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HD 109749 is a binary star about 206 light years away in the constellation of Centaurus.

HD 109749
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Centaurus
Right ascension 12h 37m 16.3786s[1]
Declination −40° 48′ 43.6244″[1]
Apparent magnitude (V) 8.1
Characteristics
Spectral type G3IV+K
Astrometry
Proper motion (μ) RA: −157.374±0.092[1] mas/yr
Dec.: −6.481±0.120[1] mas/yr
Parallax (π)15.8240 ± 0.0736 mas[1]
Distance206.1 ± 1.0 ly
(63.2 ± 0.3 pc)
Details[2]
HD 109749 A
Mass1.1 M☉
Radius1.21 R☉
Luminosity1.55 L☉
Temperature5860 K
Age4.1 Gyr
HD 109749 B
Mass0.78 M☉
Other designations
CD−40 7393, Gaia DR2 6147000074988843264, HIP 61595, SAO 223556, 2MASS J12371639-4048435[3]
Database references
SIMBADdata

Stellar system


The primary star, HD 109749 A, is a G-type subgiant with a spectral type of G3IV,[4] indicating it is an evolved star with a luminosity higher than that of a main sequence star. It has a mass of 1.14 M☉ and a radius of 1.21 R☉. The star is shining with a luminosity of 1.55 L☉ and has an effective temperature of 5,860 K. Evolutionary models estimate an age of 4.1 billion years.[5] HD 109749 A is chromospherically inactive and has a high metallicity, with an iron abundance 178% of Sun's.[4]

The secondary star, HD 109749 B, is a K-type main sequence star with an apparent magnitude of 10.3.[6] It has a mass of about 0.78 M☉ and is located at a separation of 8.4 arcseconds, which corresponds to a projected separation of 490 AU.[2] This star has the same proper motion as the primary and seems to be at the same distance, confirming they form a physical binary system.[7]


Planetary system


In 2005, an exoplanet was discovered around HD 109749 A. It was detected by the radial velocity method as part of the N2K Consortium. It is a hot Jupiter with a minimum mass of 0.28 MJ and a semimajor axis of 0.06 AU.[4]

The HD 109749 planetary system[8]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b ≥0.27±0.045 MJ 0.0615±0.004 5.239891±0.000099 0 (fixed) — —

See also



References


  1. Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. Quarles, Billy; Li, Gongjie; Kostov, Veselin; Haghighipour, Nader (2020), "Orbital Stability of Circumstellar Planets in Binary Systems", The Astronomical Journal, 159 (3): 80, arXiv:1912.11019, Bibcode:2020AJ....159...80Q, doi:10.3847/1538-3881/ab64fa, S2CID 209444271
  3. "HD 109749". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-12-19.
  4. Fischer, Debra A.; et al. (2006). "The N2K Consortium. III. Short-Period Planets Orbiting HD 149143 and HD 109749". The Astrophysical Journal. 637 (2): 1094–1101. Bibcode:2006ApJ...637.1094F. doi:10.1086/498557.
  5. Bonfanti, A.; Ortolani, S.; Nascimbeni, V. (2016). "Age consistency between exoplanet hosts and field stars". Astronomy and Astrophysics. 585. A5. arXiv:1511.01744. Bibcode:2016A&A...585A...5B. doi:10.1051/0004-6361/201527297. S2CID 53971692.
  6. "HD 109749B -- High proper-motion Star". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2018-01-20.
  7. Desidera, S.; Barbieri, M. (January 2007). "Properties of planets in binary systems. The role of binary separation". Astronomy and Astrophysics. 462 (1): 345–353. arXiv:astro-ph/0610623. Bibcode:2007A&A...462..345D. doi:10.1051/0004-6361:20066319. S2CID 13813761.
  8. Ment, Kristo; et al. (2018). "Radial Velocities from the N2K Project: Six New Cold Gas Giant Planets Orbiting HD 55696, HD 98736, HD 148164, HD 203473, and HD 211810". The Astronomical Journal. 156 (5). 213. arXiv:1809.01228. Bibcode:2018AJ....156..213M. doi:10.3847/1538-3881/aae1f5. S2CID 119243619.


На других языках

[de] HD 109749

HD 109749 ist ein ca. 184 Lichtjahre von der Erde entfernter Unterriese im Sternbild Centaurus. Er besitzt eine scheinbare Helligkeit von 8,1 mag. Im Jahre 2005 entdeckten Fischer et al. mithilfe der Radialgeschwindigkeitsmethode einen extrasolaren Planeten, der diesen Stern umkreist und der die systematische Bezeichnung HD 109749 b erhielt. Die Umlaufperiode des Begleiters beträgt 5,24 Tage und seine Mindestmasse 0,3 Jupitermassen; die grosse Halbachse seiner Umlaufbahn wird auf 0,06 Astronomischen Einheiten geschätzt.
- [en] HD 109749

[ru] HD 109749

HD 109749 — жёлтый субгигант, находящийся на расстоянии 192 световых года от Земли в созвездии Центавра. Имеет массу 1,2 солнечной и эффективную температуру в 5610 кельвинов. В 2005 году Дебра Фишер обнаружила на орбите экзопланету.


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