HAT-P-23

Last updated
HAT-P-23 / Moriah
Observation data
Epoch J2000       Equinox J2000
Constellation Delphinus
Right ascension 20h 24m 29.7235s [1]
Declination +16° 45′ 43.812″ [1]
Apparent magnitude  (V)11.94 [2]
Characteristics
Spectral type G0V
Apparent magnitude  (J)11.103±0.022 [3]
Apparent magnitude  (H)10.846±0.022 [3]
Apparent magnitude  (K)10.791±0.020 [3]
Variable type Planetary transit [4]
Astrometry
Radial velocity (Rv)-14.324 km/s
Proper motion (μ)RA: 13.325(11)  mas/yr [1]
Dec.: −5.505(11)  mas/yr [1]
Parallax (π)2.7358 ± 0.0108  mas [1]
Distance 1,192 ± 5  ly
(366 ± 1  pc)
Details [4]
Mass 1.13±0.035  M☉
Radius 1.203±0.074  R☉
Luminosity 1.58±0.23  L☉
Surface gravity (log g)4.33±0.05  cgs
Temperature 5905±80  K
Metallicity 0.15±0.04
Rotation 7.015 d [5]
Rotational velocity (v sin i)8.1±0.5 km/s
Age 4.0±1.0  Gyr
Other designations
Moriah, Gaia DR2  1808938730710633984, TYC  1632-1396-1, GSC  01632-01396, 2MASS J20242972+1645437 [2]
Database references
SIMBAD data

HAT-P-23 is a G-type main-sequence star 1192 light-years away. It has a rapid rotation (rotation period equal to 7 days) for its advanced age of 4 billion years, and exhibits a strong starspot activity. [6] The star may be in the process of being spun up by the giant planet on close orbit. [7] The star is enriched in heavy elements, having about 140% amount of metals compared to solar abundance.

Contents

Naming

In 2019, the HAT-P-23 star has received a proper name Moriah and planet HAT-P-23b - Jebus at an international NameExoWorlds contest. [8] These names mean the ancient name of the mount at the center of Jerusalem city, and ancient (pre-Roman) name of Jerusalem itself, respectively.

Planetary system

In 2010 a transiting hot Jupiter like planet was detected. [4] It has a measured dayside temperature of 2154±90 K. [9] The planet is believed to be on an unstable orbit, and expected to be engulfed by its parent star about 7.5+2.9
−1.8 million years from now, [4] although timing measurements of multiple transits since the discovery have been unable to detect any reduction in the orbital period. [5] [10] The planetary orbit is probably aligned with the equatorial plane of the star, misalignment equal to 15±22°. [11] The color of planetary atmosphere is grey. [12] The atmosphere is mostly devoid of clouds, and shows tentatively a presence of Titanium(II) oxide. [13]

Size comparison of HAT-P-23 b and Jupiter Exoplanet Comparison HAT-P-23 b.png
Size comparison of HAT-P-23 b and Jupiter
The HAT-P-23 planetary system [4] [14] [9] [12]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b (Jebus) 2.09±0.111  MJ 0.0232±0.00021.2128868±0.00000040.09685.1±1.5° 1.224±0.037  RJ

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.

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-32b is a planet orbiting the G-type or F-type star HAT-P-32, which is approximately 950 light years away from Earth. HAT-P-32b was first recognized as a possible planet by the planet-searching HATNet Project in 2004, although difficulties in measuring its radial velocity prevented astronomers from verifying the planet until after three years of observation. The Blendanal program helped to rule out most of the alternatives that could explain what HAT-P-32b was, leading astronomers to determine that HAT-P-32b was most likely a planet. The discovery of HAT-P-32b and of HAT-P-33b was submitted to a journal on 6 June 2011.

HAT-P-27, also known as WASP-40, is the primary of a binary star system about 659 light-years away. It is a G-type main-sequence star. The star's age is similar to the Sun's at 4.4 billion years. HAT-P-27 is enriched in heavy elements, having a 195% concentration of iron compared to the Sun.

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-20 is a K-type main-sequence star about 233 light-years away. The star has a strong starspot activity, and its equatorial plane is misaligned by 36+10
−12° with the planetary orbit. Although star with a giant planet on close orbit is expected to be spun-up by tidal forces, only weak indications of tidal spin-up were detected.

HAT-P-18 is a K-type main-sequence star about 530 light-years away. The star is very old and has a concentration of heavy elements similar to solar abundance. A survey in 2015 detected very strong starspot activity on HAT-P-18.

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.

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.

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.

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-64 is a star about 1200 light-years away. It is a G7 class main-sequence star, orbited by a planet WASP-64b. It is younger than the Sun at 3.6±1.6 billion years, and it has a metal abundance similar to the Sun. The star is rotating rapidly, being spun up by the giant planet in a close orbit.

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 HAT-P-23 -- Star
  3. 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
  4. 1 2 3 4 5 Bakos, G. Á.; Hartman, J.; Torres, G.; Latham, D. W.; Kovács, Géza; Noyes, R. W.; Fischer, D. A.; Johnson, J. A.; Marcy, G. W.; Howard, A. W.; Kipping, D.; Esquerdo, G. A.; Shporer, A.; Béky, B.; Buchhave, L. A.; Perumpilly, G.; Everett, M.; Sasselov, D. D.; Stefanik, R. P.; Lázár, J.; Papp, I.; Sári, P. (2010), "HAT-P-20b–HAT-P-23b: FOUR MASSIVE TRANSITING EXTRASOLAR PLANETS", The Astrophysical Journal, 742 (2): 116, arXiv: 1008.3388 , Bibcode:2011ApJ...742..116B, doi:10.1088/0004-637X/742/2/116, S2CID   119182075
  5. 1 2 Salisbury, M.A.; et al. (2021). "Monitoring of transiting exoplanets and their host stars with small aperture telescopes". New Astronomy. 83. 101477. arXiv: 2008.08379 . Bibcode: 2021NewA...8301477S . doi: 10.1016/j.newast.2020.101477 .
  6. ↑ Schrijver, Carolus J. (2020), "Testing the solar activity paradigm in the context of exoplanet transits", The Astrophysical Journal, 890 (2): 121, arXiv: 2001.01093 , Bibcode:2020ApJ...890..121S, doi: 10.3847/1538-4357/ab67c1 , S2CID   209862471
  7. ↑ Maciejewski, G.; Fernández, M.; Aceituno, F.; Martín-Ruiz, S.; Ohlert, J.; Dimitrov, D.; Szyszka, K.; von Essen, C.; Mugrauer, M.; Bischoff, R.; Michel, K. -U.; Mallonn, M.; Stangret, M.; Moździerski, D. (2018), "Planet-star interactions with precise transit timing. I. The refined orbital decay rate for WASP-12 b and initial constraints for HAT-P-23 b, KELT-1 b, KELT-16 b, WASP-33 b, and WASP-103 b", Acta Astronomica, 68 (4): 371, arXiv: 1812.02438 , Bibcode:2018AcA....68..371M, doi:10.32023/0001-5237/68.4.4, S2CID   118895482
  8. ↑ IAU 100 NameExoWorlds Approved Names
  9. 1 2 O'Rourke, Joseph G.; Knutson, Heather A.; Zhao, Ming; Fortney, Jonathan J.; Burrows, Adam; Agol, Eric; Deming, Drake; Désert, Jean-Michel; Howard, Andrew W.; Lewis, Nikole K.; Showman, Adam P.; Todorov, Kamen O. (2014). "WARMSPITZERAND PALOMAR NEAR-IR SECONDARY ECLIPSE PHOTOMETRY OF TWO HOT JUPITERS: WASP-48b AND HAT-P-23b". The Astrophysical Journal. 781 (2): 109. arXiv: 1310.0011 . Bibcode:2014ApJ...781..109O. doi:10.1088/0004-637X/781/2/109. S2CID   13149979.
  10. ↑ Patra, Kishore C.; Winn, Joshua N.; Holman, Matthew J.; Gillon, Michael; Burdanov, Artem; Jehin, Emmanuel; Delrez, Laetitia; Pozuelos, Francisco J.; Barkaoui, Khalid; Benkhaldoun, Zouhair; Narita, Norio; Fukui, Akihiko; Kusakabe, Nobuhiko; Kawauchi, Kiyoe; Terada, Yuka; Bouma, L. G.; Weinberg, Nevin N.; Broome, Madelyn (2020), "The continuing search for evidence of tidal orbital decay of hot Jupiters", The Astronomical Journal, 159 (4): 150, arXiv: 2002.02606 , Bibcode:2020AJ....159..150P, doi: 10.3847/1538-3881/ab7374 , S2CID   211066260
  11. ↑ Moutou, Claire; Diaz, Rodrigo F.; Udry, Stephane; Hebrard, Guillaume; Bouchy, Francois; Santerne, Alexandre; Ehrenreich, David; Arnold, Luc; Boisse, Isabelle; Bonfils, Xavier; Delfosse, Xavier; Eggenberger, Anne; Forveille, Thierry; Lagrange, Anne-Marie; Lovis, Christophe; Martinez, Patrick; Pepe, Francesco; Perrier, Christian; Queloz, Didier; Santos, Nuno C.; Segransan, Damien; Toublanc, Dominique; Troncin, Jean-Pierre; Vanhuysse, Michael; Vidal-Madjar, Alfred (2011), Spin-orbit inclinations of the exoplanetary systems HAT-P-8, HAT-P-9 HAT-P-16, and HAT-P-23, arXiv: 1105.3849 , Bibcode:2011A&A...533A.113M, doi:10.1051/0004-6361/201116760, S2CID   55894097
  12. 1 2 Ciceri, S.; Mancini, L.; Southworth, J.; Bruni, I.; Nikolov, N.; d'Ago, G.; Schröder, T.; Bozza, V.; Tregloan-Reed, J.; Henning, Th. (2015), "Physical properties of the HAT-P-23 and WASP-48 planetary systems from multi-colour photometry", Astronomy & Astrophysics, 577: A54, arXiv: 1503.00762 , Bibcode:2015A&A...577A..54C, doi:10.1051/0004-6361/201425449, S2CID   53607610
  13. ↑ Weaver, Ian C.; López-Morales, Mercedes; Alam, Munazza K.; Espinoza, Néstor; Rackham, Benjamin V.; Goyal, Jayesh M.; MacDonald, Ryan J.; Lewis, Nikole K.; Apai, Dániel; Bixel, Alex; Jordán, Andrés; Kirk, James; McGruder, Chima; Osip, David J. (2021), "ACCESS: An Optical Transmission Spectrum of the High-gravity Hot Jupiter HAT-P-23b", The Astronomical Journal, 161 (6): 278, arXiv: 2104.04101 , Bibcode:2021AJ....161..278W, doi: 10.3847/1538-3881/abf652 , S2CID   233204299
  14. ↑ Ramón-Fox, Felipe G.; Sada, Pedro V. (2012), "PARAMETERS OF RECENT TRANSITS OF HAT-P-23b", Revista Mexicana de Astronomía y Astrofísica, 49: 71, arXiv: 1211.6481 , Bibcode:2013RMxAA..49...71R


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