WASP-34 (original) (raw)

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Star in the constellation Crater

WASP-34

Observation dataEpoch J2000.0 Equinox J2000.0
Constellation Crater
Right ascension 11h 01m 35.8978s[1]
Declination –23° 51′ 38.387″[1]
Apparent magnitude (V) +10.28[2]
Characteristics
Spectral type G5[3]
Astrometry
Radial velocity (Rv) 49.84±0.21[1] km/s
Proper motion (μ) RA: -43.846 mas/yr[1] Dec.: -65.637 mas/yr[1]
Parallax (π) 7.6211±0.0164 mas[1]
Distance 428.0 ± 0.9 ly (131.2 ± 0.3 pc)
Details[3]
Mass 1.01±0.07 M☉
Radius 0.93±0.12 R☉
Luminosity 1.19±0.03[4] L☉
Surface gravity (log g) 4.5±0.1 cgs
Temperature 5,700±100 K
Metallicity [Fe/H] −0.02±0.10 dex
Rotation 34±15 d
Rotational velocity (v sin i) 1.4±0.6 km/s
Age 6.8±1.3[4] Gyr
Other designations
Amansinaya, CD−23 9677, CPD−23 5039, SAO 179442, TOI-744, TIC 437242640, WASP-34, TYC 6636-540-1, GSC 06636-00540, 2MASS J11013589-2351382, DENIS J110135.9-235138[5]
Database references
SIMBAD data
Exoplanet Archive data

WASP-34, also named Amansinaya,[6] is a sunlike star of spectral type G5V that has 1.01 times the mass and 0.93 times the diameter of the Sun. It rotates on its axis every 34±15 days, indicating it is around 6.7 billion years old. It hosts at least one exoplanet.[3]

In 2019 the IAU announced as part of NameExoWorlds that WASP-34 and its planet WASP-34b would be given official names chosen by school children from the Philippines.[7][8] The star is named Amansinaya, after Aman Sinaya, which is one of the two trinity deities of the Philippine's Tagalog mythology, and is the primordial deity of the ocean and protector of fisherman. The planet WASP-34b is named Haik. Haik is the successor of the primordial Aman Sinaya as the god of the sea of the Philippines' Tagalog mythology.[6]

WASP-34 has a transiting planet discovered in 2011 by the Wide Angle Search for Planets. This is a hot Jupiter, with just over half the mass of Jupiter and taking just 4.3 days to complete an orbit.[3] The planetary color was found to be redder than other hot Jupiters, hinting at peculiar chemistry.[9] The planet has a large measured temperature difference between the dayside (1185±47 K) and nightside (726±119 K).[10]

There is a long-period radial velocity trend, showing evidence for a massive object orbiting further out.[3] A 2014 study suggests an object at least 15 times the mass of Jupiter at a distance of 5 AU.[11]

The WASP-34 planetary system[12][11]

Companion(in order from star) Mass Semimajor axis(AU) Orbital period(days) Eccentricity Inclination Radius
b / Haik 0.583+0.030−0.031 MJ 0.0521±0.0012 4.3176782(45) <0.025 85.2±0.2° 1.22+0.11−0.08 RJ
c (unconfirmed) ≥14.96+6.29−3.39 _M_J 5.05+0.65−0.46 4093+750−520 ~0 — —
  1. ^ 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.
  2. ^ Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27. Bibcode:2000A&A...355L..27H.
  3. ^ a b c d e Smalley, B.; Anderson, D. R.; Collier Cameron, A.; Hellier, C.; Lendl, M.; Maxted, P. F. L.; Queloz, D.; Triaud, A. H. M. J.; West, R. G.; Bentley, S. J.; Enoch, B.; Gillon, M.; Lister, T. A.; Pepe, F.; Pollacco, D.; Segransan, D.; Smith, A. M. S.; Southworth, J.; Udry, S.; Wheatley, P. J.; Wood, P. L.; Bento, J. (2011). "WASP-34b: a near-grazing transiting sub-Jupiter-mass exoplanet in a hierarchical triple system". Astronomy and Astrophysics. 526: 5. arXiv:1012.2278. Bibcode:2011A&A...526A.130S. doi:10.1051/0004-6361/201015992. S2CID 43519917. A130.
  4. ^ a b Bonfanti, A.; Ortolani, S.; Nascimbeni, V. (2016). "Age consistency between exoplanet hosts and field stars". Astronomy and Astrophysics. 585: A5. arXiv:1511.01744. Bibcode:2016A&A...585A...5B. doi:10.1051/0004-6361/201527297. S2CID 53971692.
  5. ^ "CD-23 9677". SIMBAD. Centre de données astronomiques de Strasbourg.
  6. ^ a b "Approved names". NameExoworlds. Retrieved 2020-01-02.
  7. ^ "NameExoWorlds". 2019. Retrieved 6 September 2019.
  8. ^ "Naming". 2019. Retrieved 6 September 2019.
  9. ^ Challener, Ryan C.; Harrington, Joseph; Cubillos, Patricio E.; Blecic, Jasmina; Smalley, Barry (2021), "Spitzer Dayside Emission of WASP-34b", The Planetary Science Journal, 3 (4): 86, arXiv:2108.04101, Bibcode:2022PSJ.....3...86C, doi:10.3847/PSJ/ac1e9e
  10. ^ May, E. M.; Stevenson, K. B.; Bean, Jacob L.; Bell, Taylor J.; Cowan, Nicolas B.; Dang, Lisa; Desert, Jean-Michel; Fortney, Jonathan J.; Keating, Dylan; Kempton, Eliza M.-R.; Komacek, Thaddeus D.; Lewis, Nikole K.; Mansfield, Megan; Morley, Caroline; Parmentier, Vivien; Rauscher, Emily; Swain, Mark R.; Zellem, Robert T.; Showman, Adam (2022), "A New Analysis of Eight Spitzer Phase Curves and Hot Jupiter Population Trends: Qatar-1b, Qatar-2b, WASP-52b, WASP-34b, and WASP-140b", The Astronomical Journal, 163 (6): 256, arXiv:2203.15059, Bibcode:2022AJ....163..256M, doi:10.3847/1538-3881/ac6261, S2CID 247778438
  11. ^ a b Knutson, Heather A.; Fulton, Benjamin J.; et al. (April 2014). "Friends of Hot Jupiters. I. A Radial Velocity Search for Massive, Long-period Companions to Close-in Gas Giant Planets". The Astrophysical Journal. 785 (2): 126. arXiv:1312.2954. Bibcode:2014ApJ...785..126K. doi:10.1088/0004-637X/785/2/126.
  12. ^ 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. S2CID 118923163.