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] |
| Distance | 206.1 ± 1.0 ly (63.2 ± 0.3 pc) |
| Details[2] | |
| HD 109749 A | |
| Mass | 1.1 M☉ |
| Radius | 1.21 R☉ |
| Luminosity | 1.55 L☉ |
| Temperature | 5860 K |
| Age | 4.1 Gyr |
| HD 109749 B | |
| Mass | 0.78 M☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 109749 is a binary star about 206 light years away in the constellation of Centaurus.
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]
| 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
- ^ a b c d e 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.
- ^ a b 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, doi:10.3847/1538-3881/ab64fa, S2CID 209444271
{{citation}}: CS1 maint: unflagged free DOI (link) - ^ "HD 109749". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-12-19.
- ^ a b c 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.
- ^ 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.
- ^ "HD 109749B -- High proper-motion Star". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2018-01-20.
- ^ 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.
- ^ 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.
{{cite journal}}: CS1 maint: unflagged free DOI (link)
