HATS-3
Observation data
Epoch J2000      Equinox J2000
Constellation Capricornus[1]
Right ascension 20h 49m 49.78530s[2]
Declination −24° 25′ 43.5378″[2]
Apparent magnitude (V) 12.43[3]
Characteristics
Evolutionary stage main-sequence star
Spectral type F[4]
Astrometry
Radial velocity (Rv)−22.07±0.83[2] km/s
Proper motion (μ) RA: 10.393 mas/yr[2]
Dec.: 15.478 mas/yr[2]
Parallax (π)2.3595 ± 0.0171 mas[2]
Distance1,380 ± 10 ly
(424 ± 3 pc)
Details[5]
Mass1.210±0.040 M☉
Radius1.400±0.030 R☉
Surface gravity (log g)4.22±0.01[4] cgs
Temperature6351±76 K
Metallicity [Fe/H]−0.157±0.070 dex
Rotational velocity (v sin i)9.1±1.3 km/s
Age3.20+0.60
−0.40 Gyr
Other designations
HATS-3, TOI-103, TIC 336732616, TYC 6926-454-1, GSC 06926-00454, 2MASS J20494978-2425436[3]
Database references
SIMBADdata

HATS-3 is an F-type main-sequence star 1,380 light-years (420 parsecs) away. Its surface temperature is 6351±76 K. HATS-3 is relatively depleted in its concentration of heavy elements, with a metallicity Fe/H index of −0.157±0.07, but is slightly younger than the Sun at an age of 3.2+0.6
−0.4 billion years.[4]

A multiplicity survey in 2016 detected a candidate stellar companion to HATS-3, 3.671±0.016 arc-seconds away.[6]

Planetary system

In 2013, one planet, named HATS-3b, was discovered on a tight, nearly circular orbit.[4] The planetary orbit of HATS-3b is likely aligned with the equatorial plane of the star, at a misalignment angle of 3±25°.[7] The planetary equilibrium temperature is 1643 K.[4]

The HATS-3 planetary system[5]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b 1.10+0.18
−0.19 MJ 		0.04852+0.00053
−0.00054 		3.5478510(50) <0.30 86.20±0.30° 1.381±0.035 RJ

References

  1. ^ "Finding the constellation which contains given sky coordinates". djm.cc. 2 August 2008.
  2. ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  3. ^ a b "HATS-3". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-02-09.
  4. ^ a b c d e Bayliss, D.; Zhou, G.; Penev, K.; Bakos, G. Á.; Hartman, J. D.; Jordán, A.; Mancini, L.; Mohler-Fischer, M.; Suc, V.; Rabus, M.; Béky, B.; Csubry, Z.; Buchhave, L.; Henning, T.; Nikolov, N.; Csák, B.; Brahm, R.; Espinoza, N.; Noyes, R. W.; Schmidt, B.; Conroy, P.; Wright, D. J.; Tinney, C. G.; Addison, B. C.; Sackett, P. D.; Sasselov, D. D.; Lázár, J.; Papp, I.; Sári, P. (2013), "HATS-3b: AN INFLATED HOT JUPITER TRANSITING AN F-TYPE STAR", The Astronomical Journal, 146 (5): 113, arXiv:1306.0624, Bibcode:2013AJ....146..113B, doi:10.1088/0004-6256/146/5/113, S2CID 119194040
  5. ^ a b Bonomo, A. S.; Desidera, S.; et al. (June 2017). "The GAPS Programme with HARPS-N at TNG. XIV. Investigating giant planet migration history via improved eccentricity and mass determination for 231 transiting planets". Astronomy & Astrophysics. 602: A107. arXiv:1704.00373. Bibcode:2017A&A...602A.107B. doi:10.1051/0004-6361/201629882.
  6. ^ Evans, D. F.; Southworth, J.; Maxted, P. F. L.; Skottfelt, J.; Hundertmark, M.; Jørgensen, U. G.; Dominik, M.; Alsubai, K. A.; Andersen, M. I.; Bozza, V.; Bramich, D. M.; Burgdorf, M. J.; Ciceri, S.; d'Ago, G.; Figuera Jaimes, R.; Gu, S.-H.; Haugbølle, T.; Hinse, T. C.; Juncher, D.; Kains, N.; Kerins, E.; Korhonen, H.; Kuffmeier, M.; Mancini, L.; Peixinho, N.; Popovas, A.; Rabus, M.; Rahvar, S.; Schmidt, R. W.; et al. (2016), "High-resolution Imaging of Transiting Extrasolar Planetary systems (HITEP)", Astronomy & Astrophysics, 589: A58, arXiv:1603.03274, doi:10.1051/0004-6361/201527970, S2CID 14215845
  7. ^ Addison, B. C.; Tinney, C. G.; Wright, D. J.; Bayliss, D. (2014), "A SPIN-ORBIT ALIGNMENT FOR THE HOT JUPITER HATS-3b", The Astrophysical Journal, 792 (2): 112, arXiv:1407.7710, Bibcode:2014ApJ...792..112A, doi:10.1088/0004-637X/792/2/112, S2CID 118352072


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