HD 11506 is a star in the equatorial constellation of Cetus. It has a yellow hue and can be viewed with a small telescope but is too faint to be visible to the naked eye, having an apparent visual magnitude of 7.51.[2] The distance to this object is 167 light-years based on parallax, but it is drifting closer to the Sun with a radial velocity of −7.5 km/s.[1] It has an absolute magnitude of 3.94.[2]
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Cetus |
| Right ascension | 01h 52m 50.53442s[1] |
| Declination | −19° 30′ 25.1082″[1] |
| Apparent magnitude (V) | 7.51[2] |
| Characteristics | |
| Spectral type | G0V[3] |
| B−V color index | 0.607±0.015[2] |
| Astrometry | |
| Radial velocity (Rv) | −7.53±0.13[1] km/s |
| Proper motion (μ) | RA: 22.039(22) mas/yr[1] Dec.: −97.904(16) mas/yr[1] |
| Parallax (π) | 19.5342 ± 0.0221 mas[1] |
| Distance | 167.0 ± 0.2 ly (51.19 ± 0.06 pc) |
| Absolute magnitude (MV) | 3.94[2] |
| Details[4] | |
| Mass | 1.22±0.02[5] M☉ |
| Radius | 1.06±0.01 R☉ |
| Luminosity | 1.17±0.01 L☉ |
| Surface gravity (log g) | 4.43±0.02 cgs |
| Temperature | 5,833±28 K |
| Metallicity [Fe/H] | +0.30±0.06[5] dex |
| Rotation | ~15 days[5] |
| Rotational velocity (v sin i) | 5.5±0.5[5] km/s |
| Age | 1.6±0.9 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
This object is an ordinary G-type main-sequence star with a stellar classification of G0V,[3] which indicates it is generating energy via hydrogen fusion at its core. It is around 1.6[4] billion years old and is spinning with a projected rotational velocity of 5 km/s.[7] The star has 112% of the mass of the Sun and 106% of the Sun's radius. The spectrum shows a higher than solar abundance of elements other than hydrogen and helium – what astronomers term the metallicity.[8] The star is radiating 117% of the Sun's luminosity from its photosphere at an effective temperature of 5,833 K.[4]
Planetary system
editThe superjovian planet HD 11506 b was discovered orbiting the star by the N2K Consortium in 2007 using the Doppler spectroscopy method.[3] In 2009, a second planet discovery was claimed based on Bayesian analysis of the original data.[9] However, in 2015 additional radial velocity measurements showed that the planetary parameters were significantly different than those determined by Bayesian analysis. An additional linear trend in the radial velocities indicated a stellar or planetary companion on a long term orbit.[8]
In 2022, the presence of a third planet was confirmed, and the mass and inclination of both planet b and the new planet d were measured via astrometry.[10] A 2024 study also confirmed HD 11506 d, but found a significantly wider orbit and greater mass than previously estimated. This object orbits with a 73-year period, and at about 13 times the mass of Jupiter, it is at the borderline of being a brown dwarf.[5]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| c | ≥0.40±0.02 MJ | 0.771±0.004 | 223.92±0.37 | 0.228±0.054 | — | — |
| b | 4.80±0.08 MJ | 2.885±0.016 | 1,617.7±1.9 | 0.379±0.009 | 113+23 −53[10]° |
— |
| d | 12.8+0.6 −0.5 MJ |
18.20+0.06 −0.09 |
26,517+256 −292 |
0.29+0.02 −0.03 |
90+6 −5° |
— |
References
edit- ^ a b c d e f 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.
- ^ a b c d e Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID 119257644.
- ^ a b c Fischer, Debra A.; et al. (2007). "Five Intermediate-Period Planets from the N2K Sample". The Astrophysical Journal. 669 (2): 1336–1344. arXiv:0704.1191. Bibcode:2007ApJ...669.1336F. doi:10.1086/521869. S2CID 7774321.
- ^ a b c Bonfanti, A.; et al. (2015). "Revising the ages of planet-hosting stars". Astronomy and Astrophysics. 575. A18. arXiv:1411.4302. Bibcode:2015A&A...575A..18B. doi:10.1051/0004-6361/201424951. S2CID 54555839.
- ^ a b c d e f Ruggieri, A.; Desidera, S.; et al. (September 2024). "The GAPS Programme at TNG: LVIII. Two multi-planet systems with long-period substellar companions around metal-rich stars". Astronomy & Astrophysics. 689: A235. Bibcode:2024A&A...689A.235R. doi:10.1051/0004-6361/202449456.
- ^ "HD 11506". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-11-10.
- ^ Delgado Mena, E.; et al. (April 2015). "Li abundances in F stars: planets, rotation, and Galactic evolution". Astronomy & Astrophysics. 576: 24. arXiv:1412.4618. Bibcode:2015A&A...576A..69D. doi:10.1051/0004-6361/201425433. S2CID 56051637. A69.
- ^ a b Giguere, Matthew J.; et al. (2015). "Newly Discovered Planets Orbiting HD 5319, HD 11506, HD 75784 and HD 10442 from the N2K Consortium". The Astrophysical Journal. 799 (1). 89. arXiv:1411.5374. Bibcode:2015ApJ...799...89G. doi:10.1088/0004-637X/799/1/89. S2CID 56121568.
- ^ Tuomi, M.; Kotiranta, S. (2009). "Bayesian analysis of the radial velocities of HD 11506 reveals another planetary companion". Astronomy and Astrophysics. 496 (2): L13–L16. arXiv:0902.2997. Bibcode:2009A&A...496L..13T. doi:10.1051/0004-6361/200811531. S2CID 16414890.
- ^ a b Feng, Fabo; Butler, R. Paul; et al. (August 2022). "3D Selection of 167 Substellar Companions to Nearby Stars". The Astrophysical Journal Supplement Series. 262 (21): 21. arXiv:2208.12720. Bibcode:2022ApJS..262...21F. doi:10.3847/1538-4365/ac7e57. S2CID 251864022.