Astronomy:WASP-103

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Short description: Star in the constellation Hercules

Coordinates: Sky map 16h 37m 15.5754s, +07° 11′ 00.1190″

WASP-103
Observation data
Equinox J2000.0]] (ICRS)
Constellation Hercules
Right ascension  16h 37m 15.5766s[1]
Declination 07° 11′ 00.110″[1]
Apparent magnitude (V) 12.1[2]
Characteristics
Evolutionary stage main-sequence star[3]
Spectral type F8V[2]
Astrometry
Radial velocity (Rv)−40.69±1.00[1] km/s
Proper motion (μ) RA: −9.756[1] mas/yr
Dec.: 2.779[1] mas/yr
Parallax (π)1.8332 ± 0.1073[1] mas
Distance1,800 ± 100 ly
(550 ± 30 pc)
Details
Mass1.220+0.039−0.036[4] M☉
Radius1.436+0.052−0.031[4] R☉
Luminosity3.3[1] L☉
Surface gravity (log g)4.35±0.02[1] cgs
Temperature6110±160[5] K
Metallicity [Fe/H]0.06±0.13[4] dex
Rotational velocity (v sin i)10.60±0.90[4] km/s
Age4±1[4] Gyr
Other designations
Gaia DR2 4439085988769170432, 2MASS J16371556+0711000[6]
Database references
SIMBADdata

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 6,110±160 kelvins (K). The star's concentration of heavy elements is similar to that of the Sun.[4] WASP-103 is slightly younger than the Sun at 4±1 billion years.[4] The chromospheric activity of the star is elevated due to interaction with the giant planet on a close-in orbit.[5]

A multiplicity survey in 2015 found a suspected stellar companion to WASP-103, at a projected separation of 0.242″±0.016″.[7]

Planetary system

Artist's impression of WASP-103b and its host star

In 2014 one super-Jupiter planet, named WASP-103b, was discovered by the transit method.[8] The planet is orbiting its host star in 22 hours and may be close to the limit of tidal disruption.[2] Orbital decay was not detected by 2020.[9] In early 2022, the planet was popularized because of its shape similar to a potato.[10]

The planetary atmosphere contains water, and possibly hydrogen cyanide, titanium(II) oxide, or sodium.[11] The planet has an elevated carbon to oxygen molar fraction of 0.9[3] or 1.35+0.14−0.17, therefore it is nearly certain to be a carbon planet.[12]

The planetary equilibrium temperature is 2,484±67 K, although a big difference exists between the night side and day side. The dayside temperature is 2,930±40 K, while the night side temperature is 1,880±40 K.[3]

The WASP-103 planetary system[4]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b 1.455+0.090−0.091 MJ 0.01987+0.00020−0.00021 0.9255456±0.0000013 <0.15 87.3±1.2° 1.528+0.073−0.047 RJ

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  2. ↑ 2.0 2.1 2.2 Gillon, M.; Anderson, D. R.; Collier-Cameron, A.; Delrez, L.; Hellier, C.; Jehin, E.; Lendl, M.; Maxted, P. F. L. et al. (2014). "WASP-103 b: A new planet at the edge of tidal disruption". Astronomy & Astrophysics 562: L3. doi:10.1051/0004-6361/201323014. Bibcode: 2014A&A...562L...3G. 
  3. ↑ 3.0 3.1 3.2 Kreidberg, Laura; Line, Michael R.; Parmentier, Vivien; Stevenson, Kevin B.; Louden, Tom; Bonnefoy, Mickäel; Faherty, Jacqueline K.; Henry, Gregory W. et al. (2018). "Global Climate and Atmospheric Composition of the Ultra-hot Jupiter WASP-103b fromHSTandSpitzer Phase Curve Observations". The Astronomical Journal 156 (1): 17. doi:10.3847/1538-3881/aac3df. Bibcode: 2018AJ....156...17K. 
  4. ↑ 4.0 4.1 4.2 4.3 4.4 4.5 4.6 4.7 Bonomo, A. S. et al. (2017). "The GAPS Programme with HARPS-N at TNG". Astronomy & Astrophysics 602: A107. doi:10.1051/0004-6361/201629882. Bibcode: 2017A&A...602A.107B. 
  5. ↑ 5.0 5.1 Staab, D.; Haswell, C. A.; Smith, Gareth D.; Fossati, L.; Barnes, J. R.; Busuttil, R.; Jenkins, J. S. (2017). "SALT observations of the chromospheric activity of transiting planet hosts: Mass-loss and star–planet interactions". Monthly Notices of the Royal Astronomical Society 466 (1): 738–748. doi:10.1093/mnras/stw3172. Bibcode: 2017MNRAS.466..738S. 
  6. ↑ "WASP-103". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=WASP-103. 
  7. ↑ Wöllert, Maria; Brandner, Wolfgang (2015). "A Lucky Imaging search for stellar sources near 74 transit hosts". Astronomy & Astrophysics 579: A129. doi:10.1051/0004-6361/201526525. Bibcode: 2015A&A...579A.129W. 
  8. ↑ Southworth, John; Mancini, L.; Ciceri, S.; Budaj, J.; Dominik, M.; Figuera Jaimes, R.; Haugbølle, T.; Jørgensen, U. G. et al. (2015). "High-precision photometry by telescope defocusing – VII. The ultrashort period planet WASP-103★". Monthly Notices of the Royal Astronomical Society 447 (1): 711–721. doi:10.1093/mnras/stu2394. Bibcode: 2015MNRAS.447..711S. 
  9. ↑ Patra, Kishore C.; Winn, Joshua N.; Holman, Matthew J.; Gillon, Michael; Burdanov, Artem; Jehin, Emmanuel; Delrez, Laetitia; Pozuelos, Francisco J. et al. (2020). "The Continuing Search for Evidence of Tidal Orbital Decay of Hot Jupiters". The Astronomical Journal 159 (4): 150. doi:10.3847/1538-3881/ab7374. Bibcode: 2020AJ....159..150P. 
  10. ↑ "Astronomers Discover Planet That Looks Like a Rugby Ball" (in en). 15 January 2022. https://gadgets360.com/science/news/planet-potato-rugby-ball-wasp-103b-astronomer-host-sun-proximity-esa-nasa-hubble-2709321. 
  11. ↑ Wilson, Jamie; Gibson, Neale P.; Nikolov, Nikolay; Constantinou, Savvas; Madhusudhan, Nikku; Goyal, Jayesh; Barstow, Joanna K.; Carter, Aarynn L. et al. (2020). "Ground-based transmission spectroscopy with FORS2: A featureless optical transmission spectrum and detection of H2O for the ultra-hot Jupiter WASP-103b". Monthly Notices of the Royal Astronomical Society 497 (4): 5155–5170. doi:10.1093/mnras/staa2307. Bibcode: 2020MNRAS.497.5155W. 
  12. ↑ Shi, Yaqing; Wang, Wei; Zhao, Gang; Zhai, Meng; Chen, Guo; Jiang, Zewen; Ouyang, Qinglin; Henning, Thomas et al. (2023), "Thermal emission from the hot Jupiter WASP-103 b in J and K s bands", Monthly Notices of the Royal Astronomical Society 522: 1491–1503, doi:10.1093/mnras/stad891 

External links



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