WASP-103#Planetary system

{{Starbox observe

| epoch = J2000

| constell = Hercules

| ra = {{RA|16|37|15.5766}}

| dec = {{DEC|07|11|00.110}}

| appmag_v = 12.1

}}

{{Starbox character

| type = main-sequence star

| class = F8V

| b-v =

}}

{{Starbox astrometry

| radial_v = {{val|-40.69|1.00}}

| prop_mo_ra = −9.756{{cite Gaia DR3|4439085988769170432}}

| prop_mo_dec = 2.779

| parallax = 1.8332

| p_error = 0.1073

| parallax_footnote =

}}

{{Starbox detail

| source =

| mass = 1.220{{±|0.039|0.036}}

| radius = 1.436{{±|0.052|0.031}}

| luminosity = 3.3

| gravity = 4.35{{±|0.02}}

| temperature = 6110{{±|160}}

| metal_fe = 0.06{{±|0.13}}

| rotation =

| rotational_velocity = 10.60{{±|0.90}}

| age_gyr = 4{{±|1}}

}}

{{Starbox catalog

| names = {{odlist|2MASS = J16371556+0711000|Gaia DR2=4439085988769170432}}{{cite simbad|title=WASP-103|access-date=2021-05-05}}

}}

{{Starbox reference

| Simbad = WASP+103

}}

WASP-103 is an F-type main-sequence star located 1,800 ± 100 light-years (550 ± 30 parsecs) away in the constellation Hercules. Its surface temperature is {{val|6110|160|ul=kelvins|fmt=commas}} (K). The star's concentration of heavy elements is similar to that of the Sun. WASP-103 is slightly younger than the Sun at 4{{±|1}} billion years. The chromospheric activity of the star is elevated due to interaction with the giant planet on a close-in orbit.{{cite journal |arxiv=1612.01739 |doi=10.1093/mnras/stw3172 |bibcode=2017MNRAS.466..738S |title=SALT observations of the chromospheric activity of transiting planet hosts: Mass-loss and star–planet interactions |year=2017 |last1=Staab |first1=D. |last2=Haswell |first2=C. A. |last3=Smith |first3=Gareth D. |last4=Fossati |first4=L. |last5=Barnes |first5=J. R. |last6=Busuttil |first6=R. |last7=Jenkins |first7=J. S. |journal=Monthly Notices of the Royal Astronomical Society |volume=466 |issue=1 |pages=738–748 |doi-access=free }}

A multiplicity survey in 2015 found a suspected stellar companion to WASP-103, at a projected separation of {{val|0.242|0.016|ul=″}}.{{cite journal |arxiv=1506.05456 |doi=10.1051/0004-6361/201526525 |title=A Lucky Imaging search for stellar sources near 74 transit hosts |year=2015 |last1=Wöllert |first1=Maria |last2=Brandner |first2=Wolfgang |journal=Astronomy & Astrophysics |volume=579 |pages=A129 |bibcode=2015A&A...579A.129W |s2cid=118903879 }}

Planetary system

File:Artist impression of planet WASP-103b and its host star.png

In 2014 one super-Jupiter planet, named WASP-103b, was discovered by the transit method.{{cite journal |arxiv=1411.2767 |doi=10.1093/mnras/stu2394 |bibcode=2015MNRAS.447..711S |title=High-precision photometry by telescope defocusing – VII. The ultrashort period planet WASP-103★ |year=2015 |last1=Southworth |first1=John |last2=Mancini |first2=L. |last3=Ciceri |first3=S. |last4=Budaj |first4=J. |last5=Dominik |first5=M. |last6=Figuera Jaimes |first6=R. |last7=Haugbølle |first7=T. |last8=Jørgensen |first8=U. G. |last9=Popovas |first9=A. |last10=Rabus |first10=M. |last11=Rahvar |first11=S. |last12=von Essen |first12=C. |last13=Schmidt |first13=R. W. |last14=Wertz |first14=O. |last15=Alsubai |first15=K. A. |last16=Bozza |first16=V. |last17=Bramich |first17=D. M. |last18=Calchi Novati |first18=S. |last19=d'Ago |first19=G. |last20=Hinse |first20=T. C. |last21=Henning |first21=Th. |last22=Hundertmark |first22=M. |last23=Juncher |first23=D. |last24=Korhonen |first24=H. |last25=Skottfelt |first25=J. |last26=Snodgrass |first26=C. |last27=Starkey |first27=D. |last28=Surdej |first28=J. |journal=Monthly Notices of the Royal Astronomical Society |volume=447 |issue=1 |pages=711–721 |doi-access=free }} The planet is orbiting its host star in 22 hours and may be close to the limit of tidal disruption.{{cite journal |arxiv=1401.2784 |doi=10.1051/0004-6361/201323014 |title=WASP-103 b: A new planet at the edge of tidal disruption |year=2014 |last1=Gillon |first1=M. |last2=Anderson |first2=D. R. |last3=Collier-Cameron |first3=A. |last4=Delrez |first4=L. |last5=Hellier |first5=C. |last6=Jehin |first6=E. |last7=Lendl |first7=M. |last8=Maxted |first8=P. F. L. |last9=Pepe |first9=F. |last10=Pollacco |first10=D. |last11=Queloz |first11=D. |last12=Ségransan |first12=D. |last13=Smith |first13=A. M. S. |last14=Smalley |first14=B. |last15=Southworth |first15=J. |last16=Triaud |first16=A. H. M. J. |last17=Udry |first17=S. |last18=Van Grootel |first18=V. |last19=West |first19=R. G. |journal=Astronomy & Astrophysics |volume=562 |pages=L3 |bibcode=2014A&A...562L...3G |s2cid=53680974 }} Orbital decay was not detected by 2020.{{cite journal |arxiv=2002.02606 |doi=10.3847/1538-3881/ab7374 |title=The Continuing Search for Evidence of Tidal Orbital Decay of Hot Jupiters |year=2020 |last1=Patra |first1=Kishore C. |last2=Winn |first2=Joshua N. |last3=Holman |first3=Matthew J. |last4=Gillon |first4=Michael |last5=Burdanov |first5=Artem |last6=Jehin |first6=Emmanuel |last7=Delrez |first7=Laetitia |last8=Pozuelos |first8=Francisco J. |last9=Barkaoui |first9=Khalid |last10=Benkhaldoun |first10=Zouhair |last11=Narita |first11=Norio |last12=Fukui |first12=Akihiko |last13=Kusakabe |first13=Nobuhiko |last14=Kawauchi |first14=Kiyoe |last15=Terada |first15=Yuka |last16=Bouma |first16=L. G. |last17=Weinberg |first17=Nevin N. |last18=Broome |first18=Madelyn |journal=The Astronomical Journal |volume=159 |issue=4 |page=150 |bibcode=2020AJ....159..150P |s2cid=211066260 |doi-access=free }} In early 2022, the planet was popularized because of its shape similar to a potato.{{Cite web|title=Astronomers Discover Planet That Looks Like a Rugby Ball|url=https://gadgets360.com/science/news/planet-potato-rugby-ball-wasp-103b-astronomer-host-sun-proximity-esa-nasa-hubble-2709321|access-date=2022-02-19|website=NDTV Gadgets 360|date=15 January 2022 |language=en}}

The planetary atmosphere contains water, and possibly hydrogen cyanide, titanium(II) oxide, or sodium.{{cite journal |arxiv=2007.13510 |doi=10.1093/mnras/staa2307 |bibcode=2020MNRAS.497.5155W |title=Ground-based transmission spectroscopy with FORS2: A featureless optical transmission spectrum and detection of H2O for the ultra-hot Jupiter WASP-103b |year=2020 |last1=Wilson |first1=Jamie |last2=Gibson |first2=Neale P. |last3=Nikolov |first3=Nikolay |last4=Constantinou |first4=Savvas |last5=Madhusudhan |first5=Nikku |last6=Goyal |first6=Jayesh |last7=Barstow |first7=Joanna K. |last8=Carter |first8=Aarynn L. |last9=De Mooij |first9=Ernst J W. |last10=Drummond |first10=Benjamin |last11=Mikal-Evans |first11=Thomas |last12=Helling |first12=Christiane |last13=Mayne |first13=Nathan J. |last14=Sing |first14=David K. |journal=Monthly Notices of the Royal Astronomical Society |volume=497 |issue=4 |pages=5155–5170 |doi-access=free }} The planet has an elevated carbon to oxygen molar fraction of 0.9 or 1.35{{±|0.14|0.17}}, therefore it is nearly certain to be a carbon planet.{{citation|arxiv=2303.13732|year=2023|title=Thermal emission from the hot Jupiter WASP-103 b in J and K s bands|doi=10.1093/mnras/stad891 |last1=Shi |first1=Yaqing |last2=Wang |first2=Wei |last3=Zhao |first3=Gang |last4=Zhai |first4=Meng |last5=Chen |first5=Guo |last6=Jiang |first6=Zewen |last7=Ouyang |first7=Qinglin |last8=Henning |first8=Thomas |last9=Zhao |first9=Jingkun |last10=Crouzet |first10=Nicolas |last11=Van Boekel |first11=Roy |last12=Esteves |first12=Lisa |journal=Monthly Notices of the Royal Astronomical Society |volume=522 |pages=1491–1503 |doi-access=free }}

Though the planetary equilibrium temperature is {{val|2484|67|ul=K|fmt=commas}}, the planet is tidally locked to WASP-103 and has one side in permanent day and the other side in permanent night. A significant temperature difference exists between the night side and day side; the dayside temperature is {{val|2930|40|u=K|fmt=commas}}, while the night side temperature is {{val|1880|40|u=K|fmt=commas}}.{{cite journal |arxiv=1805.00029 |doi=10.3847/1538-3881/aac3df |title=Global Climate and Atmospheric Composition of the Ultra-hot Jupiter WASP-103b fromHSTandSpitzer Phase Curve Observations |year=2018 |last1=Kreidberg |first1=Laura |last2=Line |first2=Michael R. |last3=Parmentier |first3=Vivien |last4=Stevenson |first4=Kevin B. |last5=Louden |first5=Tom |last6=Bonnefoy |first6=Mickäel |last7=Faherty |first7=Jacqueline K. |last8=Henry |first8=Gregory W. |last9=Williamson |first9=Michael H. |last10=Stassun |first10=Keivan |last11=Beatty |first11=Thomas G. |last12=Bean |first12=Jacob L. |last13=Fortney |first13=Jonathan J. |last14=Showman |first14=Adam P. |last15=Désert |first15=Jean-Michel |last16=Arcangeli |first16=Jacob |journal=The Astronomical Journal |volume=156 |issue=1 |page=17 |bibcode=2018AJ....156...17K |s2cid=56157823 |doi-access=free }}

{{OrbitboxPlanet begin

| name = WASP-103

| table_ref ={{cite journal |arxiv=1704.00373 |doi=10.1051/0004-6361/201629882 |bibcode=2017A&A...602A.107B |title=The GAPS Programme with HARPS-N at TNG |year=2017 |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=602 |pages=A107 |s2cid=118923163 |display-authors=1 }}

}}

{{OrbitboxPlanet

| exoplanet = b

| mass = 1.455{{±|0.090|0.091}}

| radius = 1.528{{±|0.073|0.047}}

| semimajor = 0.01987{{±|0.00020|0.00021}}

| period = 0.9255456{{±|0.0000013}}

| eccentricity = <0.15

| inclination =87.3{{±|1.2}}

}}