WASP-34
| Observation data Epoch J2000.0 Equinox ICRS | |
|---|---|
| Constellation | Crater |
| Right ascension | 11h 01m 35.8978s |
| Declination | −23° 51′ 38.387″ |
| Apparent magnitude (V) | +10.28 |
| Characteristics | |
| Evolutionary stage | main sequence |
| Spectral type | G5 |
| Astrometry | |
| Radial velocity (Rv) | 49.84±0.21 km/s |
| Proper motion (μ) | RA: −43.846 mas/yr Dec.: −65.637 mas/yr |
| Parallax (π) | 7.6211±0.0164 mas |
| Distance | 428.0 ± 0.9 ly (131.2 ± 0.3 pc) |
| Details | |
| Mass | 1.01±0.07 M☉ |
| Radius | 0.93±0.12 R☉ |
| Luminosity | 1.19±0.03 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 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 | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
WASP-34, also named Amansinaya, is a Sun-like star about 428 light-years (131 parsecs) away in the constellation Crater. With spectral type G5V, it 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 two exoplanets.
Naming
The designation WASP-34 comes from the Wide Angle Search for Planets. 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. 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.
Planetary system
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. It has a near-grazing transit, passing in front of the limb of the star. The planetary color was found to be redder than other hot Jupiters, hinting at peculiar chemistry. The planet has a large measured temperature difference between the dayside (1185±47 K) and nightside (726±119 K).
There is a long-period radial velocity trend, showing evidence for a massive object orbiting further out. A 2014 study suggested an object at least 15 times the mass of Jupiter at a distance of 5 AU. A 2026 study confirmed a second planet; it is smaller and closer to the star than previously thought, with a minimum mass of about 5 Jupiter masses and orbiting at a distance of 3 AU. There may also be a third planet; if so, the two outer planets would be near a 3:2 mean-motion resonance.
| 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 | ≥5.29+0.21 −0.28 MJ |
3.158+0.049 −0.082 |
2033.4+3.6 −6.5 |
0.214+0.009 −0.014 |
— | — |
| d (unconfirmed) | ≥1.24+0.52 −0.55 MJ |
— | 3083+293 −238 |
0.243+0.050 −0.243 |
— | — |
References
- ↑ Roman, Nancy G. (1987). "Identification of a constellation from a position". Publications of the Astronomical Society of the Pacific. 99 (617): 695. Bibcode:1987PASP...99..695R. doi:10.1086/132034. Constellation record for this object at VizieR.
- 1 2 3 4 5 6 7 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.
- ↑ 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.
- 1 2 3 4 5 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.
- 1 2 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.
- ↑ "CD-23 9677". SIMBAD. Centre de données astronomiques de Strasbourg.
- 1 2 "Approved names". NameExoworlds. Retrieved 2020-01-02.
- 1 2 3 Parc, Léna; Faria, João P.; et al. (October 2026). "Companions of Hot Jupiters: two decades of radial velocity monitoring with CORALIE". Astronomy & Astrophysics. arXiv:2610.25152.
- ↑ "NameExoWorlds". 2019. Retrieved 6 September 2019.
- ↑ "Naming". 2019. Retrieved 6 September 2019.
- ↑ 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
- ↑ 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
- ↑ 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.
- ↑ 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.
