GSC 03949-00967

Last updated
GSC 03949-00967
Observation data
Epoch J2000       Equinox J2000
Constellation Cygnus
Right ascension 20h 20m 53.2482s [1]
Declination +59° 26 55.575 [1]
Apparent magnitude  (V)13.58
Characteristics
Spectral type G/K [2]
Apparent magnitude  (J)12.111±0.027 [3]
Apparent magnitude  (H)11.673±0.023 [3]
Apparent magnitude  (K)11.591±0.019 [3]
Astrometry
Proper motion (μ)RA: 9.198(14)  mas/yr [1]
Dec.: 30.739(13)  mas/yr [1]
Parallax (π)2.7654 ± 0.0115  mas [1]
Distance 1,179 ± 5  ly
(362 ± 2  pc)
Details [4] [5] [2]
Mass 0.901±0.029  M
Radius 0.851+0.014
0.013
  R
Surface gravity (log g)4.517±0.012  cgs
Temperature 5171±36  K
Metallicity [Fe/H]0.20±0.8  dex
Rotational velocity (v sin i)3.80±0.36 km/s
Age 7.38±1.87  Gyr
Other designations
Gaia DR2  2188601779406152448, GSC  03949-00967, 2MASS J20205324+5926556, TrES-5 parent star [6]
Database references
SIMBAD data

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. [4]

Contents

Planetary system

TrES-5b

In 2011 a transiting hot Jupiter planet TrES-5b was detected. [4] The host star was one of the faintest stars to which a planetary companion was detected by the transit method at the time of discovery. [2] The planet’s equilibrium temperature is 1480±24  K . [5]

TrES-5c/TrES-5B

An additional planet on a 4-day orbit in the system was suspected since 2018, [7] but refuted in 2021. Another object on a wide orbit, either star or planet, is still suspected. [8]

The GSC 03949-00967 planetary system [7]
Companion
(in order from star)
Mass Semimajor axis
(AU)
Orbital period
(days)
Eccentricity Inclination Radius
b 1.784±0.066  MJ 0.02447±0.000211.482247063±0.00000050.017±0.01284.529±0.005° 1.209±0.021  RJ

Related Research Articles

GSC 03089-00929 is a magnitude 12 star located approximately 757 light-years away in the constellation of Hercules. This star is a G type main sequence star that is similar to but slightly cooler than the Sun. This star is identified in SIMBAD as a variable star per the 1SWASP survey.

HAT-P-3, is a metal-rich K5 dwarf star located about 441 light-years away in the constellation Ursa Major. At a magnitude of about 11.5 it is not visible to the naked eye but is visible in a small to medium-sized amateur telescope. It is believed to be a relatively young star and has a slightly enhanced level of chromospheric activity.

WASP-48b is an extrasolar planet orbiting the star WASP-48 in the constellation Cygnus. The planet was detected using the transit method by the SuperWASP team, which published its discovery in 2011. It orbits its host star in just 2.14 days with a semi-major axis of 0.034 AU and has an equilibrium temperature of 1956±54 K. The dayside temperature was measured to be around 2300 K in 2018.

<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-26 is a yellow main sequence star in the constellation of Cetus.

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

Qatar-1 is an orange main sequence star in the constellation of Draco.

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-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.

WASP-50 is a G-type main-sequence star about 594 light-years away. The star is older than the Sun and slightly depleted in heavy elements compared to the Sun, and has a close to average starspot activity. Despite its advanced age, the star is rotating rapidly, being spun up by the tides raised by giant planet on close orbit.

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.

WASP-46 is a G-type main-sequence star about 1,210 light-years away. The star is older than the Sun and is strongly depleted in heavy elements compared to the Sun, having just 45% of the solar abundance. Despite its advanced age, the star is rotating rapidly, being spun up by the tides raised by a giant planet on a close orbit.

WASP-45 is a K-type main-sequence star about 701 light-years away. The star's age cannot be well constrained, but it is probably older than the Sun. Yet, WASP-45 is enriched in heavy elements compared to the Sun, having 240% of the solar abundance.

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.

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.

WASP-67 is a K-type main-sequence star about 620 light-years away. The stars age is poorly constrained, but is likely older than the Sun`s at approximately 8.7+5.5
−8.6
billion years. WASP-67 is slightly depleted in heavy elements, having 85% of the solar abundance of iron.

WASP-55 is a G-type main-sequence star about 980 light-years away. The star is much younger than the Sun at approximately 1.1+0.8
−0.6
 billion years
. WASP-55 is similar to the Sun in concentration of heavy elements.

WASP-42 is a K-type main-sequence star. Its surface temperature is 5315±79 K. WASP-42 is similar to the Sun in concentration of heavy elements, with metallicity ([Fe/H]) of 0.05±0.13, and is much older than the Sun at 11.3+1.5
−4.8
billion years. The star does exhibit starspot activity as is typical for its spectral class.

WASP-41 is a G-type main-sequence star. Its surface temperature is 5450±150 K. WASP-41 is similar to the Sun in its concentration of heavy elements, with a metallicity Fe/H index of −0.080±0.090, but is much younger at an age of 2.289±0.077 billion years. The star does exhibit strong starspot activity, with spots covering 3% of the stellar surface.

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 Maciejewski, G.; Dimitrov, D.; Mancini, L.; Southworth, J.; Ciceri, S.; D'Ago, G.; Bruni, I.; Raetz, St.; Nowak, G.; Ohlert, J.; Puchalski, D.; Saral, G.; Derman, E.; Petrucci, R.; Jofre, E.; Seeliger, M.; Henning, T. (2016), "New Transit Observations for HAT-P-30 b, HAT-P-37 b, TrES-5 b, WASP-28 b, WASP-36 b and WASP-39 b", Acta Astronomica, 66 (1): 55, arXiv: 1603.03268 , Bibcode:2016AcA....66...55M
  3. 1 2 3 Skrutskie, Michael F.; et al. (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 . Vizier catalog entry
  4. 1 2 3 Mandushev, Georgi; Quinn, Samuel N.; Buchhave, Lars A.; Dunham, Edward W.; Rabus, Markus; Oetiker, Brian; Latham, David W.; Charbonneau, David; Brown, Timothy M.; Belmonte, Juan A.; O'Donovan, Francis T. (2011), "TrES-5: A Massive Jupiter-sized Planet Transiting A Cool G-dwarf", The Astrophysical Journal, 741 (2): 114, arXiv: 1108.3572 , Bibcode:2011ApJ...741..114M, doi:10.1088/0004-637X/741/2/114, S2CID   118671116
  5. 1 2 Mislis, D.; Mancini, L.; Tregloan-Reed, J.; Ciceri, S.; Southworth, J.; d'Ago, G.; Bruni, I.; Baştürk, Ö.; Alsubai, K. A.; Bachelet, E.; Bramich, D. M.; Henning, Th.; Hinse, T. C.; Iannella, A. L.; Parley, N.; Schroeder, T. (2015), "High-precision multiband time series photometry of exoplanets Qatar-1b and TrES-5b", Monthly Notices of the Royal Astronomical Society, 448 (3): 2617–2623, arXiv: 1503.02246 , Bibcode:2015MNRAS.448.2617M, doi: 10.1093/mnras/stv197 , S2CID   53561305
  6. "GSC 03949-00967". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2022-01-06.
  7. 1 2 Sokov, Eugene N.; Sokova, Iraida A.; Dyachenko, Vladimir V.; Rastegaev, Denis A.; Burdanov, Artem; Rusov, Sergey A.; Benni, Paul; Shadick, Stan; Hentunen, Veli-Pekka; Salisbury, Mark; Esseiva, Nicolas; Garlitz, Joe; Bretton, Marc; Ogmen, Yenal; Karavaev, Yuri; Ayiomamitis, Anthony; Mazurenko, Oleg; Alonso, David; Velichko, Sergey F. (2018), "Transit timing analysis of the exoplanet TrES-5 b. Possible existence of the exoplanet TrES-5 c", Monthly Notices of the Royal Astronomical Society, 480 (1): 291–301, arXiv: 1806.03503 , Bibcode:2018MNRAS.480..291S, doi: 10.1093/mnras/sty1615 , S2CID   53665645
  8. Maciejewski, G.; et al. (December 2021). "Revisiting TrES-5 b: departure from a linear ephemeris instead of short-period transit timing variation". Astronomy & Astrophysics. 656. A88. arXiv: 2110.14294 . Bibcode: 2021A&A...656A..88M . doi: 10.1051/0004-6361/202142424 .