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{{Short description|Extrasolar planet in the constellation Sextans}}
{{good article}} {{good article}}
{{Infobox planet
{{Planetbox begin
| name = WASP-43b | name = WASP-43b / Astrolábos
| image = File:Hot Gas-Giant Exoplanet WASP-43 b (Temperature Maps) (2024-117).jpg
}}
| caption = Temperature map of WASP-43b
{{Planetbox star
| discovery_ref = <ref name=Hellier2011/>
| discoverer = Coel Hellier ''et al.''
| discovery_site = ] / ]
| discovered = Published April 15, 2011
| discovery_method = ] (secondary occultation detected later)
| alt_names = Astrolábos<ref name="NEW2022"/>
| epoch = <!--J2000-->
| apsis = astron
| semimajor = 0.01526 (± 0.00018)<ref name=Gillon2012 /> ]
| eccentricity = < 0.0298 <ref name=Gillon2012 />
| period = 0.81347753 (± 0.00000071)<ref name=Gillon2012 /> ]
| inclination = 82.33 (± 0.20) <ref name=Gillon2012 />
| star = ] | star = ]
| mean_radius = 1.04 {{±|0.07|0.09}}<ref name=EPE /> {{Jupiter radius|link=y}}
| constell = ]
| mass = 2.03 (± 0.1)<ref name=EPE /> {{Jupiter mass|link=y}}
| RA = {{RA|10|19|38}}
| albedo = <0.06<ref name=Fraine2021/>
| DEC = {{DEC|-09|48|23}}
| single_temperature = 1666{{±|48}} ]
| app_mag = 12.4
| dist_pc = ~80<ref name=Hellier2011 />
| class = K7V<ref name=Hellier2011 />
| mass = 0.58 (± 0.05)<ref name=EPE />
| radius = 0.93 {{±|0.07|0.09}}<ref name=EPE />
| temperature = 4400 (± 200)<ref name=EPE />
| metallicity = -0.05 (± 0.17)<ref name=EPE />
| age = ?
}}
{{Planetbox orbit
| epoch = J2000
| semimajor = 0.0142 (± 0.0004)<ref name=EPE />
| eccentricity = 0 (adopted)<ref name=Hellier2011 />
| period = 0.813475<ref name=EPE />
| inclination = 82.6
}}
{{Planetbox character
| mass = 2.03 (± 0.1)<ref name=EPE />
| radius = 1.04 {{±|0.07|0.09}}<ref name=EPE />
}}
{{Planetbox discovery
| discovery_date = Published April 15, 2011<ref name=Hellier2011 />
| discoverers = Coel Hellier ''et al.''<ref name=Hellier2011 />
| discovery_method = ]<ref name=Hellier2011 /> (secondary occultation detected later)
| detection_methods = Radial velocity,<br>Reflection/emission modulations
| discovery_site = ] / ]
| discovery_status = Published
}} }}
'''WASP-43b''', formally named '''Astrolábos''',<ref name="NEW2022"/> is a ] ] in orbit around the young, active, and low-mass ] ] in the constellation ]. The planet is a ] with a mass twice that of ], but with a roughly equal radius. WASP-43b was flagged as a candidate by the ] program, before they conducted follow-ups using instruments at ] in Chile, which confirmed its existence and provided orbital and physical characteristics. The planet's discovery was published on April 14, 2011.<ref name=Hellier2011 />
{{Planetbox end}}


WASP-43b has an ] of approximately 0.8 days (19.2 hours), which at the time of discovery was the second-shortest known, surpassed only by ].<ref name=Hellier2011 /> At the time of its discovery, the size of WASP-43b's orbit was the smallest known for a hot Jupiter,<ref name=Hellier2011 /> probably due to its host star's low mass.
'''WASP-43b''' is a ] planet in orbit around the young, active, and low-mass star ] in the constellation ]. The planet is a ] with a mass twice that of Jupiter, and a radius equal to Jupiter's. WASP-43b was flagged as a candidate by the ] program before they conducted follow-ups using instruments at ] in Chile, which confirmed the planet's existence and provided orbital and physical characteristics. The planet's discovery was published on April 14, 2011.<ref name=Hellier2011 />


==Nomenclature==
At the time of its discovery, WASP-43b had an ] of approximately 0.8 days (19.2 hours), the second shortest orbit ever detected, surpassed only by ].<ref name=Hellier2011 /> In addition, at the time of discovery, WASP-43b was the most closely orbiting Hot Jupiter known,<ref name=Hellier2011 /> a phenomenon that can most likely be explained by its host star's low mass.
In August 2022, this planet and its host star were included among 20 systems to be named by the third ] 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=] |access-date=27 August 2022}}</ref> The approved names, proposed by a team from ], were announced in June 2023. WASP-43b is named '''Astrolábos''' and its host star is named '''Gnomon''', after the ] and the Greek word for the ].<ref name="NEW2022"/>

In 2014, secondary transit of the planet was reported. <ref>http://arxiv.org/abs/1401.3007</ref>


==Observational history== ==Observational history==

WASP-43 was first flagged as host to a potential ] event (when a body crosses in front of and dims its host star) by data collected by ], a British organization working to discover transiting planets across the entirety of the sky. In particular, WASP-43 was observed first by the leg of WASP-South at the ] between January and May 2009.<ref name=Hellier2011 /> WASP-43 was first flagged as host to a potential ] event (when a body crosses in front of and dims its host star) by data collected by ], a British organization working to discover transiting planets across the entirety of the sky. In particular, WASP-43 was observed first by the leg of WASP-South at the ] between January and May 2009.<ref name=Hellier2011 />


Later observation by both SuperWASPs in the Northern and Southern Hemispheres led to the collection of 13,768 data points between January and May 2010 and to the use of the ] at ] in Chile. Fourteen measurements using the ] confirmed WASP-43b as a planet, revealing its mass in the process. The use of La Silla's ] telescope helped the science team working on the planet to create a ] of the planet's transit in December 2010.<ref name=Hellier2011 /> Later observation by both SuperWASPs in the ] and ]s led to the collection of 13,768 data points between January and May 2010 and to the use of the ] at ] in Chile. Fourteen measurements using the ] confirmed WASP-43b as a planet, revealing its mass in the process. The use of La Silla's ] telescope helped the science team working on the planet to create a ] of the planet's transit in December 2010.<ref name=Hellier2011 />


The initial discovery was published in the journal '']'' in 2011.<ref name=Hellier2011 /> This was followed by reporting of a second transit in 2014,<ref>{{Cite journal |arxiv = 1401.3007|bibcode = 2014A&A...563A..40C|title = Broad-band transmission spectrum and K-band thermal emission of WASP-43b as observed from the ground|journal = Astronomy and Astrophysics|volume = 563|pages = A40|last1 = Chen|first1 = G|last2 = Van Boekel|first2 = R|last3 = Wang|first3 = H|last4 = Nikolov|first4 = N|last5 = Fortney|first5 = J. J|last6 = Seemann|first6 = U|last7 = Wang|first7 = W|last8 = Mancini|first8 = L|last9 = Henning|first9 = Th|s2cid = 21723907|year = 2014|doi = 10.1051/0004-6361/201322740}}</ref> and a full observation of the phases of the planet later that year.<ref>{{Cite web | url=http://www.nasa.gov/press/2014/october/nasas-hubble-maps-the-temperature-and-water-vapor-on-an-extreme-exoplanet/index.html | title=Hubble Maps the Temperature and Water Vapor on an Extreme Exoplanet| date=2015-04-22}}</ref>
The planet's discovery was published in the journal '']'' on April 14, 2011.<ref name=Hellier2011 />


==Host star== ==Host star==
{{main|WASP-43}} {{main|WASP-43}}
WASP-43 is a ] star in the ] constellation that is about 80 ]s (261 ]s) away.<ref name=Hellier2011 /> The star has a ] of 0.58 times that of the Sun, but is more diffuse with a ] of 0.93 times that of the Sun. The star's ] is 4400 ], making the star cooler than the Sun, and is metal-poor with regards to the Sun because it has a ] of = −0.05 (89% the amount of iron in the Sun).<ref name=EPE /> The star is young, and is estimated to be 598 million years old (as compared to the Sun's 4.6 billion years).<ref name=EPE /> Analysis of emission lines have indicated that WASP-43 is an active star.<ref name=Hellier2011 /> WASP-43 is a ] star in the ] constellation that is about 80 ]s (261 ]s) away.<ref name=Hellier2011 /> The star has a ] 0.58 times that of the Sun, but is more diffuse, with a ] 0.93 times that of the Sun. The star's ] is 4,400 ], making the star cooler than the Sun, and is metal-poor with regards to the Sun because it has a ] of = −0.05 (89% the amount of iron in the Sun).<ref name=EPE /> The star is young, and is estimated to be 598 million years old (as compared to the Sun's 4.6 billion years).<ref name=EPE /> Analysis of emission lines indicate that WASP-43 is an active star.<ref name=Hellier2011 />


WASP-43 has one detected planet in its orbit, WASP-43b. The star has an ] of 12.4, and thus is too faint to be seen with the unaided eye from Earth.<ref name=EPE /> WASP-43 has one detected planet in its orbit, WASP-43b. The star has an ] of 12.4, and thus is too faint to be seen with the unaided eye from Earth.<ref name=EPE />


==Characteristics== ==Characteristics==
]
WASP-43b is a dense ] with a mass 2.05 times the ], but a ] 1.036 times that of Jupiter's. The planet orbits its host star at a ] of 0.01526 ] every 0.813478 days (19.5235 hours);<ref name=EPE /> this ], at the time of WASP-43b's discovery, was the second-shortest orbit yet detected, surpassed only by ]. In comparison, ] has an orbital period of 87.97 days and lies at a mean distance of 0.387 AU from the Sun.<ref name="Mercury" /> In addition, WASP-43b had the closest orbit to its host star (among hot Jupiters) at the time of its discovery, comparable only to the ] planet ] and to the planetary candidate orbiting KOI-961 (confirmed a year later as ]). While hot Jupiters are known to have small orbital periods, planets with ''exceptionally'' small periods below three or four days are extremely rare; however, in the case of WASP-43b, the planet's proximity can be explained because its host star has a very low mass. The rarity of systems like that of WASP-43 and its planet suggest that hot Jupiters do not usually occur around low-mass stars, or that such planets cannot maintain stable orbits around such stars.<ref name=Hellier2011 />


WASP-43b, along with the planets WASP-19b and ], conflicted with currently accepted models of tidal movements derived from observations of the orbits of ] systems. Revisions to the model with regard to planets were proposed to help the models conform to the orbital parameters of these planets.<ref name=Hellier2011 /> No orbital decay driven by tidal dissipation was detected in 2016, placing a lower limit of 10 million years on the remaining planetary lifetime.<ref>{{cite journal|arxiv=1603.01144|doi=10.3847/0004-6256/151/6/137|title=Ruling Out the Orbital Decay of the Wasp-43B Exoplanet|year=2016|last1=Hoyer|first1=Sergio|last2=Pallé|first2=Enric|last3=Dragomir|first3=Diana|last4=Murgas |first4=Felipe|s2cid=119201679|journal=The Astronomical Journal|volume=151|issue=6|page=137|bibcode=2016AJ....151..137H |doi-access=free }}</ref> Updated orbital period measurements have failed to detect orbital decay as of 2021.<ref>{{citation|arxiv=2110.04761|title=Is the orbit of the exoplanet WASP-43b really decaying? TESS and MuSCAT2 observations confirm no detection|year=2021|doi=10.1093/mnras/stab2929 |last1=Garai |first1=Z. |last2=Pribulla |first2=T. |last3=Parviainen |first3=H. |last4=Pallé |first4=E. |last5=Claret |first5=A. |last6=Szigeti |first6=L. |last7=Béjar |first7=V J S. |last8=Casasayas-Barris |first8=N. |last9=Crouzet |first9=N. |last10=Fukui |first10=A. |last11=Chen |first11=G. |last12=Kawauchi |first12=K. |last13=Klagyivik |first13=P. |last14=Kurita |first14=S. |last15=Kusakabe |first15=N. |last16=De Leon |first16=J. P. |last17=Livingston |first17=J. H. |last18=Luque |first18=R. |last19=Mori |first19=M. |last20=Murgas |first20=F. |last21=Narita |first21=N. |last22=Nishiumi |first22=T. |last23=Oshagh |first23=M. |last24=Szabó |first24=Gy M. |last25=Tamura |first25=M. |last26=Terada |first26=Y. |last27=Watanabe |first27=N. |journal=Monthly Notices of the Royal Astronomical Society |volume=508 |issue=4 |pages=5514–5523 |doi-access=free }}</ref><ref>{{citation|arxiv=2111.03346|year=2021|title=Investigation of Orbital Decay and Global Modeling of the Planet WASP-43 B|doi=10.3847/1538-3881/ac1baf |last1=Davoudi |first1=Fatemeh |last2=Baştürk |first2=Özgür |last3=Yalçınkaya |first3=Selçuk |last4=Esmer |first4=Ekrem M. |last5=Safari |first5=Hossein |journal=The Astronomical Journal |volume=162 |issue=5 |page=210 |bibcode=2021AJ....162..210D |s2cid=239464886 |doi-access=free }}</ref>
WASP-43b is a dense ] with a mass of 1.78 times the ], but a ] of 0.93 times that of Jupiter's. The planet orbits its host star at a ] of 0.0142 ] every 0.813475 days (19.5234 hours);<ref name=EPE /> this ], at the time of WASP-43b's discovery, was the second-shortest orbit yet detected, surpassed only by ]. In addition, WASP-43b had the closest orbit to its host star (among Hot Jupiters) at the time of its discovery, comparable only to the ] planet ] and to the planetary candidate orbiting KOI-961. While Hot Jupiters are known to have small orbital periods, planets with ''exceptionally'' small periods below three or four days are extremely rare; however, in the case of WASP-43b, the planet's proximity can be explained because its host star has a very low mass. The rarity of systems like that of WASP-43 and its planet suggest that Hot Jupiters do not usually occur around low-mass stars, or that such planets cannot maintain stable orbits around such stars.<ref name=Hellier2011 />
== Atmosphere ==
In 2019, the spectrum of WASP-43b was taken, with the best fit being water-containing clouds without significant amounts of alkali metals.<ref>{{cite journal|arxiv=1911.03358|last1=Chen|first1=Guo|title=ACCESS: A Visual to Near-infrared Spectrum of the Hot Jupiter WASP-43b with Evidence of H<sub>2</sub>O, but no evidence of Na or K|author2=Roy van Boekel|last3=Wang|first3=Hongchi|last4=Nikolov|first4=Nikolay|last5=Fortney|first5=Jonathan J.|last6=Seemann|first6=Ulf|last7=Wang|first7=Wei|last8=Mancini|first8=Luigi|last9=Henning|first9=Thomas|last10=Alam|first10=Munazza K.|last11=Kirk|first11=James|last12=McGruder|first12=Chima|last13=Rodler|first13=Florian|last14=Fienco|first14=Jennifer|s2cid=207847873|journal=The Astronomical Journal|year=2019|volume=159|pages=13|doi=10.3847/1538-3881/ab55da |doi-access=free }}</ref>
In 2020, further analysis of the spectra revealed the presence of bivalent aluminum oxide (AlO) and water in the atmosphere,<ref>{{cite journal|arxiv=2004.13679|last1=Chubb|first1=Katy L.|last2=Min|first2=Michiel|last3=Kawashima|first3=Yui|last4=Helling|first4=Christiane|last5=Waldmann|first5=Ingo|s2cid=216562466|title=Aluminium oxide in the atmosphere of hot Jupiter WASP-43b|journal=Astronomy & Astrophysics|year=2020|volume=639|pages=A3|doi=10.1051/0004-6361/201937267|bibcode=2020A&A...639A...3C}}</ref> while carbon monoxide, carbon dioxide and methane were not detected. Climate modelling suggests the carbon monoxide concentration may be variable, while the atmospheric spectrum of WASP-43b is dominated by clouds made of refractory mineral particles, with a small contribution from hydrocarbon haze.<ref>{{cite journal|arxiv=2005.14595|last1=Helling|first1=Ch.|last2=Kawashima|first2=Y.|last3=Graham|first3=V.|last4=Samra|first4=D.|last5=Chubb|first5=K. L.|last6=Min|first6=M.|last7=Waters|first7=L. B. F. M.|last8=Parmentier|first8=V.|title=Mineral cloud and hydrocarbon haze particles in the atmosphere of the hot Jupiter JWST target WASP-43b|journal=Astronomy & Astrophysics|year=2020|volume=641|pages=A178|doi=10.1051/0004-6361/202037633|bibcode=2020A&A...641A.178H|s2cid=219124472}}</ref> Carbon to oxygen ratio in the planet (0.75{{±|0.15}}) is elevated compared to the Solar ratio of 0.55.<ref>{{citation|arxiv=2206.09738|year=2022|title=Exoplanet Atmosphere Retrievals in 3D Using Phase Curve Data with ARCiS: Application to WASP-43b|doi=10.1051/0004-6361/202142800 |last1=Chubb |first1=Katy L. |last2=Min |first2=Michiel |journal=Astronomy & Astrophysics |volume=665 |pages=A2 |bibcode=2022A&A...665A...2C |s2cid=249560548 }}</ref> The planet is very dark overall, with no clouds on the dayside<ref name=Murphy2022/> and an albedo below 0.06.<ref name=Fraine2021/> In 2024, the James Webb Telescope observed that the skies are clear on the day side and is cloudy on its night side, with winds of 5,000 miles per hour.<ref>{{Cite web |title=NASA's Webb Maps Weather on Planet 280 Light-Years Away - NASA Science |url=https://science.nasa.gov/missions/webb/nasas-webb-maps-weather-on-planet-280-light-years-away/ |access-date=2024-04-30 |website=science.nasa.gov |language=en-US}}</ref>


There is a large difference in temperature between dayside (1479{{±|13}} ]) and nightside (755{{±|46}} ]).<ref name=Murphy2022/>
WASP-43b, along with the planets WASP-19b and ], conflicted with currently accepted models of tidal movements derived from observations of the orbits of ] systems. Revisions to the model with regard to planets were proposed to help the models conform to the orbital parameters of these planets.<ref name=Hellier2011 />

In comparison, planet ] has an orbital period of 87.97 days and lies at a mean distance of 0.387 AU from the Sun.<ref name=Mercury />


==External links== ==External links==
* {{CelestialRefEx|WASP-43b}} * {{cite simbad|title=WASP-43b}}
*
* {{cite web |url=https://www.youtube.com/watch?v=n-oDqYCf3XY |title=Hubble Hangout on planet WASP-43b |website=] |year=2014 |access-date=7 Nov 2014}}


==References== ==References==
{{reflist|refs=
<ref name=EPE>{{cite encyclopedia |url=http://www.exoplanet.eu/star.php?st=WASP-43 |archive-url=https://web.archive.org/web/20110505005400/http://exoplanet.eu/star.php?st=WASP-43 |url-status=dead |archive-date=May 5, 2011 |title=Notes for star WASP-43 |author=Jean Schneider |year=2011 |encyclopedia=] |access-date=7 May 2011}}</ref>


<ref name=Hellier2011>{{cite journal |last1=Hellier |first1=C. |last2=Anderson |first2=D.R. |s2cid=70287736 |year=2011 |title=WASP-43b: The closest-orbiting hot Jupiter |journal=] |volume= 535|pages= L7|doi= 10.1051/0004-6361/201117081|arxiv=1104.2823 |bibcode = 2011A&A...535L...7H }}</ref>
{{reflist|refs=

<ref name=Mercury>{{cite web|url=http://nssdc.gsfc.nasa.gov/planetary/factsheet/mercuryfact.html |title=Mercury Fact Sheet |author=David Williams |date=17 November 2010 |website=] |publisher=] |access-date=7 May 2011 |url-status=dead |archive-url=https://web.archive.org/web/20151106171436/http://nssdc.gsfc.nasa.gov/planetary/factsheet/mercuryfact.html |archive-date=6 November 2015 }}</ref>

<ref name=Gillon2012>{{cite journal |last1=Gillon |first1=M. |last2=Triaud |first2=A.H.M.J. |s2cid=50880195 |year=2012 |title=The TRAPPIST survey of southern transiting planets. I. Thirty eclipses of the ultra-short period planet WASP-43 b |journal=] |volume=542 |issue=A4 |pages= A4|doi=10.1051/0004-6361/201218817 |arxiv=1201.2789 |bibcode = 2012A&A...542A...4G }}</ref>

<ref name=Fraine2021>{{citation|arxiv=2103.16676|year=2021|title=The Dark World: A Tale of WASP-43b in Reflected Light with HST WFC3/UVIS|last1=Fraine|first1=Jonathan|last2=Mayorga|first2=Laura C.|last3=Stevenson|first3=Kevin B.|last4=Lewis|first4=Nikole|last5=Kataria|first5=Tiffany|last6=Bean|first6=Jacob|last7=Bruno|first7=Giovanni|last8=Fortney|first8=Jonathan J.|last9=Kreidberg|first9=Laura|last10=Morley|first10=Caroline V.|last11=Mouawad|first11=Nelly|last12=Todorov|first12=Kamen O.|last13=Parmentier|first13=Vivien|last14=Wakeford|first14=Hannah R.|last15=Katherina Feng|first15=Y.|last16=Kilpatrick|first16=Brian M.|last17=Line|first17=Michael R.|journal=The Astronomical Journal |volume=161 |issue=6 |page=269 |doi=10.3847/1538-3881/abe8d6 |bibcode=2021AJ....161..269F |s2cid=232428234 |doi-access=free }}</ref>


<ref name=Murphy2022>{{citation|arxiv=2212.03240|year=2023|title=A Lack of Variability between Repeated Spitzer Phase Curves of WASP-43b|last1=Murphy |first1=Matthew M. |last2=Beatty |first2=Thomas G. |last3=Roman |first3=Michael T. |last4=Malsky |first4=Isaac |last5=Wingate |first5=Alex |last6=Ochs |first6=Grace |last7=Cinque |first7=L. |last8=Beltz |first8=Hayley |last9=Rauscher |first9=Emily |last10=Kempton |first10=Emiza M. -R. |last11=Stevenson |first11=Kevin B. |journal=The Astronomical Journal |volume=165 |issue=3 |page=107 |doi=10.3847/1538-3881/acaec5 |bibcode=2023AJ....165..107M |s2cid=254275218 |doi-access=free }}</ref>
*<ref name=EPE>
{{cite web |url=http://www.exoplanet.eu/star.php?st=WASP-43 |title=Notes for star WASP-43 |author=Jean Schneider |year=2011 |work= |publisher=] |accessdate=7 May 2011}}</ref>


<ref name="NEW2022">{{cite web |url=https://www.nameexoworlds.iau.org/2022approved-names |title=2022 Approved Names |website=nameexoworlds.iau.org |publisher=] |access-date=7 June 2023}}</ref>
*<ref name=Hellier2011>
{{cite journal |last1=Hellier |first1=C. |last2=Anderson |first2=D.R. |year=2011 |title=WASP-43b: The closest-orbiting hot Jupiter |journal=] |volume= |issue= |pages= |publisher=] |doi= |arxiv=1104.2823 |bibcode = 2011arXiv1104.2823H }}</ref>


*<ref name=Mercury>
{{cite web |url=http://nssdc.gsfc.nasa.gov/planetary/factsheet/mercuryfact.html |title=Mercury Fact Sheet |author=David Williams |date=17 November 2010 |work=] |publisher=] |accessdate=7 May 2011}}</ref>
}} }}


{{Sextans}}
{{2011 in space}}


{{DEFAULTSORT:WASP-43b}}
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Latest revision as of 00:21, 2 September 2024

Extrasolar planet in the constellation Sextans

WASP-43b / Astrolábos
Temperature map of WASP-43b
Discovery
Discovered byCoel Hellier et al.
Discovery siteLa Silla Observatory / South African Astronomical Observatory
Discovery datePublished April 15, 2011
Detection methodtransit method (secondary occultation detected later)
Designations
Alternative namesAstrolábos
Orbital characteristics
Semi-major axis0.01526 (± 0.00018) AU
Eccentricity< 0.0298
Orbital period (sidereal)0.81347753 (± 0.00000071) d
Inclination82.33 (± 0.20)
StarWASP-43
Physical characteristics
Mean radius1.04
−0.09 RJ
Mass2.03 (± 0.1) MJ
Albedo<0.06
Temperature1666±48 K

WASP-43b, formally named Astrolábos, is a transiting planet in orbit around the young, active, and low-mass star WASP-43 in the constellation Sextans. The planet is a hot Jupiter with a mass twice that of Jupiter, but with a roughly equal radius. WASP-43b was flagged as a candidate by the SuperWASP program, before they conducted follow-ups using instruments at La Silla Observatory in Chile, which confirmed its existence and provided orbital and physical characteristics. The planet's discovery was published on April 14, 2011.

WASP-43b has an orbital period of approximately 0.8 days (19.2 hours), which at the time of discovery was the second-shortest known, surpassed only by WASP-19b. At the time of its discovery, the size of WASP-43b's orbit was the smallest known for a hot Jupiter, probably due to its host star's low mass.

Nomenclature

In August 2022, this planet and its host star were included among 20 systems to be named by the third NameExoWorlds project. The approved names, proposed by a team from Romania, were announced in June 2023. WASP-43b is named Astrolábos and its host star is named Gnomon, after the gnomon and the Greek word for the astrolabe.

Observational history

WASP-43 was first flagged as host to a potential transiting event (when a body crosses in front of and dims its host star) by data collected by SuperWASP, a British organization working to discover transiting planets across the entirety of the sky. In particular, WASP-43 was observed first by the leg of WASP-South at the South African Astronomical Observatory between January and May 2009.

Later observation by both SuperWASPs in the Northern and Southern Hemispheres led to the collection of 13,768 data points between January and May 2010 and to the use of the CORALIE spectrograph at La Silla Observatory in Chile. Fourteen measurements using the radial velocity method confirmed WASP-43b as a planet, revealing its mass in the process. The use of La Silla's TRAPPIST telescope helped the science team working on the planet to create a light curve of the planet's transit in December 2010.

The initial discovery was published in the journal Astronomy and Astrophysics in 2011. This was followed by reporting of a second transit in 2014, and a full observation of the phases of the planet later that year.

Host star

Main article: WASP-43

WASP-43 is a K-type star in the Sextans constellation that is about 80 parsecs (261 light years) away. The star has a mass 0.58 times that of the Sun, but is more diffuse, with a radius 0.93 times that of the Sun. The star's effective temperature is 4,400 K, making the star cooler than the Sun, and is metal-poor with regards to the Sun because it has a metallicity of = −0.05 (89% the amount of iron in the Sun). The star is young, and is estimated to be 598 million years old (as compared to the Sun's 4.6 billion years). Analysis of emission lines indicate that WASP-43 is an active star.

WASP-43 has one detected planet in its orbit, WASP-43b. The star has an apparent magnitude of 12.4, and thus is too faint to be seen with the unaided eye from Earth.

Characteristics

Artist's concept of WASP-43b

WASP-43b is a dense hot Jupiter with a mass 2.05 times the mass of Jupiter, but a radius 1.036 times that of Jupiter's. The planet orbits its host star at a mean distance of 0.01526 AU every 0.813478 days (19.5235 hours); this orbital period, at the time of WASP-43b's discovery, was the second-shortest orbit yet detected, surpassed only by WASP-19b. In comparison, Mercury has an orbital period of 87.97 days and lies at a mean distance of 0.387 AU from the Sun. In addition, WASP-43b had the closest orbit to its host star (among hot Jupiters) at the time of its discovery, comparable only to the super-Earth planet GJ 1214 b and to the planetary candidate orbiting KOI-961 (confirmed a year later as Kepler-42). While hot Jupiters are known to have small orbital periods, planets with exceptionally small periods below three or four days are extremely rare; however, in the case of WASP-43b, the planet's proximity can be explained because its host star has a very low mass. The rarity of systems like that of WASP-43 and its planet suggest that hot Jupiters do not usually occur around low-mass stars, or that such planets cannot maintain stable orbits around such stars.

WASP-43b, along with the planets WASP-19b and WASP-18b, conflicted with currently accepted models of tidal movements derived from observations of the orbits of binary star systems. Revisions to the model with regard to planets were proposed to help the models conform to the orbital parameters of these planets. No orbital decay driven by tidal dissipation was detected in 2016, placing a lower limit of 10 million years on the remaining planetary lifetime. Updated orbital period measurements have failed to detect orbital decay as of 2021.

Atmosphere

In 2019, the spectrum of WASP-43b was taken, with the best fit being water-containing clouds without significant amounts of alkali metals. In 2020, further analysis of the spectra revealed the presence of bivalent aluminum oxide (AlO) and water in the atmosphere, while carbon monoxide, carbon dioxide and methane were not detected. Climate modelling suggests the carbon monoxide concentration may be variable, while the atmospheric spectrum of WASP-43b is dominated by clouds made of refractory mineral particles, with a small contribution from hydrocarbon haze. Carbon to oxygen ratio in the planet (0.75±0.15) is elevated compared to the Solar ratio of 0.55. The planet is very dark overall, with no clouds on the dayside and an albedo below 0.06. In 2024, the James Webb Telescope observed that the skies are clear on the day side and is cloudy on its night side, with winds of 5,000 miles per hour.

There is a large difference in temperature between dayside (1479±13 K) and nightside (755±46 K).

External links

References

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