HAT-P-16

Last updated
HAT-P-16
Observation data
Epoch J2000       Equinox J2000
Constellation Andromeda
Right ascension 00h 38m 17.5584s [1]
Declination +42° 27′ 47.217″ [1]
Apparent magnitude  (V)10.91
Characteristics
Spectral type F8V
Astrometry
Radial velocity (Rv)-15.51 km/s
Proper motion (μ)RA: −21.535(12)  mas/yr [1]
Dec.: −4.582(12)  mas/yr [1]
Parallax (π)4.4958 ± 0.0155  mas [1]
Distance 725 ± 3  ly
(222.4 ± 0.8  pc)
Details [2] [3]
Mass 1.218±0.039  M☉
Radius 1.237±0.054  R☉
Luminosity 1.97±0.22  L☉
Surface gravity (log g)4.34±0.03  cgs
Temperature 6140±72  K
Metallicity 0.12±0.08
Rotational velocity (v sin i)3.5±0.5 km/s
Age 2.0±0.8  Gyr
Other designations
Gaia DR2  3815923136483872000, TYC  2792-1700-1, GSC  02792-01700, 2MASS J00381756+4227470 [4]
Database references
SIMBAD data

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, [2] and low starspot activity. [5] The survey in 2015 have failed to find any stellar companions to it. [6] 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. [7]


Planetary system

In 2010 a transiting hot superjovian planet was detected. [2] Transit-timing variation analysis in 2016 have failed to detect an additional planets in the system. [8]

In 2011 the observation utilizing a Rossiter–McLaughlin effect was performed, and the orbit of HAT-P-16b was found to be probably aligned with the equatorial plane of the star, misalignment angle equal to 10±16°. [9]

The planet HAT-P-16b equilibrium temperature was found to be equal to 1567±22 K in 2013. [3] The multiband photometry have failed to find any Rayleigh scattering in the HAT-P-16b atmosphere, which may indicate a presence of hazes or dense cloud deck. [10]

Size comparison of HAT-P-16 b and Jupiter Exoplanet Comparison HAT-P-16 b.png
Size comparison of HAT-P-16 b and Jupiter
The HAT-P-16 planetary system [2] [11] [3] [8] [12]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b4.221±0.092  MJ 0.04134+0.00044
−0.00045		2.7759704±0.00000070.0462+0.0027
−0.0024		86.6±0.7° 1.190±0.037  RJ

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.

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-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.

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.

Kepler-13 or KOI-13 is a stellar triple star system consisting of Kepler-13A, around which an orbiting hot Jupiter exoplanet was discovered with the Kepler spacecraft in 2011, and Kepler-13B a common proper motion companion star which has an additional star orbiting it.

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-26 is a K-type main-sequence star about 466 light-years away. A survey in 2015 did not find any stellar companions in orbit around it, although a red dwarf companion with a temperature 4000+100
−350 K is suspected on wide orbit.

HD 233731, or HAT-P-22, is a suspected multiple star system in the northern circumpolar constellation of Ursa Major. It is invisible to the naked eye, having an apparent visual magnitude of 9.732. This system is located at a distance of 267 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +13 km/s.

HAT-P-21 is a G-type main-sequence star about 927 light-years away. The star has amount of metals similar to solar abundance. The survey in 2015 has failed to detect any stellar companions. The star is rotating rapidly, being spun up by the tides of giant planet on close orbit.

HAT-P-15 is a G-type main-sequence star about 630 light-years away. The star is older than Sun yet has a concentration of heavy elements roughly 190% of solar abundance. The star has no noticeable starspot activity.

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.

HAT-P-28 is the primary of a binary star system about 1320 light-years away. It is a G-type main-sequence star. The star's age is older than the Sun's at 6.1+2.6
−1.9 billion years. HAT-P-28 is slightly enriched in heavy elements, having a 130% concentration of iron compared to the Sun. Since 2014, the binary star system is suspected to be surrounded by a debris disk with a 6.1″(2500 AU) radius.

References

  1. 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.
  2. 1 2 3 4 Buchhave, L. A.; Bakos, G. Á.; Hartman, J. D.; Torres, G.; Kovács, G.; Latham, D. W.; Noyes, R. W.; Esquerdo, G. A.; Everett, M.; Howard, A. W.; Marcy, G. W.; Fischer, D. A.; Johnson, J. A.; Andersen, J.; Fűrész, G.; Perumpilly, G.; Sasselov, D. D.; Stefanik, R. P.; Béky, B.; Lázár, J.; Papp, I.; Sári, P. (2010), "HAT-P-16b: A 4MJPLANET TRANSITING a BRIGHT STAR ON AN ECCENTRIC ORBIT", The Astrophysical Journal, 720 (2): 1118–1125, arXiv: 1005.2009 , Bibcode:2010ApJ...720.1118B, doi:10.1088/0004-637X/720/2/1118, S2CID   34104016
  3. 1 2 3 Ciceri, S.; Mancini, L.; Southworth, J.; Nikolov, N.; Bozza, V.; Bruni, I.; Calchi Novati, S.; d'Ago, G.; Henning, Th. (2013). "Simultaneous follow-up of planetary transits: Revised physical properties for the planetary systems HAT-P-16 and WASP-21". Astronomy & Astrophysics. 557: A30. arXiv: 1307.5874 . Bibcode:2013A&A...557A..30C. doi:10.1051/0004-6361/201321669. S2CID   55192357.
  4. ↑ HAT-P-16 -- Star
  5. ↑ Shkolnik, Evgenya L. (2013), "An Ultraviolet Investigation of Activity on Exoplanet Host Stars", The Astrophysical Journal, 766 (1): 9, arXiv: 1301.6192 , Bibcode:2013ApJ...766....9S, doi:10.1088/0004-637X/766/1/9, S2CID   118415788
  6. ↑ Piskorz, Danielle; Knutson, Heather A.; Ngo, Henry; Muirhead, Philip S.; Batygin, Konstantin; Crepp, Justin R.; Hinkley, Sasha; Morton, Timothy D. (2015), "Friends of Hot Jupiters. III. An Infrared Spectroscopic Search for Low-Mass Stellar Companions", The Astrophysical Journal, 814 (2): 148, arXiv: 1510.08062 , Bibcode:2015ApJ...814..148P, doi:10.1088/0004-637X/814/2/148, S2CID   11525988
  7. ↑ Teske, Johanna K.; Cunha, Katia; Smith, Verne V.; Schuler, Simon C.; Griffith, Caitlin A. (2014), "C/O Ratios of Stars with Transiting Hot Jupiter Exoplanets", The Astrophysical Journal, 788 (1): 39, arXiv: 1403.6891 , Bibcode:2014ApJ...788...39T, doi:10.1088/0004-637X/788/1/39, S2CID   119210392
  8. 1 2 Sada, Pedro V.; Ramón-Fox, Felipe G. (2016), "Exoplanet Transits Registered at the Universidad de Monterrey Observatory. I. HAT-P-12b, HAT-P-13b, HAT-P-16b, HAT-P-23b, and WASP-10b", Publications of the Astronomical Society of the Pacific, 128 (960): 024402, arXiv: 1601.02292 , Bibcode:2016PASP..128b4402S, doi:10.1088/1538-3873/128/960/024402, S2CID   119303757
  9. ↑ Moutou, C.; Díaz, R. F.; Udry, S.; Hébrard, G.; Bouchy, F.; Santerne, A.; Ehrenreich, D.; Arnold, L.; Boisse, I.; Bonfils, X.; Delfosse, X.; Eggenberger, A.; Forveille, T.; Lagrange, A.-M.; Lovis, C.; Martinez, P.; Pepe, F.; Perrier, C.; Queloz, D.; Santos, N. C.; Ségransan, D.; Toublanc, D.; Troncin, J. P.; Vanhuysse, M.; Vidal-Madjar, A. (2011), "Spin-orbit inclinations of the exoplanetary systems HAT-P-8b, HAT-P-9b, HAT-P-16b, and HAT-P-23b", Astronomy & Astrophysics, 533: A113, arXiv: 1105.3849 , Bibcode:2011A&A...533A.113M, doi:10.1051/0004-6361/201116760, S2CID   55894097
  10. ↑ Pearson, Kyle A.; Turner, Jake D.; Sagan, Thomas G. (2013), "Photometric observation of HAT-P-16b in the near-UV", New Astronomy, 27: 102–110, arXiv: 1310.5397 , doi:10.1016/j.newast.2013.08.002, S2CID   119309058
  11. ↑ Husnoo, Nawal; Pont, Frédéric; Mazeh, Tsevi; Fabrycky, Daniel; Hébrard, Guillaume; Bouchy, François; Shporer, Avi (2012), "Observational constraints on tidal effects using orbital eccentricities★", Monthly Notices of the Royal Astronomical Society, 422 (4): 3151–3177, arXiv: 1202.6379 , Bibcode:2012MNRAS.422.3151H, doi:10.1111/j.1365-2966.2012.20839.x, S2CID   119179880
  12. ↑ Bonomo, A. S.; et al. (2017), "The GAPS Programme with HARPS-N at TNG", Astronomy & Astrophysics, 602: A107, arXiv: 1704.00373 , Bibcode:2017A&A...602A.107B, doi:10.1051/0004-6361/201629882, S2CID   118923163
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