HAT-P-6

Last updated
HAT-P-6 / Sterrennacht
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Andromeda [1]
Right ascension 23h 39m 05.8103s [2]
Declination +42° 27′ 57.505″ [2]
Apparent magnitude  (V)+10.47 [3]
Characteristics
Spectral type F8V [4]
B−V color index 0.41 [3]
Variable type planetary transit [5]
Astrometry
Radial velocity (Rv)−22.13(44) [6]  km/s
Proper motion (μ)RA: −20.202(18)  mas/yr [2]
Dec.: 2.996(18)  mas/yr [2]
Parallax (π)3.6459 ± 0.0221  mas [2]
Distance 895 ± 5  ly
(274 ± 2  pc)
Absolute magnitude  (MV)+3.36(16) [5]
Details
Mass 1.29 ± 0.06 [7]   M☉
Radius 1.46 ± 0.06 [7]   R☉
Luminosity 3.57+0.52
−0.43 [5]   L☉
Surface gravity (log g)4.22 ± 0.03 [8]   cgs
Temperature 6,570 ± 80 [7]   K
Metallicity [Fe/H]–0.13 ± 0.08 [7]   dex
Rotational velocity (v sin i)8.7 ± 1.0 [7]  km/s
Age 2.3+0.5
−0.7 [7]   Gyr
Other designations
Sterrennacht, Gaia DR3  1925321658551399040, TYC  3239-992-1, GSC  03239-00992, 2MASS J23390581+4227575 [9]
Database references
SIMBAD data

HAT-P-6 also named Sterrennacht [10] 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. [5] A search for a binary companion star using adaptive optics at the MMT Observatory turned out negative. [11]

Contents

The name Sterrennacht (Starry Night) was selected in the NameExoWorlds held by the IAU after a painting by Van Gogh. [10]

Planetary system

The companion planet HAT-P-6b is a transiting planet discovered on October 15, 2007 by the HATNet Project. The planet's true mass is slightly more than Jupiter at only 5.7%, but the radius is 33% greater, making the planet's density of 0.45 g/cm3. Its large size compared to mass comes from the great amount of heat received from the nearby star that expands the planet's atmosphere, categorizing as "hot Jupiter". The orbital period is 3.852985 days and the distance from its star is 0.05235 AU. [5] The inclination of the orbit with respect to the stellar rotation axis is roughly 166º. [12]

The HAT-P-6 planetary system [5] [7]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b / Nachtwacht 1.106+0.039
−0.040  MJ 		0.05239+0.00080
−0.00082		3.852985±0.000005<0.044166±10 [12] ° 1.330±0.061  RJ

See also

Related Research Articles

HD 147506, also known as HAT-P-2 and formally named Hunor, is a magnitude 8.7 F8 dwarf star that is somewhat larger and hotter than the Sun. The star is approximately 419 light-years from Earth and is positioned near the keystone of Hercules. It is estimated to be 2 to 3 billion years old, towards the end of its main sequence life. There is one known transiting exoplanet, and a second planet not observed to transit.

<span class="mw-page-title-main">HAT-P-2b</span> Extrasolar planet

HAT-P-2b is an extrasolar planet detected by the HATNet Project in May 2007. It orbits a class F star HAT-P-2,, located about 420 light-years away in the constellation Hercules.

<span class="mw-page-title-main">HAT-P-6b</span> Extrasolar planet in the Andromeda constellation

HAT-P-6b is a transiting extrasolar planet discovered by Noyes et al. on October 15, 2007. It is located approximately 910 light-years away in the constellation of Andromeda, orbiting the star HAT-P-6. This hot Jupiter planet orbits with a semi-major axis of about 0.05 AU, and takes 92 hours, 28 minutes, 17 seconds to orbit the star. It has true mass of 5.7% greater than Jupiter and a radius 33% greater than Jupiter, corresponding to a density of 0.583 g/cm3, which is less than water.

HD 118203 is a star with an orbiting exoplanet located in the northern circumpolar constellation of Ursa Major. It has the proper name Liesma, which means flame, and it is the name of a character from the Latvian poem Staburags un Liesma. The name was selected in the NameExoWorlds campaign by Latvia, during the 100th anniversary of the IAU.

WASP-11/HAT-P-10 is a binary star. It is a primary main-sequence orange dwarf star. Secondary is M-dwarf with a projected separation of 42 AU. The system is located about 424 light-years away in the constellation Aries.

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.

HAT-P-8 is a magnitude 10 star located 700 light-years away in Pegasus. It is a F-type star about 28% more massive than the Sun. Two red dwarf companions have been detected around HAT-P-8. The first has a spectral type of M5V and has a mass of 0.22 M☉. The second is even less massive, at 0.18 M☉, and its spectral type is M6V.

HAT-P-13, also known as GSC 03416-00543, is a G-type main sequence star approximately 800 light-years away in the constellation Ursa Major. In 2009 it was discovered that this star is orbited by two massive planets, the innermost of which transits the star. This was the first known example of an extrasolar transiting planet with an additional planet in the same system.

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">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.

HAT-P-17 is a K-type main-sequence star about 92.4 parsecs (301 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.

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'.

HAT-P-16 is a F-type main-sequence star about 725 light-years away. The star has a concentration of heavy elements slightly higher than solar abundance, and low starspot activity. The survey in 2015 have failed to find any stellar companions to it. The spectral analysis in 2014 have discovered the HAT-P-16 has a carbon to oxygen molar ratio of 0.58±0.08, close to Sun`s value of 0.55.

HAT-P-30, also known as WASP-51, is the primary of a binary star system about 700 light-years away. It is a G-type main-sequence star. HAT-P-30 has a similar concentration of heavy elements compared to the Sun.

WASP-41 is a G-type main-sequence star. Its surface temperature is 5450±150 K. WASP-41 is similar to the Sun in its concentration of heavy elements, with a metallicity Fe/H index of −0.080±0.090, but is much younger at an age of 2.289±0.077 billion years. The star does exhibit strong starspot activity, with spots covering 3% of the stellar surface.

HAT-P-41 is a binary star system. Its primary is a F-type main-sequence star. Its surface temperature is 6390±100 K. compared to the Sun, HAT-P-41 is enriched in heavy elements, with a metallicity Fe/H index of 0.21±0.10, but is much younger at an age of 2.2±0.4 billion years.

HATS-3 is an F-type main-sequence star 1,380 light-years away. Its surface temperature is 6351±76 K. HATS-3 is relatively depleted in its concentration of heavy elements, with a metallicity Fe/H index of −0.157±0.07, but is slightly younger than the Sun at an age of 3.2+0.6
−0.4 billion years.

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 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. 1 2 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 & Astrophysics, 355: L27–L30, Bibcode:2000A&A...355L..27H.
  4. ↑ Faedi, F.; Staley, T.; Gómez Maqueo Chew, Y.; Pollacco, D.; Dhital, S.; Barros, S. C. C.; Skillen, I.; Hebb, L.; MacKay, C.; Watson, C. A. (2013). "Lucky imaging of transiting planet host stars with LuckyCam". Monthly Notices of the Royal Astronomical Society. 433 (3): 2097. arXiv: 1305.3795 . Bibcode:2013MNRAS.433.2097F. doi: 10.1093/mnras/stt885 . S2CID   21090559.
  5. 1 2 3 4 5 6 Noyes, R. W.; et al. (2008). "HAT-P-6b: A Hot Jupiter Transiting a Bright F Star". The Astrophysical Journal Letters. 673 (1): L79–L82. arXiv: 0710.2894 . Bibcode:2008ApJ...673L..79N. doi:10.1086/527358. S2CID   2301387.
  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.
  7. 1 2 3 4 5 6 7 Bonomo, A. S.; et al. (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 and Astrophysics. 602. A107. arXiv: 1704.00373 . Bibcode:2017A&A...602A.107B. doi:10.1051/0004-6361/201629882. S2CID   118923163.
  8. ↑ 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.
  9. ↑ "HAT-P-6". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2023-02-26.
  10. 1 2 "Approved names". NameExoworlds. Retrieved 2020-01-02.
  11. ↑ Adams, E. R.; et al. (2013). "Adaptive Optics Images. II. 12 Kepler Objects of Interest and 15 Confirmed Transiting Planets". The Astronomical Journal. 146 (1). 9. arXiv: 1305.6548 . Bibcode:2013AJ....146....9A. doi:10.1088/0004-6256/146/1/9. S2CID   119117620.
  12. 1 2 Hébrard, Guillaume; Ehrenreich, David; Bouchy, François; Delfosse, Xavier; Moutou, Claire; Arnold, Luc; Boisse, Isabelle; Bonfils, Xavier; Díaz, Rodrigo F.; Eggenberger, Anne; Forveille, Thierry; Lagrange, Anne-Marie; Lovis, Christophe; Pepe, Francesco; Perrier, Christian; Queloz, Didier; Santerne, Alexandre; Santos, Nuno C.; Ségransan, Damien; Udry, Stéphane; Vidal-Madjar, Alfred (2011). "The retrograde orbit of the HAT-P-6b exoplanet". Astronomy and Astrophysics. 527: L11. arXiv: 1101.5009 . Bibcode:2011A&A...527L..11H. doi:10.1051/0004-6361/201016331. S2CID   56130884.
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