HAT-P-25

Last updated
HAT-P-25
Observation data
Epoch J2000       Equinox J2000
Constellation Aries
Right ascension 03h 13m 44.4981s [1]
Declination +25° 11′ 50.689″ [1]
Apparent magnitude  (V)13.15 [2]
Characteristics
Spectral type G5V
Astrometry
Proper motion (μ)RA: 13.490(21)  mas/yr [1]
Dec.: −13.684(16)  mas/yr [1]
Parallax (π)3.3128 ± 0.0178  mas [1]
Distance 985 ± 5  ly
(302 ± 2  pc)
Details [3]
Mass 1.012+0.051
−0.051  M☉
Radius 0.919±0.034  R☉
Surface gravity (log g)4.516+0.026
−0.025  cgs
Temperature 5519+78
−76  K
Metallicity 0.29±0.08
Age 3.2±2.3  Gyr
Other designations
Gaia DR2  3668036348641580288, TYC  320-1027-1, GSC  0320-01027, 2MASS J14123753+0403359 [2]
Database references
SIMBAD data

HAT-P-25 is a G-type main-sequence star about 985 light-years away. It has a very low flare activity. [4] The star is enriched in heavy elements, having about twice amount of metals compared to solar abundance.

Planetary system

In 2010 a transiting hot Jupiter like planet was detected. [5] It has an equilibrium temperature of 1182±25 K. [3] The stability of orbits within circumstellar habitable zone is not significantly affected by the HAT-P-25b planet. [6]

Size comparison of HAT-P-25 b and Jupiter Exoplanet Comparison HAT-P-25 b.png
Size comparison of HAT-P-25 b and Jupiter
The HAT-P-25 planetary system [5] [3]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b0.569+0.023
−0.022  MJ 		0.0466±0.00053.65281514+0.00000076
−0.00000075		0.023+0.022
−0.014		87.6±0.5° 1.135±0.048  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-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.

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-27, also known as WASP-40, is the primary of a binary star system about 650 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.

WASP-37 is a yellow main sequence star in the constellation of Virgo.

WASP-36 is a yellow main sequence star in the Hydra constellation.

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-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-29, also known as Muspelheim since 2019, is a star about 1,040 light-years away. It is a G-type main-sequence star. The star's age of 2.2±1.0 billion years is less than half that of the Sun. HAT-P-29 is slightly enriched in heavy elements, having 35% more iron than 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.

Qatar-4 is a faint K-dwarf star that hosts a planet in the constellation Andromeda. With an apparent magnitude of 13.60, it is impossible to detect with the naked eye, but can be detected with a powerful telescope. Qatar-4 is currently located 1,083 light years away based on parallax.

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-25 -- Star
  3. 1 2 3 Wang, Xian-Yu; Wang, Songhu; Hinse, Tobias C.; Li, Kai; Wang, Yong-Hao; Laughlin, Gregory; Liu, Hui-Gen; Zhang, Hui; Wu, Zhen-Yu; Zhou, Xu; Zhou, Ji-Lin; Hu, Shao-Ming; Wu, Dong-Hong; Peng, Xi-Yan; Chen, Yuan-Yuan (2018), "Transiting Exoplanet Monitoring Project (TEMP). IV. Refined System Parameters, Transit Timing Variations and Orbital Stability of the Transiting Planetary System HAT-P-25", Publications of the Astronomical Society of the Pacific, 130 (988): 064401, arXiv: 1805.01580 , Bibcode:2018PASP..130f4401W, doi:10.1088/1538-3873/aab93e, S2CID   118993367
  4. ↑ Evgenya L. Shkolnik, "AN ULTRAVIOLET INVESTIGATION OF ACTIVITY ON EXOPLANET HOST STARS", 2013
  5. 1 2 Quinn, S. N.; Bakos, G. Á.; Hartman, J.; Torres, G.; Kovács, G.; Latham, D. W.; Noyes, R. W.; Fischer, D. A.; Johnson, J. A.; Marcy, G. W.; Howard, A. W.; Szentgyorgyi, A.; Fűrész, G.; Buchhave, L. A.; Béky, B.; Sasselov, D. D.; Stefanik, R. P.; Perumpilly, G.; Everett, M.; Lázár, J.; Papp, I.; Sári, P. (2010), "HAT-P-25b: a Hot-Jupiter Transiting a Moderately Faint G Star", The Astrophysical Journal, 745: 80, arXiv: 1008.3565 , doi:10.1088/0004-637X/745/1/80, S2CID   119291022
  6. ↑ Nikolaos Georgakarakos, Siegfried Eggl, and Ian Dobbs-Dixon, "Giant Planets: Good Neighbors for Habitable Worlds?", 2018


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