GSC 03089-00929

Last updated
GSC 03089-00929 / Pipoltr
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Hercules
Right ascension 17h 52m 07.0184s [1]
Declination +37° 32′ 46.237″ [1]
Apparent magnitude  (V)12.4
Characteristics
Spectral type G
Apparent magnitude  (B)13.114 ±0.009 [2]
Apparent magnitude  (V)12.402 ±0.006 [2]
Apparent magnitude  (I)11.603000 ±0.010 [2]
Apparent magnitude  (J)11.015 ±0.022 [2]
Apparent magnitude  (H)10.655000 ±0.030 [2]
Apparent magnitude  (K)10.608000 ±0.028 [2]
Variable type planetary transits [2] [3]
Astrometry
Proper motion (μ)RA: −24.462(10)  mas/yr [1]
Dec.: 34.772(11)  mas/yr [1]
Parallax (π)4.3106 ± 0.0091  mas [1]
Distance 757 ± 2  ly
(232.0 ± 0.5  pc)
Absolute magnitude  (MV)5.39±0.11 [4]
Details
Mass 0.928+0.028
−0.048 [4]   M☉
Radius 0.826±0.012 [5]   R☉
Luminosity 0.625+0.066
−0.058 [4]   L☉
Surface gravity (log g)4.57±0.01 [5]   cgs
Temperature 5650±75 [4]   K
Metallicity [Fe/H]−0.19±0.08 [4]   dex
Rotational velocity (v sin i)1.5±1.0 km/s
Age 0.9+2.8
−0.8 [4]   Gyr
Other designations
TrES-3 Parent Star, 1SWASP J175207.01+373246.3, UCAC2 45017453, [2] V1434 Her
Database references
SIMBAD data

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. [2] This star is identified in SIMBAD as a variable star per the 1SWASP survey. [6]

Contents

The star GSC 03089-00929 is named Pipoltr. The name was selected in the NameExoWorlds campaign by Liechtenstein, during the 100th anniversary of the IAU. In the local dialect of Triesenberg, Pipoltr is a bright and visible butterfly. [7] [8]

Planetary system

In 2007 the TrES program found exoplanet TrES-3b, later named Umbäässa, orbiting this star by using the transit method. [9]

The transit timing variation analysis did not reveal any additional planets in the system as of 2020, [10] and the physical mechanism underlying transit timing variations remains unexplained as in 2022. [11]

The GSC 03089-00929 planetary system [12] [5] [4]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
TrES-3b / Umbäässa 1.910+0.075
−0.080  MJ 		0.02282+0.00023
−0.00040		1.30618652(4)0 (fixed)81.89±0.12 ° 1.381±0.033  RJ

See also

Related Research Articles

GSC 02652-01324 is an orange dwarf main sequence star approximately 521 light-years away in the constellation of Lyra.

<span class="mw-page-title-main">TrES-3b</span>

TrES-3b is an extrasolar planet orbiting the star GSC 03089-00929. It has an orbital period of just 31 hours and nearly twice the mass of Jupiter.

<span class="mw-page-title-main">WASP-1</span> Star in the constellation Andromeda

WASP-1 is a metal-rich magnitude 12 star located about 1,300 light-years away in the Andromeda constellation.

HD 118203 is a star with an orbiting exoplanet located in the northern circumpolar constellation of Ursa Major. It has the proper name Liesma, which means flame, and it is the name of a character from the Latvian poem Staburags un Liesma. The name was selected in the NameExoWorlds campaign by Latvia, during the 100th anniversary of the IAU.

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.

Lupus-TR-3 is a star located in the southern constellation Lupus. It has an apparent magnitude of 17.4, making it visible only in power telescopes. Its distance is not well known, but it is estimated to be roughly 2,000 parsecs away from the Solar System.

XO-3 is a star in the constellation Camelopardalis. The star has a magnitude of 10 and is not visible to the naked eye but is visible through a small telescope. A search for a binary companion star using adaptive optics at the MMT Observatory was negative.

<span class="mw-page-title-main">GSC 03549-02811</span> Main sequence star in the constellation Draco

GSC 03549-02811 is a yellow main-sequence star similar to the Sun. This star is located approximately 704 light-years away in the constellation of Draco. The apparent magnitude of this star is 11.41, 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 5 billion years.

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.

XO-4 is a star located approximately 863 light-years away from Earth in the Lynx constellation. It has a magnitude of about 11 and cannot be seen with the naked eye but is visible through a small telescope. A search for a binary companion star using adaptive optics at MMT Observatory was negative.

HAT-P-12 is a magnitude 13 low-metallicity K dwarf star approximately 463 light years away in the constellation Canes Venatici, which hosts one known exoplanet.

WASP-17 is an F-type main sequence star approximately 1,300 light-years away in the constellation Scorpius.

<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.

HD 146389, is a star with a yellow-white hue in the northern constellation of Hercules. The star was given the formal name Irena by the International Astronomical Union in January 2020. It is invisible to the naked eye with an apparent visual magnitude of 9.4 The star is located at a distance of approximately 446 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −9 km/s. The star is known to host one exoplanet, designated WASP-38b or formally named 'Iztok'.

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

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.

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.

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.

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.

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 4 5 6 7 8 9 "NAME TrES-3 Parent Star". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2009-04-23.
  3. ↑ Lister, T. A.; West, R. G.; Wilson, D. M.; Collier Cameron, A.; Clarkson, W. I.; Street, R. A.; Enoch, B.; Parley, N. R.; et al. (June 30, 2007). "SuperWASP-North extrasolar planet candidates: candidates from fields 17h<RA<18h" (PDF). Monthly Notices of the Royal Astronomical Society. 379 (2): 647–662. arXiv: 0705.2603 . Bibcode:2007MNRAS.379..647L. doi:10.1111/j.1365-2966.2007.11948.x. S2CID   14333676.
  4. 1 2 3 4 5 6 7 Sozzetti, Alessandro; et al. (2009). "A New Spectroscopic and Photometric Analysis of the Transiting Planet Systems TrES-3 and TrES-4". The Astrophysical Journal. 691 (2): 1145–1158. arXiv: 0809.4589 . Bibcode:2009ApJ...691.1145S. doi:10.1088/0004-637X/691/2/1145. S2CID   3741198.
  5. 1 2 3 Püsküllü, Ç.; et al. (2017). "Photometric investigation of hot exoplanets: TrES-3b and Qatar-1b". New Astronomy. 55: 39–47. arXiv: 1704.03697 . Bibcode:2017NewA...55...39P. doi:10.1016/j.newast.2017.04.001. S2CID   119208251.
  6. ↑ "Objects in reference 2007MNRAS.379..647L". Centre de Données astronomiques de Strasbourg . Retrieved 2009-05-03.
  7. ↑ "Approved names". NameExoworlds. Archived from the original on 2019-12-19. Retrieved 2020-01-02.
  8. ↑ "International Astronomical Union | IAU". www.iau.org. Retrieved 2020-01-02.
  9. ↑ O'Donovan, Francis T.; Charbonneau, David; Bakos, Gáspár Á.; Mandushev, Georgi; Dunham, Edward W.; Brown, Timothy M.; Latham, David W.; Torres, Guillermo; et al. (July 1, 2007). "TrES-3: A Nearby, Massive, Transiting Hot Jupiter in a 31-Hour Orbit". Astrophysical Journal Letters. 663 (1): L37–L40. arXiv: 0705.2004 . Bibcode:2007ApJ...663L..37O. doi:10.1086/519793. S2CID   17637874.
  10. ↑ Mannaday, Vineet Kumar; Thakur, Parijat; Jiang, Ing-Guey; Sahu, D. K.; Joshi, Y. C.; Pandey, A. K.; Joshi, Santosh; Yadav, Ram Kesh; Su, Li-Hsin; Sariya, Devesh P.; Yeh, Li-Chin; Griv, Evgeny; Mkrtichian, David; Shlyapnikov, Aleksey; Moskvin, Vasilii; Ignatov, Vladimir; Vaňko, M.; Püsküllü, Ç. (2020). "Probing Transit Timing Variation and Its Possible Origin with 12 New Transits of TrES-3b". The Astronomical Journal. 160 (1): 47. arXiv: 2006.00599 . Bibcode:2020AJ....160...47M. doi: 10.3847/1538-3881/ab9818 . S2CID   219176648.
  11. ↑ Mannaday, Vineet Kumar; Thakur, Parijat; Southworth, John; Jiang, Ing-Guey; Sahu, D. K.; Mancini, L.; Vaňko, M.; Kundra, Emil; Gajdoš, Pavol; a-Thano, Napaporn; Sariya, Devesh P.; Yeh, Li-Chin; Griv, Evgeny; Mkrtichian, David; Shlyapnikov, Aleksey (2022), "Revisiting the Transit Timing Variations in the TrES-3 and Qatar-1 Systems with TESS Data", The Astronomical Journal, 164 (5): 198, arXiv: 2209.04080 , Bibcode:2022AJ....164..198M, doi: 10.3847/1538-3881/ac91c2 , S2CID   252185524
  12. ↑ MacKebrandt, F.; et al. (2017). "Transmission spectroscopy of the hot Jupiter TrES-3 b: Disproof of an overly large Rayleigh-like feature". Astronomy and Astrophysics. 608. A26. arXiv: 1709.06124 . Bibcode:2017A&A...608A..26M. doi:10.1051/0004-6361/201730512. S2CID   53995250.


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