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
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
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. 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 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. [9]

The HD 73526 planetary system [9]
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

Related Research Articles

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<span class="mw-page-title-main">HD 136118</span> Star in the constellation Serpens

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HD 4113 is a dual star system in the southern constellation of Sculptor. It is too faint to be viewed with the naked eye, having an apparent visual magnitude of 7.88. The distance to this star, as estimated by parallax measurements, is 137 light years. It is receding away from the Sun with a radial velocity of +5 km/s.

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HD 73526 c is an extrasolar planet orbiting about 97 million miles away from its parent star. Based on its mass, this planet is likely to be a gas giant. At the distance this planet orbits from its star, which is more luminous than the Sun, HD 73526 c would receive insolation 84% that of Venus.

HD 30562 is a star in the equatorial constellation of Eridanus. It has a golden hue and can be viewed with the naked eye under good seeing conditions, having an apparent visual magnitude of 5.77. The distance to this star is 85 light years based on parallax. It is drifting further away with a high radial velocity of +77 km/s, having come to within 46.8 light-years some 236,000 years ago.

HD 129445 is a G-type star found in the Circinus constellation located 219 light-years away from the Sun based on parallax. It is invisible to the naked eye with an apparent visual magnitude of 8.80. The star was observed by the Magellan Planet Search Program due to its absolute visual magnitude and high metallicity. The Magellan program conducted 17 doppler velocity measurements, which spans a full orbital period. The results led the program to detect a planet dubbed HD 129445 b. In 2023, the inclination and true mass of HD 129445 b were determined via astrometry.

HD 175167 is a star with an exoplanet companion in the southern constellation of Pavo. It is too faint to be visible with the naked eye at an apparent visual magnitude of 8.01. The system is located at a distance of 232 light-years from the Sun based on parallax measurements, and it is drifting further away with a radial velocity of 5 km/s. It shows a high proper motion, traversing the celestial sphere at an angular rate of 0.190 arcsec yr−1.

HD 38283, or Bubup, is a star in the southern circumpolar constellation Mensa. With an magnitude of 6.70, its invisible to the naked eye but can be seen with binoculars. Bubup is located relatively close at a distance of 124 light-years but is recceding with a heliocentric radial velocity of 61.4 km/s.

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. 1 2 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. 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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