HAT-P-11

Last updated
HAT-P-11
Observation data
Epoch J2000       Equinox J2000
Constellation Cygnus [1]
Right ascension 19h 50m 50.2473s [2]
Declination +48° 04′ 51.101″ [2]
Apparent magnitude  (V)9.59 [3]
Characteristics
Spectral type K4V [3]
Apparent magnitude  (B)10.66±0.05 [4]
Apparent magnitude  (J)7.608±0.029 [5]
Apparent magnitude  (H)7.131±0.021 [5]
Apparent magnitude  (K)7.009±0.020 [5]
Variable type planetary transit [3]
Astrometry
Radial velocity (Rv)−63.46±0.13 [2]  km/s
Proper motion (μ)RA: 126.095(13)  mas/yr [2]
Dec.: 232.726(13)  mas/yr [2]
Parallax (π)26.4274 ± 0.0108  mas [2]
Distance 123.42 ± 0.05  ly
(37.84 ± 0.02  pc)
Absolute magnitude  (MV)6.57±0.09 [3]
Details
Mass 0.81+0.03
−0.02 [3]   M☉
Radius 0.683±0.009 [6]   R☉
Luminosity 0.26±0.02 [3]   L☉
Surface gravity (log g)4.59±0.03 [3]   cgs
Temperature 4780±50 [3]   K
Metallicity [Fe/H]0.31±0.05 [3]   dex
Rotation ~29.2 days [3]
Rotational velocity (v sin i)1.5±1.5 [3]  km/s
Age 6.5+5.9
−4.1 [3]   Gyr
Other designations
BD+47°2936, HIP  97657, NLTT  48335, KOI-3, KIC  10748390, GSC  03561-02092 [4]
Database references
SIMBAD data
KIC data

HAT-P-11, also designated GSC 03561-02092 and Kepler-3, is an orange dwarf metal rich star 123 light-years (38 parsecs ) away in the constellation Cygnus. This star is notable for its relatively large rate of proper motion. The apparent magnitude of this star is about 9.6, 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. [3]

Contents

The star has active latitudes that generate starspots. [7] The star appears to have an unusually small radius, which can be explained by the anomalously high helium fraction. [8]

Planetary system

Artist Illustration of planet HAT-P-11b. Artist Illustration of planet HAT-P-11b.jpg
Artist Illustration of planet HAT-P-11b.

An exoplanet, designated HAT-P-11b, was discovered by the HATNet Project using the transit method, believed to be a little larger than the planet Neptune. [3]

The planet orbits out of alignment from the star's spin axis, with an obliquity of about 100°. [7] This star system was within the field of view of the Kepler Mission planet-hunter spacecraft. [3] Water vapor and ammonia have been detected in the atmosphere of HAT-P-11b. [10]

A trend in the radial velocity measurements taken to confirm the planet indicated a possible additional body in the system. [3] This was confirmed in 2018 when a second planet, HAT-P-11c, was detected on an approximately nine-year orbit. [11] In 2020, an astrometric detection of HAT-P-11c was published, along with Pi Mensae b, allowing its inclination and true mass to be determined. [12]

However, a 2024 study suggests that the radial velocity variations attributed to HAT-P-11c may actually be caused by a magnetic activity cycle of the star. If this is the case, an outer planet may still exist given the evidence for one from astrometry, but farther from the star and with a different mass than previously thought. [10]

The HAT-P-11 planetary system [10] [11] [12]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b 25.0±1.5  M🜨 0.0532±0.00104.887802443(34)0.2577+0.0033
−0.0025		89.027±0.068 ° 4.901±0.065  R🜨
c(disputed)2.3+0.7
−0.5 MJ 		4.13+0.29
−0.16		3397+71
−64		0.604±0.03135.7+12.1
−21.4 ° 		—

See also

Related Research Articles

The Hungarian Automated Telescope Network (HATNet) project is a network of six small fully automated "HAT" telescopes. The scientific goal of the project is to detect and characterize extrasolar planets using the transit method. This network is used also to find and follow bright variable stars. The network is maintained by the Center for Astrophysics | Harvard & Smithsonian.

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.

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-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.

<span class="mw-page-title-main">HAT-P-11b</span> Super Neptune orbiting HAT-P-11

HAT-P-11b is an extrasolar planet orbiting the star HAT-P-11. It was discovered by the HATNet Project team in 2009 using the transit method, and submitted for publication on 2 January 2009.

HAT-P-7 is a F-type main sequence star located about 1088 light-years away in the constellation Cygnus. The apparent magnitude of this star is 10.5, which means it is not visible to the naked eye but can be seen with a small telescope on a clear dark night.

<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-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.

Kepler-17 is a main-sequence yellow dwarf star that is much more active than the Sun with starspots covering roughly 6% of its surface. Starspots are long-lived, with at least one persisting for 1400 days.

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.

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.

Kepler-411 is a binary star system. Its primary star Kepler-411A is a K-type main-sequence star, orbited by the red dwarf star Kepler-411B on a wide orbit, discovered in 2012.

Kepler-410 is a binary star system. Its primary star, also known as Kepler-410A, is a F-type subgiant star, orbited by the orange dwarf star Kepler-410B on a wide orbit. The companion star was discovered in 2012.

<span class="mw-page-title-main">K2-25</span>

K2-25 is a young red dwarf star located in the Hyades cluster. There is a single known Neptune-sized planet in a 3.5 day orbit.

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. 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 Bakos, G. Á.; et al. (2010). "HAT-P-11b: A Super-Neptune Planet Transiting a Bright K Star in the Kepler Field". The Astrophysical Journal. 710 (2): 1724–1745. arXiv: 0901.0282 . Bibcode: 2010ApJ...710.1724B . doi: 10.1088/0004-637X/710/2/1724 .
  4. 1 2 "BD+47 2936". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2009-04-22.
  5. 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
  6. ↑ Deming, Drake; et al. (2011). "Kepler and Ground-based Transits of the Exo-Neptune HAT-P-11b". The Astrophysical Journal. 740 (1). 33. arXiv: 1107.2977 . Bibcode: 2011ApJ...740...33D . doi: 10.1088/0004-637X/740/1/33 .
  7. 1 2 Sanchis-Ojeda, R.; Winn, J. N.; Fabrycky, D. C. (2012). "Starspots and spin-orbit alignment for Kepler cool host stars". Astronomische Nachrichten. 334 (1–2): 180–183. arXiv: 1211.2002 . Bibcode:2013AN....334..180S. doi:10.1002/asna.201211765. S2CID   38743202.
  8. ↑ Maxted, P. F. L.; Serenelli, A. M.; Southworth, J. (2015), "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
  9. ↑ "Clear skies on exo-Neptune". www.spacetelescope.org. ESA/Hubble. Retrieved 25 September 2014.
  10. 1 2 3 Basilicata, M.; Giacobbe, P.; et al. (March 2024). "The GAPS Programme at TNG LV. Multiple molecular species in the atmosphere of HAT-P-11 b and review of the HAT-P-11 planetary system". Astronomy & Astrophysics . arXiv: 2403.01527 . doi:10.1051/0004-6361/202347659.
  11. 1 2 Yee, Samuel W.; et al. (2018). "HAT-P-11: Discovery of a Second Planet and a Clue to Understanding Exoplanet Obliquities". The Astronomical Journal. 155 (6). 255. arXiv: 1805.09352 . Bibcode: 2018AJ....155..255Y . doi: 10.3847/1538-3881/aabfec .
  12. 1 2 Xuan, Jerry W.; Wyatt, Mark C. (2020), "Evidence for a high mutual inclination between the cold Jupiter and transiting super Earth orbiting π Men", Monthly Notices of the Royal Astronomical Society, 497 (2): 2096–2118, arXiv: 2007.01871 , Bibcode:2020MNRAS.497.2096X, doi:10.1093/mnras/staa2033
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