WASP-41

{{Starbox observe

| epoch = J2000

| ra = {{RA|12|42|28.4950}}

| dec = {{DEC|-30|38|23.529}}

| appmag_v = 11.6{{citation|arxiv=1512.05549|title=High-precision photometry by telescope defocussing. III. WASP-22, WASP-41, WASP-42 and WASP-55|year=2015|doi=10.1093/mnras/stw279|last1=Southworth|first1=John|last2=Tregloan-Reed|first2=J.|last3=Andersen|first3=M. I.|last4=Calchi Novati|first4=S.|last5=Ciceri|first5=S.|last6=Colque|first6=J. P.|last7=D'Ago|first7=G.|last8=Dominik|first8=M.|last9=Evans|first9=D.|last10=Gu|first10=S. -H.|last11=Herrera-Cruces|first11=A.|last12=Hinse|first12=T. C.|last13=Jorgensen|first13=U. G.|last14=Juncher|first14=D.|last15=Kuffmeier|first15=M.|last16=Mancini|first16=L.|last17=Peixinho|first17=N.|last18=Popovas|first18=A.|last19=Rabus|first19=M.|last20=Skottfelt|first20=J.|last21=Tronsgaard|first21=R.|last22=Unda-Sanzana|first22=E.|last23=Wang|first23=X. -B.|last24=Wertz|first24=O.|last25=Alsubai|first25=K. A.|last26=Andersen|first26=J. M.|last27=Bozza|first27=V.|last28=Bramich|first28=D. M.|last29=Burgdorf|first29=M.|last30=Damerdji|first30=Y.|doi-access=free |s2cid=44864064|display-authors=29}}

}}

{{Starbox character

| type = main-sequence star

| class = G8V

}}

{{Starbox astrometry

| radial_v = 4.153{{cite Gaia DR3|6160877943251930368}}

| prop_mo_ra = 14.878

| prop_mo_dec = 11.988

| parallax = 6.1193

| p_error = 0.0203

| parallax_footnote =

}}

{{Starbox detail

| mass = 0.930{{±|0.030}}

| radius = 0.900{{±|0.050}}

| temperature = 5,450{{±|150}}

| luminosity = 0.65

| gravity = 4.48

| metal_fe = −0.080{{±|0.090}}

| rotation = 18.4 d

| rotational_velocity = 1.50{{±|0.05}}

| age_gyr = 2.289{{±|0.077}}{{citation|arxiv=2006.07880|title=TATOO: Tidal-chronology standalone tool to estimate the age of massive close-in planetary systems|year=2020|doi=10.1051/0004-6361/202038058|last1=Gallet|first1=F.|author2=Gallet|journal=Astronomy & Astrophysics|volume=641|pages=A38|bibcode=2020A&A...641A..38G|s2cid=219687851}}

}}

{{Starbox catalog

| names = {{odlist|CD=-29 98732|2MASS = J12422849-3038235|GSC=07247-00587|TYC=7247-587-1}}{{cite simbad|title=CD-29 9873|access-date=2020-12-22}}

}}

{{Starbox reference

| Simbad = CD-29 9873

}}

WASP-41 is a G-type main-sequence star. Its surface temperature is 5450{{±|150}} K. WASP-41 is similar to the Sun in its concentration of heavy elements, with a metallicity Fe/H index of −0.080{{±|0.090}}, but is much younger at an age of 2.289{{±|0.077}} billion years. The star does exhibit strong starspot activity, with spots covering 3% of the stellar surface.

Multiplicity surveys did not detect any stellar companions as of 2017.{{citation|arxiv=1709.07476|title=High-resolution Imaging of Transiting Extrasolar Planetary systems (HITEP). II. Lucky Imaging results from 2015 and 2016|year=2018|doi=10.1051/0004-6361/201731855|last1=Evans|first1=D. F.|last2=Southworth|first2=J.|last3=Smalley|first3=B.|last4=Jørgensen|first4=U. G.|last5=Dominik|first5=M.|last6=Andersen|first6=M. I.|last7=Bozza|first7=V.|last8=Bramich|first8=D. M.|last9=Burgdorf|first9=M. J.|last10=Ciceri|first10=S.|last11=d'Ago|first11=G.|last12=Figuera Jaimes|first12=R.|last13=Gu|first13=S.-H.|last14=Hinse|first14=T. C.|last15=Henning|first15=Th.|last16=Hundertmark|first16=M.|last17=Kains|first17=N.|last18=Kerins|first18=E.|last19=Korhonen|first19=H.|last20=Kokotanekova|first20=R.|last21=Kuffmeier|first21=M.|last22=Longa-Peña|first22=P.|last23=Mancini|first23=L.|last24=MacKenzie|first24=J.|last25=Popovas|first25=A.|last26=Rabus|first26=M.|last27=Rahvar|first27=S.|last28=Sajadian|first28=S.|last29=Snodgrass|first29=C.|last30=Skottfelt|first30=J.|journal=Astronomy & Astrophysics|volume=610|pages=A20|bibcode=2018A&A...610A..20E|s2cid=53400492|display-authors=29}}

Planetary system

In 2012, one planet, named WASP-41b, was discovered on a tight, circular orbit.{{citation|arxiv=1012.2977|title=WASP-41 b: A transiting hot Jupiter planet orbiting a magnetically-active G8 V star|year=2010|doi=10.1086/660007|last1=Maxted|first1=P. F. L.|last2=Anderson|first2=D. R.|last3=Collier Cameron|first3=A.|last4=Hellier|first4=C.|last5=Queloz|first5=D.|last6=Smalley|first6=B.|last7=Street|first7=R. A.|last8=Triaud|first8=A. H. M. J.|last9=West|first9=R. G.|last10=Gillon|first10=M.|last11=Lister|first11=T. A.|last12=Pepe|first12=F.|last13=Pollacco|first13=D.|last14=Ségransan|first14=D.|last15=Smith|first15=A. M. S.|last16=Udry|first16=S.|journal=Publications of the Astronomical Society of the Pacific|volume=123|issue=903|pages=547–554|s2cid=40017204}} The transmission spectrum taken in 2017 was gray and featureless. No atmospheric constituents could be distinguished.{{citation|arxiv=1710.11209|title=PyTranSpot- A tool for multiband light curve modeling of planetary transits and stellar spots|year=2018|doi=10.1051/0004-6361/201731345|last1=Juvan|first1=Ines G.|last2=Lendl|first2=M.|last3=Cubillos|first3=P. E.|last4=Fossati|first4=L.|last5=Tregloan-Reed|first5=J.|last6=Lammer|first6=H.|last7=Guenther|first7=E. W.|last8=Hanslmeier|first8=A.|journal=Astronomy & Astrophysics|volume=610|pages=A15|bibcode=2018A&A...610A..15J|s2cid=55138492}} The planetary orbit of WASP-41b is slightly misaligned with the equatorial plane of the star, at a misalignment angle of 9.15{{±|2.85|2.62}}°.{{citation |arxiv=1809.01027 |title=Activity induced variation in spin-orbit angles as derived from Rossiter-McLaughlin measurements |year=2018 |doi=10.1051/0004-6361/201833709 |last1=Oshagh |first1=M. |last2=Triaud |first2=A. H. M. J. |last3=Burdanov |first3=A. |last4=Figueira |first4=P. |last5=Reiners |first5=Ansgar |last6=Santos |first6=N. C. |last7=Faria |first7=J. |last8=Boue |first8=G. |last9=Díaz |first9=R. F. |last10=Dreizler |first10=S. |last11=Boldt |first11=S. |last12=Delrez |first12=L. |last13=Ducrot |first13=E. |last14=Gillon |first14=M. |last15=Guzman Mesa |first15=A. |last16=Jehin |first16=E. |last17=Khalafinejad |first17=S. |last18=Kohl |first18=S. |last19=Serrano |first19=L. |last20=Udry |first20=S. |journal=Astronomy & Astrophysics |volume=619 |pages=A150 |bibcode=2018A&A...619A.150O |s2cid=54578441 }} Planetary equilibrium temperature is 1242{{±|12}} K.

Another planet, WASP-41c, was discovered in 2015.{{cite journal | title=Hot Jupiters with relatives: Discovery of additional planets in orbit around WASP-41 and WASP-47 | url=https://www.aanda.org/articles/aa/full_html/2016/02/aa26965-15/aa26965-15.html | last1=Neveu-VanMalle | first1=M. | last2=Queloz | first2=D. | last3=Anderson | first3=D. R. | last4=Brown | first4=D. J. A. | last5=Collier Cameron | first5=A. | last6=Delrez | first6=L. | last7=Díaz | first7=R. F. | last8=Gillon | first8=M. | last9=Hellier | first9=C. | last10=Jehin | first10=E. | last11=Lister | first11=T. | last12=Pepe | first12=F. | last13=Rojo | first13=P. | last14=Ségransan | first14=D. | last15=Triaud | first15=A. H. M. J. | last16=Turner | first16=O. D. | last17=Udry | first17=S. | display-authors=1 | journal=Astronomy and Astrophysics | volume=586 | at=A93 | year=2016 | arxiv=1509.07750 | bibcode=2016A&A...586A..93N | doi=10.1051/0004-6361/201526965 | s2cid=53354547 }} The planets are too far apart to significantly affect each other's orbits.{{citation|arxiv=1710.11140|title=How do External Companions Affect Spin-Orbit Misalignment of Hot Jupiters?|year=2018|doi=10.1093/mnras/sty133|last1=Lai|first1=Dong|last2=Anderson|first2=Kassandra R.|last3=Pu|first3=Bonan|journal=Monthly Notices of the Royal Astronomical Society|volume=475|issue=4|pages=5231–5236|doi-access=free |bibcode=2018MNRAS.475.5231L|s2cid=119066265}} The planetary equilibrium temperature of WASP-41c is 247{{±|5}} K.

{{OrbitboxPlanet begin

| name = WASP-41

| table_ref ={{citation|arxiv=1704.00373|title=The GAPS Programme with HARPS-N@TNG XIV. Investigating giant planet migration history via improved eccentricity and mass determination for 231 transiting planets|year=2017|doi=10.1051/0004-6361/201629882|last1=Bonomo|first1=A. S.|last2=Desidera|first2=S.|last3=Benatti|first3=S.|last4=Borsa|first4=F.|last5=Crespi|first5=S.|last6=Damasso|first6=M.|last7=Lanza|first7=A. F.|last8=Sozzetti|first8=A.|last9=Lodato|first9=G.|last10=Marzari|first10=F.|last11=Boccato|first11=C.|last12=Claudi|first12=R. U.|last13=Cosentino|first13=R.|last14=Covino|first14=E.|last15=Gratton|first15=R.|last16=Maggio|first16=A.|last17=Micela|first17=G.|last18=Molinari|first18=E.|last19=Pagano|first19=I.|last20=Piotto|first20=G.|last21=Poretti|first21=E.|last22=Smareglia|first22=R.|last23=Affer|first23=L.|last24=Biazzo|first24=K.|last25=Bignamini|first25=A.|last26=Esposito|first26=M.|last27=Giacobbe|first27=P.|last28=Hébrard|first28=G.|last29=Malavolta|first29=L.|last30=Maldonado|first30=J.|journal=Astronomy & Astrophysics|volume=A107|page=602|bibcode=2017A&A...602A.107B|s2cid=118923163|display-authors=29}}

}}

{{OrbitboxPlanet

| exoplanet = b

| mass = 0.941{{±|0.065|0.064}}

| radius = 1.200{{±|0.060}}

| semimajor = 0.04022{{±|0.00044}}

| period = 3.0524010{{±|0.000004}}

| eccentricity = <0.12

| inclination = 87.700{{±|0.080}}

}}

{{OrbitboxPlanet

| exoplanet = c{{citation|arxiv=1710.01737|year=2017|doi=10.3847/1538-3881/aa9176|last1=Becker|first1=Juliette C.|last2=Vanderburg|first2=Andrew|last3=Adams|first3=Fred C.|last4=Khain|first4=Tali|last5=Bryan|first5=Marta|title=Exterior Companions to Hot Jupiters Orbiting Cool Stars Are Coplanar|journal=The Astronomical Journal|volume=154|issue=6|page=230|bibcode=2017AJ....154..230B|s2cid=119198122 |doi-access=free }}

| mass = >3.2{{±|0.20}}

| radius =

| semimajor = 1.36{{±|0.04}}

| period = 421{{±|2}}

| eccentricity = 0.294{{±|0.024}}

| inclination = >70

}}

References

{{Reflist|refs=

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Category:Centaurus

Category:Planetary transit variables

Category:G-type main-sequence stars

Category:Planetary systems with two confirmed planets

J12422849-3038235

CD-29 98732