Astronomy:WASP-26
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Cetus |
| Right ascension | 00h 18m 24.7008s[1] |
| Declination | −15° 16′ 02.2775″[1] |
| Apparent magnitude (V) | 11.30[2] |
| Characteristics | |
| Evolutionary stage | main sequence star |
| Spectral type | G0V |
| B−V color index | 0.32 |
| J−H color index | 0.246 |
| J−K color index | 0.411 |
| Astrometry | |
| Radial velocity (Rv) | 9.60±0.54[1] km/s |
| Proper motion (μ) | RA: 27.416±0.022[1] mas/yr Dec.: -24.454±0.021[1] mas/yr |
| Parallax (π) | 3.9574 ± 0.0247[1] mas |
| Distance | 824 ± 5 ly (253 ± 2 pc) |
| Details[3][4][5][6] | |
| Mass | 1.09±0.01 M☉ |
| Radius | 1.284±0.035 R☉ |
| Luminosity | 1.26 L☉ |
| Surface gravity (log g) | 4.40±0.01 cgs |
| Temperature | 6015±55 K |
| Metallicity [Fe/H] | -0.02±0.09 dex |
| Rotational velocity (v sin i) | 3.9±0.4 km/s |
| Age | 6±2 Gyr |
| Other designations | |
WASP-26, TYC 5839-876-1, DENIS J001824.6-151601, 2MASS J00182469-1516022, Gaia DR2 2416782701664155008[7] | |
| Database references | |
| SIMBAD | data |
WASP-26 is a yellow main sequence star in the constellation of Cetus.
Star characteristics
WASP-26 is an old star close to leaving the main sequence and is part of a wide binary. The binary's projected separation is 3800 astronomical units, its companion star being a red dwarf with an effective temperature of 4600K and a visual magnitude of 13.6.[3] WASP-26 produces a large amount of ultraviolet light due to frequent flares, with an average ultraviolet flux close to the F7 class main-sequence star WASP-1.[8]
Planetary system
The "Hot Jupiter" class planet WASP-26b was discovered around WASP-26 in 2010.[3] The planet would have an equilibrium temperature of 1660±40 K, but measured temperatures are slightly higher at 1775K and no noticeable difference exists between the day-side and the night-side of the planet.[9] A 2011 study using the Rossiter-McLaughlin effect failed to determine the inclination of the planetary orbit to the equatorial plane of the parent star due to high stellar noise,[5] but an initial constraint of -34+36−26° was published in 2012.[10]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 1.02±0.03 MJ | 0.0400±0.0003 | 2.75660±0.00001 | 0 | 82.5±0.5° | 1.216±0.047 RJ |
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ Høg, E. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics 355: L27–L30. Bibcode: 2000A&A...355L..27H.
- ↑ 3.0 3.1 3.2 3.3 Smalley, B.; Anderson, D. R.; Collier Cameron, A.; Gillon, M.; Hellier, C.; Lister, T. A.; Maxted, P. F. L.; Queloz, D. et al. (2010). "WASP-26b: A 1-Jupiter-mass planet around an early-G-type star". Astronomy and Astrophysics 520: A56. doi:10.1051/0004-6361/201014705. Bibcode: 2010A&A...520A..56S.
- ↑ A. Bonfanti, S. Ortolani, and V. Nascimbeni, "Age consistency between exoplanet hosts and field stars", 2016
- ↑ 5.0 5.1 Anderson, D. R.; Collier Cameron, A.; Gillon, M.; Hellier, C.; Jehin, E.; Lendl, M.; Queloz, D.; Smalley, B. et al. (2011). "Spin-orbit measurements and refined parameters for the exoplanet systems WASP-22 and WASP-26". Astronomy & Astrophysics 534: A16. doi:10.1051/0004-6361/201117597. Bibcode: 2011A&A...534A..16A.
- ↑ 6.0 6.1 Southworth, John; Hinse, T. C.; Burgdorf, M.; Calchi Novati, S.; Dominik, M.; Galianni, P.; Gerner, T.; Giannini, E. et al. (2014). "High-precision photometry by telescope defocussing – VI. WASP-24, WASP-25 and WASP-26★". Monthly Notices of the Royal Astronomical Society 444 (1): 776–789. doi:10.1093/mnras/stu1492. Bibcode: 2014MNRAS.444..776S.
- ↑ "WASP-26". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=WASP-26.
- ↑ Evgenya L. Shkolnik, "AN ULTRAVIOLET INVESTIGATION OF ACTIVITY ON EXOPLANET HOST STARS", 2013
- ↑ Mahtani, D. P.; Maxted, P. F. L.; Anderson, D. R.; Smith, A. M. S.; Smalley, B.; Tregloan-Reed, J.; Southworth, J.; Madhusudhan, N. et al. (2013). "Warm Spitzer occultation photometry of WASP-26b at 3.6 and 4.5 μm". Monthly Notices of the Royal Astronomical Society 432 (1): 693–701. doi:10.1093/mnras/stt505. Bibcode: 2013MNRAS.432..693M.
- ↑ Albrecht, Simon; Winn, Joshua N.; Johnson, John A.; Howard, Andrew W.; Marcy, Geoffrey W.; Butler, R. Paul; Arriagada, Pamela; Crane, Jeffrey D. et al. (2012), "Obliquities of Hot Jupiter host stars: Evidence for tidal interactions and primordial misalignments", The Astrophysical Journal 757 (1): 18, doi:10.1088/0004-637X/757/1/18, Bibcode: 2012ApJ...757...18A
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