WASP-78#Planetary system

{{Starbox observe

| epoch = J2000

| constell = Eridanus

| ra = {{RA|04|15|01.5043}}

| dec = {{DEC|-22|06|59.103}}

| appmag_v = 12.0{{citation|arxiv=1206.1177|title=WASP-78b and WASP-79b: Two highly-bloated hot Jupiter-mass exoplanets orbiting F-type stars in Eridanus|year=2012|doi=10.1051/0004-6361/201219731|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.|journal=Astronomy & Astrophysics|volume=547|pages=A61|bibcode=2012A&A...547A..61S|s2cid=119233646}}

}}

{{Starbox character

| type=main sequence

| class = F8

}}

{{Starbox astrometry

| radial_v = 1.26

| prop_mo_ra = {{val|−0.367|(11)}}

| prop_mo_dec = {{val|6.395|(13)}}

| pm_footnote =

| parallax = 1.3851

| p_error = 0.0136

| parallax_footnote =

}}

{{Starbox detail

| source =

| mass = 1.33{{±|0.09}}

| radius = 2.20{{±|0.12}}

| gravity = 3.88{{±|0.04}}

| luminosity = {{val|5.2|0.1}}

| temperature = 6,100{{±|150}}

| metal_fe = −0.35{{±|0.14}}

| rotation = 0.4{{±|0.4}}

| rotational_velocity =6.63{{±|0.16}}

| age_gyr = 3.4{{±|1.5|0.8}}

}}

{{Starbox catalog

| names = {{odlist|TYC=5889-271-1|GSC=05889-00271|2MASS=J04150149-2206591|Gaia DR3=5089851638095503616}}

}}

{{Starbox reference

| Simbad = WASP-78

}}

WASP-78, is a single F-type main-sequence star about 2350 light-years away. It is likely to be younger than the Sun at 3.4{{±|1.5|0.8}} billion years. WASP-78 is depleted in heavy elements, having a 45% concentration of iron compared to the Sun.

Planetary system

In 2012 a transiting hot Jupiter planet b was detected on a circular orbit. The planetary equilibrium temperature is 2350{{±|80}} K, while the nightside temperature measured in 2019 is 2200{{±|41}} K.{{citation|arxiv=1901.07040|year=2020|doi=10.3847/1538-3881/ab6cff|last1=Garhart|first1=Emily|last2=Deming|first2=Drake|last3=Mandell|first3=Avi|last4=Knutson|first4=Heather A.|last5=Wallack|first5=Nicole|last6=Burrows|first6=Adam|last7=Fortney|first7=Jonathan J.|last8=Hood|first8=Callie|last9=Seay|first9=Christopher|last10=Sing|first10=David K.|last11=Benneke|first11=Björn|last12=Fraine|first12=Jonathan D.|last13=Kataria|first13=Tiffany|last14=Lewis|first14=Nikole|last15=Madhusudhan|first15=Nikku|last16=McCullough|first16=Peter|last17=Stevenson|first17=Kevin B.|last18=Wakeford|first18=Hannah|title=Statistical Characterization of Hot Jupiter Atmospheres Using Spitzer's Secondary Eclipses|journal=The Astronomical Journal|volume=159|issue=4|page=137|bibcode=2020AJ....159..137G|s2cid=119209434 |doi-access=free }} The dayside planetary temperature measured in 2020 is {{val|fmt=commas|2560|130|ul=K}}.{{citation|arxiv=2003.06407|title=Systematic phase curve study of known transiting systems from year one of the TESS mission|year=2020|doi=10.3847/1538-3881/ababad|last1=Wong|first1=Ian|last2=Shporer|first2=Avi|last3=Daylan|first3=Tansu|last4=Benneke|first4=Björn|last5=Fetherolf|first5=Tara|last6=Kane|first6=Stephen R.|last7=Ricker|first7=George R.|last8=Vanderspek|first8=Roland|last9=Latham|first9=David W.|last10=Winn|first10=Joshua N.|last11=Jenkins|first11=Jon M.|last12=Boyd|first12=Patricia T.|last13=Glidden|first13=Ana|last14=Goeke|first14=Robert F.|last15=Sha|first15=Lizhou|last16=Ting|first16=Eric B.|last17=Yahalomi|first17=Daniel|journal=The Astronomical Journal|volume=160|issue=4|page=155|bibcode=2020AJ....160..155W|s2cid=212717799 |doi-access=free }}

A survey in 2016 measured a Rossiter-McLaughlin effect and found the planetary orbit is well aligned with the equatorial plane of the star, misalignment equal to −6.4{{±|5.9}}°{{citation|arxiv=1610.00600|title=Rossiter–McLaughlin 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 |s2cid=53497449}} The planet cannot have formed in its current orbit and has likely undergone in the past a migration from the initial highly eccentric orbit.{{citation|arxiv=1403.1870|last1=Valsecchi|first1=Francesca|title=Planets on the Edge|journal=The Astrophysical Journal|year=2014|volume=787|issue=1|pages=L9|doi=10.1088/2041-8205/787/1/L9|bibcode=2014ApJ...787L...9V|s2cid=118451863}}

{{OrbitboxPlanet begin

| table_ref =

}}

{{OrbitboxPlanet

| exoplanet = b

| mass = 0.89{{±|0.08}}

| radius = 1.70{{±|0.11}}

| semimajor = 0.0362{{±|0.0008}}

| period = 2.17517632{{±|0.0000047}}

| eccentricity = 0

| inclination = 83.2{{±|2.3|1.6}}

}}