HD 73526

Last updated
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  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
CD−40°4454, HD  73526, HIP  42282, SAO  220191 [7]
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]

Contents

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

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]

The HD 73526 planetary system [10]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b ≥2.25±0.12  MJ 0.65±0.01188.9±0.10.29±0.03——
c ≥2.25±0.13  MJ 1.03±0.02379.1±0.50.28±0.05——

See also

References

  1. 1 2 3 4 5 6 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.
  2. 1 2 3 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.
  3. 1 2 3 4 5 6 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 .
  4. 1 2 3 4 5 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.
  5. 1 2 3 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 .
  6. ↑ 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.
  7. ↑ "HD 73526". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2019-09-27.
  8. ↑ Tinney, Chris (2007-09-07). "AAPS Discovered Planets". Anglo-Australian Planet Search. University of New South Wales. Retrieved 2018-04-17.
  9. ↑ 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 .
  10. 1 2 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 .
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