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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 318 light years 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]

HD 73526
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Vela
Right ascension 08h 37m 16.4835s[1]
Declination −41° 19′ 08.7873″[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: −61.097[1] mas/yr
Dec.: 158.982[1] mas/yr
Parallax (π)10.2551 ± 0.0339 mas[1]
Distance318 ± 1 ly
(97.5 ± 0.3 pc)
Absolute magnitude (MV)+4.1±0.2[5]
Absolute bolometric
magnitude (Mbol)		+3.7±0.2[5]
Details[4]
Mass1.01±0.04
1.14±0.15[6] M☉
Radius1.53±0.03[6] R☉
Luminosity2.14+0.68
−0.52 L☉
Surface gravity (log g)4.13±0.06 cgs
Temperature5,564±16 K
Metallicity [Fe/H]+0.23±0.02 dex
Rotational velocity (v sin i)1.69±0.26 km/s
Age9.59±1.00 Gyr
Other designations
CD−40° 4454, HD 73526, HIP 42282, SAO 220191[7]
Database references
SIMBADdata

The stellar classification of HD 73526 is G6 V,[3] indicating this is a G-type main-sequence star that, like the Sun, it 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 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. This planet forms a 2:1 orbital resonance with planet b.[3] Although these are minimum masses as the inclinations of these planets are unknown, orbital stability analysis indicated that orbital inclinations of both planets are likely to be near 90°, making the minimum masses very close to the true masses of the planets.[9]

The HD 73526 planetary system[3]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b >2.07 ± 0.16 MJ 0.66 ± 0.05 187.5 ± 0.3 0.39 ± 0.05 — —
c >2.30 ± 0.17 MJ 1.05 ± 0.08 376.9 ± 0.9 0.40 ± 0.05 — —

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. 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. 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. 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. 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. 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.



На других языках

[de] HD 73526

HD 73526 ist ein Gelber Zwerg, der von mindestens zwei Planeten, HD 73526 b und HD 73526 c, umkreist wird. Der Stern besitzt die Spektralklasse G6V und die Leuchtkraftklasse V. Seine Masse liegt bei etwa 1,02 Sonnenmassen. Seine Begleiter wurden in den Jahren 2002 und 2006 durch Messungen seiner Radialgeschwindigkeit entdeckt.
- [en] HD 73526


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