HAT-P-36

Last updated
HAT-P-36 / Tuiren
Canes Venatici IAU.svg
Cercle rouge 100%25.svg
Location of HAT-P-36 (circled) within Canes Venatici
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Canes Venatici [1]
Right ascension 12h 33m 03.9061s [2]
Declination +44° 54′ 55.196″ [2]
Apparent magnitude  (V)12.26
Characteristics
Spectral type G
Astrometry
Radial velocity (Rv)−16.434 km/s
Proper motion (μ)RA: −11.622(8)  mas/yr [2]
Dec.: 8.138(10)  mas/yr [2]
Parallax (π)3.4055 ± 0.0110  mas [2]
Distance 958 ± 3  ly
(293.6 ± 0.9  pc)
Details
Mass 1.022 ± 0.049  M☉
Radius 1.096 ± 0.056  R☉
Temperature 5580 ± 100.0  K
Metallicity [Fe/H]0.26 ± 0.08  dex
Age 6.6 ± 1.8  Gyr
Other designations
Tuiren, Gaia DR3  1541532207133249920, TYC  3020-2221-1, 2MASS J12330390+4454552 [3]
Database references
SIMBAD data

HAT-P-36, also referred to as Tuiren [4] is a 12th magnitude G-type main-sequence star estimated to be approximately 958 light-years away from Earth [2] in the constellation Canes Venatici. HAT-P-36 is too faint to be seen with the naked eye, but it is possible to view it with binoculars or a small telescope. In 2012 a hot Jupiter-type exoplanet was discovered orbiting HAT-P-36 with an orbital period of about 1.3 Earth days. [5] In December 2019, HAT-P-36 was named Tuiren and its planetary companion, HAT-P-36b, was named Bran as a result of Ireland's contribution to the 2019 NameExoWorlds campaign. [6] Bran has a mass approximately 1.8 times that of Jupiter and a radius 1.2 times larger.

Contents

Etymology

Tuiren (centre) as viewed in the Sloan Digital Sky Survey. The bright star to the top-left is TYC 3020-2195-1, an A-type main-sequence star approximately 3,156 light-years away. Tuiren (HAT-P-36) in Aladin Lite (cropped).png
Tuiren (centre) as viewed in the Sloan Digital Sky Survey. The bright star to the top-left is TYC 3020-2195-1, an A-type main-sequence star approximately 3,156 light-years away.

HAT-P-36 and its planet are named after characters from The Birth of Bran, a story in the book Irish Fairy Tales by James Stephens. The book is a re-telling of various stories from Irish folklore. Tuiren was the aunt of the mythical hero Fionn mac Cumhaill and was turned into a hound by the fairy Uchtdealbh after Tuiren married her husband. Bran and Sceólan were the two puppies mothered by Tuiren while she was a dog. They were cousins of Fionn mac Cumhaill. The names were proposed by John Murphy, a teacher at Regina Mundi College, Cork. [8]

Planets

The HAT-P-36b planetary system [9]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b (Bran)≥1.832±0.099  MJ 0.0238±0.00041.327347±0.0000030.063±0.03286±1.3 ° 1.264±0.071  RJ

HAT-P-36b (Bran) was discovered in 2012 by the HATNet Project using the transit method. [5] A search for transit timing variation did not result in detection of additional planets in the system as at 2021. [10] Surprisingly, a planetary orbital period increase by 0.014 seconds per year was detected by 2021. [11]

Size comparison
JupiterHAT-P-36b (Bran)
Small Jupiter.jpg Exoplanet sphere.jpg

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XO-1 is a magnitude 11 G-type main-sequence star located approximately 530 light-years away in the constellation Corona Borealis. XO-1 has a mass and radius similar to the Sun. In 2006 the extrasolar planet XO-1b was discovered orbiting XO-1 by the transit method using the XO Telescope.

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HAT-P-5 is a 12th magnitude star in the constellation Lyra, approximately 1,000 light years away from Earth. It is a spectral type G star, about 1.16 solar masses and radii greater than the Sun, and only 200 kelvins hotter. It is estimated to be 2.6 billion years old.

HAT-P-6 also named Sterrennacht is a star in the constellation Andromeda, located approximately 895 light years or 274 parsecs away from the Earth. It is an F-type star, implying that it is hotter and more massive than the Sun. The apparent magnitude of the star is +10.54, which means that it can only be visible through the telescope. The absolute magnitude of +3.36 is brighter than the Sun's +4.83, meaning that the star itself is brighter than the Sun. A search for a binary companion star using adaptive optics at the MMT Observatory turned out negative.

ADS 16402 is a binary star system, composed of two sun-like stars located approximately 525 light-years away in the constellation Lacerta. It was first identified as a binary star by John Herschel in 1831. The two stars are separated by 11.26 arcseconds which leads to a projected separation of roughly 1500 astronomical units at the distance of ADS 16402. The star system is estimated to be 1.9 ± 0.6 billion years old. The secondary star ADS 16402 B is also designated HAT-P-1.

XO-5 is a yellow dwarf main sequence star located approximately 910 light-years away from Earth in the Lynx constellation. It has a magnitude of about 12 and cannot be seen with the naked eye but is visible through a small telescope.

HAT-P-9 is a magnitude 12 F star approximately 1500 light years away in the constellation Auriga. A search for a binary companion star using adaptive optics at the MMT Observatory was negative.

HAT-P-4 is a wide binary star consisting of a pair of G-type main-sequence stars in the constellation of Boötes. It is also designated BD+36°2593.

XO-2 is a binary star. It consists of two components: XO-2S and XO-2N, both of which has two known exoplanets.

HAT-P-11, also designated GSC 03561-02092 and Kepler-3, is an orange dwarf metal rich star about 123 light-years away in the constellation Cygnus. This star is notable for its relatively large rate of proper motion. The magnitude of this star is about 9, which means it is not visible to the naked eye but can be seen with a medium-sized amateur telescope on a clear dark night. The age of this star is about 6.5 billion years.

HAT-P-3, is a metal-rich K5 dwarf star located about 441 light-years away in the constellation Ursa Major. At a magnitude of about 11.5 it is not visible to the naked eye but is visible in a small to medium-sized amateur telescope. It is believed to be a relatively young star and has a slightly enhanced level of chromospheric activity.

XO-4 is a star located approximately 896 light-years away from Earth in the Lynx constellation. It has a magnitude of about 11 and cannot be seen with the naked eye but is visible through a small telescope. A search for a binary companion star using adaptive optics at MMT Observatory was negative.

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.

HAT-P-33 is a late-F dwarf star. It is orbited by a planet called HAT-P-33b. A search for a binary companion star using adaptive optics at the MMT Observatory was negative.

HAT-P-17 is a K-type main-sequence star about 92.6 parsecs (302 ly) away. It has a mass of about 0.857 ± 0.039 M☉. It is the host of two planets, HAT-P-17b and HAT-P-17c, both discovered in 2010. A search for a binary companion star using adaptive optics at the MMT Observatory was negative. A candidate companion was detected by a spectroscopic search of high-resolution K band infrared spectra taken at the Keck observatory.

WASP-121, also known as CD-38 3220, 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.

HAT-P-29, also known as Muspelheim since 2019, is a star about 1,040 light-years away. It is a G-type main-sequence star. The star's age of 2.2±1.0 billion years is less than half that of the Sun. HAT-P-29 is slightly enriched in heavy elements, having 35% more iron than the Sun.

WASP-72 is the primary of a binary star system. It is an F7 class dwarf star, with an internal structure just on the verge of the Kraft break. It is orbited by a planet WASP-72b. The age of WASP-72 is younger than the Sun at 3.55±0.82 billion years.

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-52 is a K-type main-sequence star about 570 light-years away. It is older than the Sun at 10.7+1.9
−4.5 billion years, but it has a similar fraction of heavy elements. The star has prominent starspot activity, with 3% to 14% of the stellar surface covered by areas 575±150 K cooler than the rest of the photosphere.

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) (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics . arXiv: 2208.00211 . doi: 10.1051/0004-6361/202243940 . Gaia DR3 record for this source at VizieR.
  3. ↑ "HAT-P-36". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2023-02-23.
  4. ↑ "IAU100 NameExoWorlds Approved Names" (PDF). NameExoWorlds. International Astronomical Union. Retrieved 24 July 2020.
  5. 1 2 "HAT-P-36". Open Exoplanet Catalogue. Retrieved 24 July 2020.
  6. ↑ Smith, Niall (29 September 2019). "Sky Matters: Ireland has the chance to name a star and a planet - any ideas?". Irish Examiner. Retrieved 24 July 2020.
  7. ↑ "TYC 3020-2195-1". Centre de Données astronomiques de Strasbourg. SIMBAD. Retrieved 24 July 2020.
  8. ↑ Gorey, Colm (18 December 2019). "Cork teacher names exoplanet and star after Irish mythical dogs". Silicon Republic. Retrieved 24 July 2020.
  9. ↑ "Planet HAT-P-36 b". Extrasolar Planets Encyclopaedia. Retrieved 24 July 2020.
  10. ↑ Sonbas, E.; Karaman, N.; Özdönmez, A.; Er, H.; Dhuga, K. S.; Göğüş, E.; Nasiroglu, I.; Zejmo, M. (2022), "Probing Transit Timing Variations of three hot Jupiters: HATP-36b, HATP-56b, and WASP-52b", Monthly Notices of the Royal Astronomical Society, 509 (4): 5102–5116, arXiv: 2111.05220 , doi:10.1093/mnras/stab3270
  11. ↑ Yalçınkaya, S.; Baştürk, Ö.; ElHelweh, F.; Esmer, E.M.; Yörükoğlu, O.; Yılmaz, M.; Şenavcı, H.V.; Kılıçoğlu, T.; Selam, S.O. (2021), "Analysis of the Most Precise Light Curves of HAT-P-36 Detrended from Spot Signals", Acta Astronomica, 71 (3), arXiv: 2111.11531 , doi:10.32023/0001-5237/71.3.3, S2CID   244488216
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