WASP-26

Last updated
WASP-26
Observation data
Epoch J2000       Equinox
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  mas [1]
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.

Contents

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]

The WASP-26 planetary system [3] [6]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b 1.02±0.03  MJ 0.0400±0.00032.75660±0.00001082.5±0.5° 1.216±0.047  RJ

Related Research Articles

WASP-79b is an extrasolar planet orbiting the star CD-30 1812. This planet is in the constellation Eridanus, and is about 810 light-years from Earth.

WASP-32 is a yellow main-sequence star in the constellation of Pisces. The star was given the formal name Parumleo in January 2020, Latin for small lion and referencing the national animal of Singapore.

WASP-25 is a yellow main sequence star in the constellation of Hydra.

WASP-50 is a G-type main-sequence star about 610 light-years away. The star is older than the Sun and slightly depleted in heavy elements compared to the Sun, and has a close to average starspot activity. Despite its advanced age, the star is rotating rapidly, being spun up by the tides raised by giant planet on close orbit.

WASP-48 is a subgiant star about 1400 light-years away. The star is likely older than Sun and slightly depleted in heavy elements. It shows an infrared excess noise of unknown origin, yet has no detectable ultraviolet emissions associated with the starspot activity. The discrepancy may be due to large interstellar absorption of light in interstellar medium for WASP-48. The measurements are compounded by the emission from eclipsing contact binary NSVS-3071474 projected on sky plane nearby, although no true stellar companions were detected by survey in 2015.

WASP-46 is a G-type main-sequence star about 1240 light-years away. The star is older than Sun and is strongly depleted in heavy elements compared to Sun, having just 45% of solar abundance. Despite its advanced age, the star is rotating rapidly, being spun up by the tides raised by giant planet on close orbit.

WASP-45 is a K-type main-sequence star about 690 light-years away. The star age cannot be well constrained, but it is probably older than Sun. Yet, WASP-45 is enriched in heavy elements compared to Sun, having 240% of solar abundance.

WASP-78, is a single F-type main-sequence star about 2500 light-years away. It is likely to be younger than the Sun at 3.4+1.5
−0.8 billion years. WASP-78 is depleted in heavy elements, having a 45% concentration of iron compared to the Sun.

BD+00 316, also known as WASP-71 since 2019, is an F-class main sequence star about 1200 light-years away. The star is younger than the Sun at approximately 3.6 billion years, yet is already close to leaving the main sequence. BD+00 316 is enriched in heavy elements, having 140% of the solar abundance of iron.

WASP-64 is a star about 1200 light-years away. It is a G7 class main-sequence star, orbited by a planet WASP-64b. It is younger than the Sun at 3.6±1.6 billion years, and it has a metal abundance similar to the Sun. The star is rotating rapidly, being spun up by the giant planet in a close orbit.

WASP-62 is a single star about 575 light-years away. It is an F class main-sequence star, orbited by a planet, WASP-62b. The age of WASP-62 is much younger than the Sun at 0.8±0.6 billion years, and it has a metal abundance similar to the Sun. WASP-62 was named Naledi in 2019.

WASP-61 is a single F-type main-sequence star about 1560 light-years away. The star age is much likely younger than the Sun's at approximately 3.8+1.8
−0.9 billion years. WASP-61 is depleted in heavy elements, having just 40% of the solar abundance of iron.

WASP-59 is a K-type main-sequence star about 379 light-years away. The star's age is essentially unconstrained by observations. WASP-59 is slightly depleted in heavy elements, having 70% of the solar abundance of iron. The star produces extremely low levels of ultraviolet light, indicating an absence of flare activity.

WASP-42 is a K-type main-sequence star. Its surface temperature is 5315±79 K. WASP-42 is similar to the Sun in concentration of heavy elements, with metallicity ([Fe/H]) of 0.05±0.13, and is much older than the Sun at 11.3+1.5
−4.8 billion years. The star does exhibit starspot activity as is typical for its spectral class.

WASP-69 is a K-type main-sequence star. Its surface temperature is 4782±15 K. WASP-69 is slightly enriched in heavy elements compared to the Sun, with a metallicity Fe/H index of 0.10±0.01, and is much younger than the Sun at 2 billion years. The data regarding starspot activity of WASP-69 are inconclusive, but spot coverage of the photosphere may be very high.

BD+02 2056, also known as WASP-84 is a G-type main-sequence star. Its surface temperature is 5350±31 K, and is slightly enriched in heavy elements compared to the Sun, with a metallicity Fe/H index of 0.05±0.02. It is rich in carbon and depleted of oxygen. BD+02 2056's age is probably older than the Sun at 8.5+4.1
−5.5 billion years. The star appears to have an anomalously small radius, which can be explained by the unusually high helium fraction or by it being very young.

WASP-80 is a K-type main-sequence star about 162 light-years away. The star's age is much younger than the Sun's at 1.352±0.222 billion years. WASP-80 is similar to the Sun in concentration of heavy elements, although this measurement is highly uncertain.

References

  1. 1 2 3 4 5 6 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR.
  2. ↑ Høg, E.; et al. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27–L30. Bibcode:2000A&A...355L..27H.
  3. 1 2 3 4 Smalley, B.; Anderson, D. R.; Collier Cameron, A.; Gillon, M.; Hellier, C.; Lister, T. A.; Maxted, P. F. L.; Queloz, D.; Triaud, A. H. M. J.; West, R. G.; Bentley, S. J.; Enoch, B.; Pepe, F.; Pollacco, D. L.; Segransan, D.; Smith, A. M. S.; Southworth, J.; Udry, S.; Wheatley, P. J.; Wood, P. L.; Bento, J. (2010). "WASP-26b: A 1-Jupiter-mass planet around an early-G-type star". Astronomy and Astrophysics. 520: A56. arXiv: 1004.1542 . Bibcode:2010A&A...520A..56S. doi:10.1051/0004-6361/201014705. S2CID   55114421.
  4. ↑ A. Bonfanti, S. Ortolani, and V. Nascimbeni, "Age consistency between exoplanet hosts and field stars", 2016
  5. 1 2 Anderson, D. R.; Collier Cameron, A.; Gillon, M.; Hellier, C.; Jehin, E.; Lendl, M.; Queloz, D.; Smalley, B.; Triaud, A. H. M. J.; Vanhuysse, M. (2011). "Spin-orbit measurements and refined parameters for the exoplanet systems WASP-22 and WASP-26". Astronomy & Astrophysics. 534: A16. arXiv: 1106.6092 . Bibcode:2011A&A...534A..16A. doi:10.1051/0004-6361/201117597. S2CID   31204371.
  6. 1 2 Southworth, John; Hinse, T. C.; Burgdorf, M.; Calchi Novati, S.; Dominik, M.; Galianni, P.; Gerner, T.; Giannini, E.; Gu, S.-H.; Hundertmark, M.; Jørgensen, U. G.; Juncher, D.; Kerins, E.; Mancini, L.; Rabus, M.; Ricci, D.; Schäfer, S.; Skottfelt, J.; Tregloan-Reed, J.; Wang, X.-B.; Wertz, O.; Alsubai, K. A.; Andersen, J. M.; Bozza, V.; Bramich, D. M.; Browne, P.; Ciceri, S.; d'Ago, G.; Damerdji, Y.; 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. arXiv: 1407.6253 . Bibcode:2014MNRAS.444..776S. doi:10.1093/mnras/stu1492. S2CID   53641330.
  7. ↑ "WASP-26". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2022-02-19.
  8. ↑ Evgenya L. Shkolnik, "AN ULTRAVIOLET INVESTIGATION OF ACTIVITY ON EXOPLANET HOST STARS", 2013
  9. ↑ Mahtani, D. P.; Maxted, P. F. L.; Anderson, D. R.; Smith, A. M. S.; Smalley, B.; Tregloan-Reed, J.; Southworth, J.; Madhusudhan, N.; Collier Cameron, A.; Gillon, M.; Harrington, J.; Hellier, C.; Pollacco, D.; Queloz, D.; Triaud, A. H. M. J.; West, R. G. (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. arXiv: 1303.4596 . Bibcode:2013MNRAS.432..693M. doi:10.1093/mnras/stt505. S2CID   55842630.
  10. ↑ Albrecht, Simon; Winn, Joshua N.; Johnson, John A.; Howard, Andrew W.; Marcy, Geoffrey W.; Butler, R. Paul; Arriagada, Pamela; Crane, Jeffrey D.; Shectman, Stephen A.; Thompson, Ian B.; Hirano, Teruyuki; Bakos, Gaspar; Hartman, Joel D. (2012), "Obliquities of Hot Jupiter host stars: Evidence for tidal interactions and primordial misalignments", The Astrophysical Journal, 757 (1): 18, arXiv: 1206.6105 , Bibcode:2012ApJ...757...18A, doi:10.1088/0004-637X/757/1/18, S2CID   17174530


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