HD 188753

Last updated
HD 188753
Observation data
Epoch J2000.0        Equinox J2000.0
Constellation Cygnus
Right ascension 19h 54m 58.37177s [1]
Declination +41° 52′ 17.5298″ [1]
Apparent magnitude  (V)+7.43 [2]
Characteristics
Spectral type A: G8V [3]
U−B color index +0.42 [2]
B−V color index +0.79 [2]
Astrometry
Radial velocity (Rv)-23.5 [4]  km/s
Proper motion (μ)RA: -51.32 [1]   mas/yr
Dec.: 286.57 [1]   mas/yr
Parallax (π)21.63 ± 0.65 [1]   mas
Distance 151 ± 5  ly
(46 ± 1  pc)
Absolute magnitude  (MV)4.17[ citation needed ]
Orbit [5]
PrimaryHD 188753 A
CompanionHD 188753 BC
Period (P)25.63 yr
Semi-major axis (a)0.2587"
(11.8  au)
Eccentricity (e)0.502
Inclination (i)31.1°
Longitude of the node (Ω)45.7°
Periastron epoch (T)1988.1
Argument of periastron (ω)
(secondary)		233.3°
Semi-amplitude (K1)
(primary)		4.8 km/s
Semi-amplitude(K2)
(secondary)		3.4 km/s
Details
Mass A: 1.06 ± 0.07 [6]  M☉
B: 0.96 ± 0.05 [6]  M☉
C: 0.67 ± 0.05 [6]   M☉
Temperature A: 5,750 [3]   K
Other designations
BD+41 3535, HIP  98001, SAO  48968, ADS  13125, WDS J19550+4152 [7]
Database references
SIMBAD data

HD 188753 is a hierarchical triple star system approximately 151 light-years away in the constellation of Cygnus, the Swan. In 2005, an extrasolar planet was announced to be orbiting the primary star (designated HD 188753 A) in the system. Follow-up measurements by an independent group in 2007 did not confirm the planet's existence. [8]

Contents

Stellar components

The orbit of HD 188753 BC around A HD188753 orbit.jpg
The orbit of HD 188753 BC around A

The primary star, HD 188753 A, is similar to the Sun [9] with a mass only 6% larger and a stellar classification of G8V. [3] Orbiting this primary at a distance of 12.3  AU [10] is a pair of smaller stars that orbit each other with a period of 156.0 ± 0.1 days, a semi-major axis of 0.67 AU, and eccentricity of 0.1 ± 0.03. The pair have estimated masses of 0.96 and 0.67 solar masses. [10] They orbit the primary with a period of about 25.7 years and an orbital eccentricity of about 0.50. [10] The periastron distance of this orbit is 6.2 AU. [8]

Possible planet

Artist's impression of the sight from a (hypothetical) moon of HD 188753 Ab (upper left). The brightest companion is just below the horizon. Triple-star sunset.jpg
Artist's impression of the sight from a (hypothetical) moon of HD 188753 Ab (upper left). The brightest companion is just below the horizon.

In 2005 the discovery of a candidate planet orbiting the primary star of the triple star system was announced. This planet, which received the designation HD 188753 Ab, was announced by a Polish astronomer working in the United States, Dr. Maciej Konacki. [9] This would not be the first known planet in a triple star system – for example, the planet 16 Cygni Bb had been discovered earlier, orbiting one of the components of a wide triple system also in the constellation of Cygnus.

Since HD 188753 Ab was believed to be orbiting in a multi-star system, Konacki referred to planets of this type as "Tatooine planets" after Luke Skywalker's home world. [11] The detection of this planet has been challenged by Eggenberger et al. [8] [12]

The candidate planet, a hot Jupiter gas giant slightly more massive than Jupiter, was thought to orbit the star HD 188753 A once every 80 hours or so (3.3 days), at a distance of about 8 million kilometers, a twentieth of the distance between Earth and the Sun. The existence of HD 188753 Ab in a relatively close triple star system challenged the current models of planet formation. The current idea is that giant planets form in the outer reaches of their system (in orbits similar to those of Jupiter and Saturn). Once formed, some of these planets may migrate close to their stars, becoming hot Jupiters. The theoretical difficulty in understanding HD 188753 Ab is that any protoplanetary disk would have ended around 1 astronomical unit from the primary star (due to the presence of the secondary stars). A Jovian planet should not have been able to form so close to the primary, and with no disk material beyond 1 AU, a planet should not have been able to form beyond that distance to migrate inward. [13] One of the possibilities suggested that the planet formed before the secondary stars had reached their current configuration. This suggests that the two secondary stars were once more distant than they are now.

An attempt to confirm the discovery failed. In 2007, a team at the Geneva Observatory stated that they had the precision and sampling rate sufficient to have detected the would-be planet, and that they did not detect it. [8] Konacki responded to this, stating that the precision of the follow-up measurements was not sufficient to confirm or deny the planet's existence and that he planned to release an update in 2007. [12] As of August 2012, no update appears to have been published.

See also

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References

  1. 1 2 3 4 5 van Leeuwen, F. (November 2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv: 0708.1752 . Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID   18759600.
  2. 1 2 3 Nicolet, B. (October 1978). "Photoelectric photometric Catalogue of homogeneous measurements in the UBV System". Astronomy and Astrophysics Supplement Series. 34: 1–49. Bibcode:1978A&AS...34....1N.
  3. 1 2 3 Dodson-Robinson, Sarah E.; et al. (January 2011). "A Spitzer Infrared Spectrograph Study of Debris Disks Around Planet-host Stars". The Astronomical Journal. 141 (1): 11. arXiv: 1010.3292 . Bibcode:2011AJ....141...11D. doi:10.1088/0004-6256/141/1/11. S2CID   118645999.
  4. ↑ Evans, D. S. (June 20–24, 1966). "The Revision of the General Catalogue of Radial Velocities". In Batten, Alan Henry; Heard, John Frederick (eds.). Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30. University of Toronto: International Astronomical Union (published 1967). pp. 57–63. Bibcode:1967IAUS...30...57E.
  5. ↑ Marcadon, F.; Appourchaux, T.; Marques, J. P. (2018). "Asteroseismic and orbital analysis of the triple star system HD 188753 observed by Kepler". Astronomy and Astrophysics. 617: A2. arXiv: 1804.09296 . Bibcode:2018A&A...617A...2M. doi:10.1051/0004-6361/201731628. S2CID   56108054.
  6. 1 2 3 Pfahl, Eric (December 2005). "Cluster Origin of the Triple Star HD 188753 and Its Planet". The Astrophysical Journal. 635 (1): L89–L92. arXiv: astro-ph/0509490 . Bibcode:2005ApJ...635L..89P. doi:10.1086/499162. S2CID   15862182.
  7. ↑ "HD 188753 -- Spectroscopic binary". SIMBAD. Centre de Données astronomiques de Strasbourg . Retrieved 2011-12-15.
  8. 1 2 3 4 Eggenberger, A.; et al. (May 2007). "No evidence of a hot Jupiter around HD 188753 A". Astronomy and Astrophysics. 466 (3): 1179–1183. arXiv: astro-ph/0702574 . Bibcode:2007A&A...466.1179E. doi:10.1051/0004-6361:20066835. S2CID   15308737.
  9. 1 2 Peplow, Mark (July 13, 2005). "The triple sunset that should not exist". Nature. doi:10.1038/news050711-6 . Retrieved 2011-12-15.
  10. 1 2 3 Portegies Zwart, Simon F.; McMillan, Stephen L. W. (November 2005). "Planets in Triple Star Systems: The Case of HD 188753". The Astrophysical Journal. 633 (2): L141–L144. arXiv: astro-ph/0509767 . Bibcode:2005ApJ...633L.141P. doi:10.1086/498302. S2CID   17648565.
  11. ↑ Tindol, Robert (July 13, 2005). "First Planet Under Three Suns Is Discovered". Caltech Media Relations. Archived from the original on October 27, 2009. Retrieved 2011-12-16.
  12. 1 2 Konacki, Maciej (July 2007). "An extrasolar giant planet in a close triple-star system HD188753". Nature. 436 (7048): 230–233. Bibcode:2005Natur.436..230K. doi:10.1038/nature03856. PMID   16015323. S2CID   4396402.
  13. ↑ Hatzes AP; Wuchterl G (2005). "Astronomy: giant planet seeks nursery place". Nature . 436 (7048): 182–3. Bibcode:2005Natur.436..182H. doi: 10.1038/436182a . PMID   16015311.

Coordinates: Jupiter and moon.png 19h 54m 58.37s, +41° 52′ 17.5″

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