger|last3=Edwards|first3=Billy|last4=Changeat|first4=Quentin|last5=Morvan|first5=Mario|last6=Kiefer|first6=Flavien|last7=Blain|first7=Doriann|last8=Zingales|first8=Tiziano|last9=Poveda|first9=Mathilde|last10=Al-Refaie|first10=Ahmed|last11=Baeyens|first11=Robin|last12=Gressier|first12=Amelie|last13=Guilluy|first13=Gloria|author14=Adam Yassin Jaziri|last15=Modirrousta-Galian|first15=Darius|last16=Mugnai|first16=Lorenzo V.|last17=Pluriel|first17=William|last18=Whiteford|first18=Niall|last19=Wright|first19=Sam|author20=Kai Hou Yip|last21=Charnay|first21=Benjamin|last22=Leconte|first22=Jeremy|last23=Drossart|first23=Pierre|last24=Tsiaras|first24=Angelos|last25=Venot|first25=Olivia|last26=Waldmann|first26=Ingo|last27=Beaulieu|first27=Jean-Philippe|title=ARES. II. Characterizing the Hot Jupiters WASP-127 b, WASP-79 b, and WASP-62b with the Hubble Space Telescope|journal=The Astronomical Journal |year=2020|volume=160 |issue=3 |page=109 |doi=10.3847/1538-3881/ab94a3 |bibcode=2020AJ....160..109S |s2cid=218684714 |doi-access=free }} The presence of iron hydride was confirmed in 2021, along with tentative detection of vanadium oxide.{{citation|arxiv=2107.14334|year=2022|title=The Emission Spectrum of the Hot Jupiter WASP-79b from HST/WFC3|doi=10.3847/1538-3881/ac2f4a |last1=Foote |first1=Trevor O. |last2=Lewis |first2=Nikole K. |last3=Kilpatrick |first3=Brian M. |last4=Goyal |first4=Jayesh M. |last5=Bruno |first5=Giovanni |last6=Wakeford |first6=Hannah R. |last7=Robbins-Blanch |first7=Nina |last8=Kataria |first8=Tiffany |last9=MacDonald |first9=Ryan J. |last10=López-Morales |first10=Mercedes |last11=Sing |first11=David K. |last12=Mikal-Evans |first12=Thomas |last13=Bourrier |first13=Vincent |last14=Henry |first14=Gregory |last15=Buchhave |first15=Lars A. |journal=The Astronomical Journal |volume=163 |issue=1 |page=7 |bibcode=2022AJ....163....7F |s2cid=236635028 |doi-access=free }} Also, in 2022 an atmospheric sodium has been detected.{{citation|arxiv=2205.01623|year=2022|title=A survey of sodium absorption in 10 giant exoplanets with high-resolution transmission spectroscopy|doi=10.1093/mnras/stac1539 |last1=Langeveld |first1=Adam B. |last2=Madhusudhan |first2=Nikku |last3=Cabot |first3=Samuel H C. |journal=Monthly Notices of the Royal Astronomical Society |volume=514 |issue=4 |pages=5192–5213 |doi-access=free }}
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