HAT-P-19

Last updated
HAT-P-19
Observation data
Epoch J2000       Equinox J2000
Constellation Andromeda
Right ascension 00h 38m 04.0136s [1]
Declination +34° 42′ 41.554″ [1]
Apparent magnitude  (V)12.901 [2]
Characteristics
Spectral type K1V
Astrometry
Radial velocity (Rv)−20.27 km/s
Proper motion (μ)RA: −26.745(11)  mas/yr [1]
Dec.: −32.568(10)  mas/yr [1]
Parallax (π)4.9567 ± 0.0137  mas [1]
Distance 658 ± 2  ly
(201.7 ± 0.6  pc)
Details [3]
Mass 0.863+0.029
−0.025  M☉
Radius 0.851±0.013  R☉
Luminosity 0.37+0.08
−0.06 [4]   L☉
Surface gravity (log g)4.514+0.019
−0.017  cgs
Temperature 5049+42
−65  K
Metallicity 0.283+0.081
−0.079
Rotation 14.66±0.03 d [4]
Rotational velocity (v sin i)0.7±0.5 [4]  km/s
Age 8.8±5.2 [4]   Gyr
Other designations
Gaia DR2  3654266795168165128, 2MASS J00380401+3442416 [5]
Database references
SIMBAD data

HAT-P-19 is a K-type main-sequence star about 658 light-years away. The star is old yet metal enriched, having amount of heavy elements 250% of solar abundance. [4] The survey in 2012 have failed to find any stellar companions to HAT-P-19. [6]

Planetary system

In 2010 a transiting hot Saturn-sized planet was detected. [2] Its equilibrium temperature is 984±10 K, [7] and it is grey in color. [8]

The transit-timing variation measurements in 2015 and 2018 did not detect additional planets in the system. [9] [10]

Size comparison of HAT-P-19 b and Jupiter Exoplanet Comparison HAT-P-19 b.png
Size comparison of HAT-P-19 b and Jupiter
The HAT-P-19 planetary system [2] [7]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b0.290±0.016  MJ 0.04649±4.00878236+0.00000050
−0.00000049		0.084±0.04188.67+0.41
−0.25 ° 		1.089±0.018  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-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-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.

<span class="mw-page-title-main">WASP-21</span> Star in the constellation Pegasus

WASP-21 is a G-type star that is reaching the end of its main sequence lifetime approximately 850 light years from Earth in the constellation of Pegasus. The star is relatively metal-poor, having 40% of heavy elements compared to the Sun. Kinematically, WASP-21 belongs to the thick disk of the Milky Way. It has an exoplanet named WASP-21b.

WASP-29 is a binary star system 285 light-years away in the constellation of Phoenix. The primary star is a K-type main-sequence star. Its comoving companion, a red dwarf star, was discovered in 2021. The star system kinematically belongs to the thin disk of the Milky Way. The primary is an old star with small starspot activity and low x-ray flux.

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.

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

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.

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.

GSC 03949-00967 is a G-type main-sequence star about 1179 light-years away. It is older than the Sun, yet is enriched by heavy elements compared to the Sun, having 160% of solar abundance.

HD 108863 is a subgiant star, the primary of a binary star system 540 light-years away, belonging to spectral class K0. Its age is younger than the Sun's at 1.8±0.4 billion years. The primary star is slightly enriched in heavy elements, having 115% of solar abundance. The primary star does not have detectable flare activity.

KELT-1 is a F-type main-sequence star. Its surface temperature is 6518±50 K. It is similar to the Sun in its concentration of heavy elements, with a metallicity Fe/H index of 0.008±0.073, but is much younger at an age of 1.75±0.25 billion years. The star is rotating very rapidly.

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 Hartman, J. D.; Bakos, G. Á.; Sato, B.; Torres, G.; Noyes, R. W.; Latham, D. W.; Kovács, G.; Fischer, D. A.; Howard, A. W.; Johnson, J. A.; Marcy, G. W.; Buchhave, L. A.; Füresz, G.; Perumpilly, G.; Béky, B.; Stefanik, R. P.; Sasselov, D. D.; Esquerdo, G. A.; Everett, M.; Csubry, Z.; Lázár, J.; Papp, I.; Sári, P. (2010), "HAT-P-18b and HAT-P-19b: Two Low-Density Saturn-Mass Planets Transiting Metal-Rich K Stars", The Astrophysical Journal, 726: 52, arXiv: 1007.4850 , doi:10.1088/0004-637X/726/1/52, S2CID   10896305
  3. ↑ Wang, Xian-Yu; et al. (1 July 2021). "Transiting Exoplanet Monitoring Project (TEMP). VI. The Homogeneous Refinement of System Parameters for 39 Transiting Hot Jupiters with 127 New Light Curves". The Astrophysical Journal Supplement Series. 255 (1). 15. arXiv: 2105.14851 . Bibcode:2021ApJS..255...15W. doi: 10.3847/1538-4365/ac0835 . S2CID   235253975.
  4. 1 2 3 4 5 Everett, Mark E.; Howell, Steve B.; Silva, David R.; Szkody, Paula (2013), "Spectroscopy of Faint Kepler Mission Exoplanet Candidate Host Stars", The Astrophysical Journal, 771 (2): 107, arXiv: 1305.0578 , Bibcode:2013ApJ...771..107E, doi:10.1088/0004-637X/771/2/107, S2CID   119270620
  5. ↑ HAT-P-19 -- Star
  6. ↑ Ginski, C.; Mugrauer, M.; Seeliger, M.; Eisenbeiss, T. (2012), "A lucky imaging multiplicity study of exoplanet host stars", Monthly Notices of the Royal Astronomical Society, 421 (3): 2498–2509, arXiv: 1202.4586 , Bibcode:2012MNRAS.421.2498G, doi: 10.1111/j.1365-2966.2012.20485.x , S2CID   118573795
  7. 1 2 Basturk, Ozgur; Yalcinkaya, Selcuk; Esmer, Ekrem M.; Tanriverdi, Taner; Keten, Burak (2019), A Holistic and Probabilistic Approach to the Ground-based Data of HAT-P-19 System, arXiv: 1911.07903 , doi: 10.1093/mnras/staa1758 , S2CID   208158330
  8. ↑ Mallonn, M.; von Essen, C.; Weingrill, J.; Strassmeier, K. G.; Ribas, I.; Carroll, T. A.; Herrero, E.; Granzer, T.; Claret, A.; Schwope, A. (2015), "Transmission spectroscopy of the inflated exo-Saturn HAT-P-19b", Astronomy & Astrophysics, 580: A60, arXiv: 1506.05685 , Bibcode:2015A&A...580A..60M, doi:10.1051/0004-6361/201423778, S2CID   91175943
  9. ↑ Seeliger, M.; Kitze, M.; Errmann, R.; Richter, S.; Ohlert, J. M.; Chen, W. P.; Guo, J. K.; Göğüş, E.; Güver, T.; Aydın, B.; Mottola, S.; Hellmich, S.; Fernandez, M.; Aceituno, F. J.; Dimitrov, D.; Kjurkchieva, D.; Jensen, E.; Cohen, D.; Kundra, E.; Pribulla, T.; Vaňko, M.; Budaj, J.; Mallonn, M.; Wu, Z.-Y.; Zhou, X.; Raetz, St.; Adam, C.; Schmidt, T. O. B.; Ide, A.; et al. (2015), "Ground-based transit observations of the HAT-P-18, HAT-P-19, HAT-P-27/WASP40 and WASP-21 systems", Monthly Notices of the Royal Astronomical Society, 451 (4): 4060–4072, arXiv: 1508.06215 , doi: 10.1093/mnras/stv1187 , S2CID   56034663
  10. ↑ MacIejewski, G.; Stangret, M.; Ohlert, J.; Basaran, Ç.S.; MacIejczak, J.; Puciata-Mroczynska, M.; Boulanger, E. (2018), "New transit timing observations for GJ 436 b, HAT-P-3 b, HAT-P-19 b, WASP-3 b, and XO-2 B", Information Bulletin on Variable Stars, 6243 (6243): 1, arXiv: 1808.03306 , Bibcode:2018IBVS.6243....1M, doi:10.22444/IBVS.6243, S2CID   118872603
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