HD 73526
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Vela |
| Right ascension | 08h 37m 16.48335s[1] |
| Declination | −41° 19′ 08.7904″[1] |
| Apparent magnitude (V) | +8.99[2] |
| Characteristics | |
| Evolutionary stage | Main sequence[3] |
| Spectral type | G6 V[3] |
| B−V color index | 0.737±0.005[2] |
| Variable type | Constant[3] |
| Astrometry | |
| Radial velocity (Rv) | +26.31±0.10[4] km/s |
| Proper motion (μ) | RA: −60.993 mas/yr [1] Dec.: 159.192 mas/yr [1] |
| Parallax (π) | 10.3311 ± 0.0144 mas [1] |
| Distance | 315.7 ± 0.4 ly (96.8 ± 0.1 pc) |
| Absolute magnitude (MV) | +4.1±0.2[5] |
| Absolute bolometric magnitude (Mbol) | +3.7±0.2[5] |
| Details[4] | |
| Mass | 1.01±0.04 1.14±0.15[6] M☉ |
| Radius | 1.53±0.03[6] R☉ |
| Luminosity | 2.14+0.68 −0.52 L☉ |
| Surface gravity (log g) | 4.13±0.06 cgs |
| Temperature | 5,564±16 K |
| Metallicity [Fe/H] | +0.23±0.02 dex |
| Rotational velocity (v sin i) | 1.69±0.26 km/s |
| Age | 9.59±1.00 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 73526 is a star in the southern constellation of Vela. With an apparent visual magnitude of +8.99,[2] it is much too faint to be viewed with the naked eye. The star is located at a distance of approximately 316 light-years (97 parsecs) from the Sun based on parallax,[1] and is drifting further away with a radial velocity of +26 km/s.[4] It is a member of the thin disk population.[4]
The stellar classification of HD 73526 is G6 V,[3] indicating this is a G-type main-sequence star that, like the Sun, is generating energy through core hydrogen fusion. Based on its properties, it may be starting to evolve off the main sequence.[3] This star has slightly more mass than the Sun and a 53% greater radius. The abundance of iron in its atmosphere suggests the star's metallicity – what astronomers term the abundance of elements with higher atomic number than helium – is 70% greater than in the Sun. It is a much older star with an estimated age of nearly ten billion years, and is spinning slowly with a projected rotational velocity of 1.7 km/s. The star is radiating more than double the luminosity of the Sun from its photosphere at an effective temperature of 5,564 K.[4]
Planetary system
[edit ]On June 13 2002,[8] a 2.1 MJ planet HD 73526 b was announced orbiting HD 73526 in an orbit just a little smaller than that of Venus' orbit around the Sun.[5] This planet receives an insolation 3.65 times that of Earth or 1.89 times that of Venus. This was a single planet system until 2006 when a 2.3 MJ second planet HD 73526 c was discovered. These planets forms a 2:1 orbital resonance with planet b.[3] In fact, they seem to be in a very deep resonance with very long timescale stability due to an ACR (Apsidal Corotation Resonance) the planets seem to satisfy.[9] Although these are minimum masses as the inclinations of these planets are unknown, orbital stability analysis indicates that the orbital inclinations of both planets are likely to be near 90°, making the minimum masses very close to the true masses of the planets.[10]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥2.25±0.12 MJ | 0.65±0.01 | 188.9±0.1 | 0.29±0.03 | — | — |
| c | ≥2.25±0.13 MJ | 1.03±0.02 | 379.1±0.5 | 0.28±0.05 | — | — |
See also
[edit ]References
[edit ]- ^ a b c d e 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 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 d e f Tinney, C. G.; et al. (2006). "The 2 : 1 Resonant Exoplanetary System Orbiting HD 73526". The Astrophysical Journal. 647 (1): 594–599. arXiv:astro-ph/0602557 . Bibcode:2006ApJ...647..594T . doi:10.1086/503706 .
- ^ a b c d e Jofré, E.; et al. (2015). "Stellar parameters and chemical abundances of 223 evolved stars with and without planets". Astronomy & Astrophysics. 574. A50. arXiv:1410.6422 . Bibcode:2015A&A...574A..50J. doi:10.1051/0004-6361/201424474. S2CID 53666931.
- ^ a b c Tinney, C. G.; et al. (2003). "Four New Planets Orbiting Metal-enriched Stars". The Astrophysical Journal. 587 (1): 423–428. arXiv:astro-ph/0207128 . Bibcode:2003ApJ...587..423T . doi:10.1086/368068 .
- ^ a b Stassun, Keivan G.; et al. (March 2017). "Accurate Empirical Radii and Masses of Planets and Their Host Stars with Gaia Parallaxes". The Astronomical Journal. 153 (3): 20. arXiv:1609.04389 . Bibcode:2017AJ....153..136S. doi:10.3847/1538-3881/aa5df3 . S2CID 119219062. 136.
- ^ "HD 73526". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2019年09月27日.
- ^ Tinney, Chris (2007年09月07日). "AAPS Discovered Planets". Anglo-Australian Planet Search. University of New South Wales. Retrieved 2018年04月17日.
- ^ Pons, J.; Gallardo, T. (May 2024). "Secular evolution of resonant planets in the coplanar case. Application to the systems HD 73526 and HD 31527". Astronomy & Astrophysics. 685: A105. Bibcode:2024A&A...685A.105P. doi:10.1051/0004-6361/202348378 . (Keywords – methods: numerical, celestial mechanics, planets and satellites: dynamical evolution and stability)
- ^ a b Wittenmyer, Robert A.; et al. (2014). "A Detailed Analysis of the HD 73526 2:1 Resonant Planetary System". The Astrophysical Journal. 780 (2). 140. arXiv:1311.6559 . Bibcode:2014ApJ...780..140W . doi:10.1088/0004-637X/780/2/140 .
External links
[edit ]- "HD 73526". Extrasolar Planets Encyclopaedia . Archived from the original on November 6, 2007.
- Extrasolar Planet Interactions Archived 2016年05月05日 at the Wayback Machine by Rory Barnes & Richard Greenberg, Lunar and Planetary Lab, University of Arizona