WASP-19

Last updated
WASP-19 / Wattle
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Vela [1]
Right ascension 09h 53m 40.07656s [2]
Declination −45° 39′ 33.0572″ [2]
Apparent magnitude  (V)12.312 ± 0.017 [3]
Characteristics
Spectral type G8V
Apparent magnitude  (B)13.58
Apparent magnitude  (R)12.17
Apparent magnitude  (I)11.35
Apparent magnitude  (J)10.911 ± 0.026 [4]
Apparent magnitude  (H)10.602 ± 0.022 [4]
Apparent magnitude  (K)10.481 ± 0.023 [4]
B−V color index 1.3
V−R color index 0.1
R−I color index 0.82
Variable type planetary transit
Astrometry
Radial velocity (Rv)21.41±0.95 [2]  km/s
Proper motion (μ)RA: −35.457  mas/yr [2]
Dec.: 17.378  mas/yr [2]
Parallax (π)3.7516 ± 0.0090  mas [2]
Distance 869 ± 2  ly
(266.6 ± 0.6  pc)
Absolute magnitude  (MV)5.3
Details [5]
Mass 0.97±0.02 [6]   M☉
Radius 0.885+0.086
−0.084  R☉
Luminosity 0.71  L☉
Surface gravity (log g)4.45 ± 0.05 [7]   cgs
Temperature 5568 ± 71 [7]   K
Metallicity [Fe/H]0.15 ± 0.07 [7]   dex
Rotation 11.76±0.09 d
Rotational velocity (v sin i)4.0 ± 1.0 [7]  km/s
Age 9.95±2.49  Gyr
Other designations
Wattle, TOI-655, WASP-19, GSC  08181-01711, 2MASS J09534008-4539330, USNO-B1.0 0443-00193111
Database references
SIMBAD data

WASP-19, formally named Wattle, [8] is a magnitude 12.3 star about 869 light-years (266 parsecs ) away, located in the Vela constellation of the southern hemisphere. [9] This star has been found to host a transiting hot Jupiter-type planet in tight orbit.

Contents

WASP-19 is older than the Sun, has a fraction of heavy elements above the solar abundance, and is rotating rapidly, being spun up by the tides raised by the giant planet on a close orbit. [5]

Nomenclature

The designation WASP-19 indicates that this was the 19th star found to have a planet by the Wide Angle Search for Planets.

In August 2022, this planetary system was included among 20 systems to be named by the third NameExoWorlds project. [10] The approved names were proposed by a team from Brandon Park Primary School in Wheelers Hill (Melbourne, Australia), led by scientist Lance Kelly and teacher David Maierhofer [11] and announced in June 2023. WASP-19 is named "Wattle" and its planet is named "Banksia", after the plant genera Wattle (specifically the golden wattle Acacia pycnantha ) and Banksia (specifically the scarlet banksia Banksia coccinea ) respectively. [8]

Planetary system

In December 2009, the SuperWASP project announced that a hot Jupiter type exoplanet, WASP-19b, was orbiting very close to this star and with the shortest orbital period of any transiting exoplanet known at the time. [9]

The WASP-19 planetary system [12] [6]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b / Banksia 1.168±0.023  MJ 0.01634 ± 0.000190.7888396 ± 0.00000010078.76 ± 0.13° 1.18±0.12  RJ

See also

Related Research Articles

<span class="mw-page-title-main">WASP-6b</span> Extrasolar planet

WASP-6b, also named Boinayel, is an exoplanet approximately 650 light years away in the constellation Aquarius. It was discovered in 2008, by the WASP survey, by astronomical transit across its parent star WASP-6. This planet orbits at only 4% of the Earth-Sun distance. The planet has a mass half that of Jupiter, but its insolation has forced a thermal expansion of its radius to greater than that of Jupiter. Thus, this planet is an inflated hot Jupiter. Starspots on the host star WASP-6 helped to refine the measurements of the mass and the radius of the planet.

<span class="mw-page-title-main">WASP-4</span> G-type main sequence star in the constellation Phoenix

WASP-4 is a G-type main-sequence star approximately 891 light-years away in the constellation of Phoenix. Despite its advanced age, the star is rotating rapidly, being spun up by the tides raised by a giant planet on a close orbit.

GSC 03089-00929 is a magnitude 12 star located approximately 757 light-years away in the constellation of Hercules. This star is a G type main sequence star that is similar to but slightly cooler than the Sun. This star is identified in SIMBAD as a variable star per the 1SWASP survey.

HAT-P-12 is a magnitude 13 low-metallicity K dwarf star approximately 463 light years away in the constellation Canes Venatici, which hosts one known exoplanet.

WASP-17 is an F-type main sequence star approximately 1,310 light-years away in the constellation Scorpius.

WASP-16 is a magnitude 11 yellow dwarf main sequence star, with characteristics similar to the Sun, located in the Virgo constellation.

WASP-18 is a magnitude 9 star located 400 light-years away in the Phoenix constellation of the southern hemisphere. It has a mass of 1.29 solar masses.

<span class="mw-page-title-main">WASP-19b</span> Extrasolar planet in the constellation Vela

WASP-19b, formally named Banksia, is an exoplanet, notable for possessing one of the shortest orbital periods of any known planetary body: 0.79 days or approximately 18.932 hours. It has a mass close to that of Jupiter, but by comparison has a much larger radius ; making it nearly the size of a low-mass star. It orbits the star WASP-19 in the Vela constellation. At the time of discovery it was the shortest period hot Jupiter discovered as planets with shorter orbital periods had a rocky, or metallic composition.

<span class="mw-page-title-main">HAT-P-14b</span> Exoplanet in the constellation of Hercules

HAT-P-14b, officially named Sissi also known as WASP-27b, is an extrasolar planet located approximately 224.2 ± 0.6 parsecs (731.2 ± 2.0 ly) away in the constellation of Hercules, orbiting the 10th magnitude F-type main-sequence star HAT-P-14. This planet was discovered in 2010 by the HATNet Project using the transit method. It was independently detected by the SuperWASP project.

HAT-P-24 is an F8 dwarf star about 413 parsecs away. A planet was discovered with the transit method by the HATNet Project in 2010. HAT-P-24b, is a typical hot Jupiter orbiting in only 3 days.

<span class="mw-page-title-main">WASP-22b</span> Jovian size planet orbiting WASP-22

WASP-22b, also named Koyopa', is an extrasolar planet orbiting the Sun-like star WASP-22 320 parsecs (1,000 ly) in the constellation Eridanus. This hot Jupiter has an orbit of 3.53 days and a mass of 0.617 MJ and was detected by transit via SuperWASP. The system is a hierarchical triple system.

WASP-121, also known as CD-38 3220 and formally named Dilmun, is a magnitude 10.4 star located approximately 858 light-years away in the constellation Puppis. WASP-121 has a mass and radius similar to the Sun's. It hosts one known exoplanet.

HD 146389, is a star with a yellow-white hue in the northern constellation of Hercules. The star was given the formal name Irena by the International Astronomical Union in January 2020. It is invisible to the naked eye with an apparent visual magnitude of 9.4 The star is located at a distance of approximately 446 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −9 km/s. The star is known to host one exoplanet, designated WASP-38b or formally named 'Iztok'.

WASP-26 is a yellow main sequence star in the constellation of Cetus.

WASP-46 is a G-type main-sequence star about 1,210 light-years away. The star is older than the Sun and is strongly depleted in heavy elements compared to the Sun, having just 45% of the solar abundance. Despite its advanced age, the star is rotating rapidly, being spun up by the tides raised by a giant planet on a close orbit.

Qatar-2 is a K-type main-sequence star about 595 light-years away in the constellation of Virgo. The star is much older than Sun, and has a concentration of heavy elements similar to solar abundance. The star features a numerous and long-lived starspots, and belongs to a peculiar variety of inflated K-dwarfs with strong magnetic activity inhibiting internal convection.

WASP-62, formally named Naledi, is a single star about 573 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-69, also named Wouri, is a K-type main-sequence star 164 light-years away. 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.

References

  1. ↑ Roman, Nancy G. (1987). "Identification of a Constellation From a Position". Publications of the Astronomical Society of the Pacific. 99 (617): 695–699. Bibcode:1987PASP...99..695R. doi: 10.1086/132034 . Vizier query form
  2. 1 2 3 4 5 6 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. ↑ Maxted, P. F. L.; et al. (2011). "UBV(RI)C photometry of transiting planet hosting stars". Monthly Notices of the Royal Astronomical Society. 418 (2): 1039–1042. arXiv: 1108.0349 . Bibcode:2011MNRAS.418.1039M. doi: 10.1111/j.1365-2966.2011.19554.x . S2CID   117056033.
  4. 1 2 3 Skrutskie, Michael F.; Cutri, Roc M.; Stiening, Rae; Weinberg, Martin D.; Schneider, Stephen E.; Carpenter, John M.; Beichman, Charles A.; Capps, Richard W.; Chester, Thomas; Elias, Jonathan H.; Huchra, John P.; Liebert, James W.; Lonsdale, Carol J.; Monet, David G.; Price, Stephan; Seitzer, Patrick; Jarrett, Thomas H.; Kirkpatrick, J. Davy; Gizis, John E.; Howard, Elizabeth V.; Evans, Tracey E.; Fowler, John W.; Fullmer, Linda; Hurt, Robert L.; Light, Robert M.; Kopan, Eugene L.; Marsh, Kenneth A.; McCallon, Howard L.; Tam, Robert; Van Dyk, Schuyler D.; Wheelock, Sherry L. (1 February 2006). "The Two Micron All Sky Survey (2MASS)". The Astronomical Journal. 131 (2): 1163–1183. Bibcode:2006AJ....131.1163S. doi: 10.1086/498708 . ISSN   0004-6256. S2CID   18913331. Vizier catalog entry
  5. 1 2 Maxted, P. F. L.; Serenelli, A. M.; Southworth, J. (2015), "A comparison of gyrochronological and isochronal age estimates for transiting exoplanet host stars", Astronomy & Astrophysics, 577: A90, arXiv: 1503.09111 , Bibcode:2015A&A...577A..90M, doi:10.1051/0004-6361/201525774, S2CID   53324330
  6. 1 2 Dragomir, Diana; Kane, Stephen R.; Pilyavsky, Genady; Mahadevan, Suvrath; Ciardi, David R.; Zachary Gazak, J.; Gelino, Dawn M.; Payne, Alan; Rabus, Markus; Ramirez, Solange V.; von Braun, Kaspar; Wright, Jason T.; Wyatt, Pamela (2011). "Terms Photometry of Known Transiting Exoplanets". The Astronomical Journal. 142 (4): 115. arXiv: 1108.2308 . Bibcode:2011AJ....142..115D. doi:10.1088/0004-6256/142/4/115. S2CID   118606598.
  7. 1 2 3 4 Torres, Guillermo; et al. (2012). "Improved Spectroscopic Parameters for Transiting Planet Hosts". The Astrophysical Journal. 757 (2). 161. arXiv: 1208.1268 . Bibcode:2012ApJ...757..161T. doi:10.1088/0004-637X/757/2/161. S2CID   16580774.
  8. 1 2 "2022 Approved Names". nameexoworlds.iau.org. IAU . Retrieved 7 June 2023.
  9. 1 2 Hebb, L.; et al. (2010). "WASP-19b: The Shortest Period Transiting Exoplanet Yet Discovered". The Astrophysical Journal. 708 (1): 224–231. arXiv: 1001.0403 . Bibcode:2010ApJ...708..224H. doi:10.1088/0004-637X/708/1/224. S2CID   119189785.
  10. ↑ "List of ExoWorlds 2022". nameexoworlds.iau.org. IAU. 8 August 2022. Retrieved 27 August 2022.
  11. ↑ "Facebook". www.facebook.com.
  12. ↑ Mancini, L.; et al. (2013). "Physical properties, transmission and emission spectra of the WASP-19 planetary system from multi-colour photometry". Monthly Notices of the Royal Astronomical Society . 436 (1): 2–18. arXiv: 1306.6384 . Bibcode:2013MNRAS.436....2M. doi: 10.1093/mnras/stt1394 . S2CID   55455709.
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