Astronomy:HD 150706
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Ursa Minor[1] |
| Right ascension | 16h 31m 17.583s[2] |
| Declination | +79° 47′ 23.20″[2] |
| Apparent magnitude (V) | 7.016[3] |
| Characteristics | |
| Evolutionary stage | main sequence |
| Spectral type | G0V[4] |
| B−V color index | 0.607±0.005[1] |
| Astrometry | |
| Radial velocity (Rv) | −17.208±0.0009[5] km/s |
| Proper motion (μ) | RA: 94.947[2] mas/yr Dec.: −86.853[2] mas/yr |
| Parallax (π) | 35.4827 ± 0.0135[2] mas |
| Distance | 91.92 ± 0.03 ly (28.18 ± 0.01 pc) |
| Absolute magnitude (MV) | 4.76[1] |
| Details | |
| Mass | 1.04+0.01−0.04[6] M☉ |
| Radius | 0.96±0.02[4] R☉ |
| Luminosity | 1.18[1] L☉ |
| Surface gravity (log g) | 4.47±0.03[6] cgs |
| Temperature | 5,921±50[6] K |
| Metallicity [Fe/H] | −0.07±0.04[6] dex |
| Rotation | ≈5.6 days[4] |
| Rotational velocity (v sin i) | 3.7±1.0[4] km/s |
| Age | 1.59+3.03−0.17[6] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 150706 is a star with an orbiting exoplanet in the northern constellation of Ursa Minor. It is located 92 light years away from the Sun, based on parallax measurements. At that distance, it is not visible to the unaided eye. However, with an apparent visual magnitude of 7.02,[3] it is an easy target for binoculars. It is located only about 10° from the northern celestial pole so it is always visible in the northern hemisphere except for near the equator. Likewise, it is never visible in most of the southern hemisphere. The star is drifting closer to the Sun with a radial velocity of −17.2 km/s.[5]
The Sun-like spectrum of HD 150706 presents as a G-type main-sequence star with a stellar classification of G0V.[4] It has a similar mass, radius, and metallicity as the Sun.[4] The star is radiating 1.18[1] times the luminosity of the Sun from its photosphere at an effective temperature of 5,921 K.[6] It displays magnetic activity in its chromosphere in the form of star spots. Age estimates are poorly bounded, ranging from 1.16 up to 5.1 billion years.[4]
Based on an infrared excess, a dusty debris disk is orbiting the star. There is a hole in the center of this disk with a radius of ~20 astronomical unit|AU. It may be kept free of dust by a planetary system.[8]
Exoplanet
The existence of an exoplanet orbiting this star was announced at the Scientific Frontiers in Research on Extrasolar Planets conference in 2002.[9] The claimed planet had a minimum mass equal to the mass of Jupiter and was thought to be located in an elliptical orbit with a period of 264 days. However independent measurements of the star failed to confirm the existence of this planet.[10]
A different planet was discovered in the system in 2012; this Jupiter-twin completes one orbit in roughly 16 years. Its eccentricity and orbit is very poorly constrained.[4] In 2023, the inclination and true mass of HD 150706 b were determined via astrometry, and its orbit was revised, finding a substantially wider but still poorly constrained orbit with a period of about 36 years.[11]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (years) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 2.43+0.48 −0.38 MJ |
11.5+5.0 −2.4 |
36.0+26.0 −11.0 |
0.787+0.076 −0.083 |
70+14 −17 or 110+17 −14° |
— |
See also
- HD 149143
- List of extrasolar planets
References
- ↑ 1.0 1.1 1.2 1.3 1.4 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A.
- ↑ 2.0 2.1 2.2 2.3 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 3.0 3.1 Høg, E. et al. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics 355: L27. Bibcode: 2000A&A...355L..27H.
- ↑ 4.0 4.1 4.2 4.3 4.4 4.5 4.6 4.7 Boisse, Isabelle et al. (2012). "The SOPHIE search for northern extrasolar planets V. Follow-up of ELODIE candidates: Jupiter-analogs around Sun-like stars". Astronomy and Astrophysics 545: A55. doi:10.1051/0004-6361/201118419. Bibcode: 2012A&A...545A..55B.
- ↑ 5.0 5.1 Soubiran, C. et al. (2018). "Gaia Data Release 2. The catalogue of radial velocity standard stars". Astronomy and Astrophysics 616: A7. doi:10.1051/0004-6361/201832795. Bibcode: 2018A&A...616A...7S.
- ↑ 6.0 6.1 6.2 6.3 6.4 6.5 Aguilera-Gómez, Claudia et al. (2018). "Lithium abundance patterns of late-F stars: An in-depth analysis of the lithium desert". Astronomy and Astrophysics 614: A55. doi:10.1051/0004-6361/201732209. Bibcode: 2018A&A...614A..55A.
- ↑ "HD 150706". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+150706.
- ↑ Meyer, M. R. et al. (September 2004). "The Formation and Evolution of Planetary Systems: First Results from a Spitzer Legacy Science Program". The Astrophysical Journal Supplement Series 154 (1): 422–427. doi:10.1086/423177. Bibcode: 2004ApJS..154..422M.
- ↑ Udry, S.; Mayor, M.; Queloz, D. (2003). "Extrasolar Planets: from Individual Detections to Statistical Properties". in Deming, Drake; Seager, Sara. San Francisco: ASP. pp. 17-26. ISBN 1-58381-141-9. Bibcode: 2003ASPC..294...17U.
- ↑ Wright, J. T. et al. (2007). "Four New Exoplanets and Hints of Additional Substellar Companions to Exoplanet Host Stars". The Astrophysical Journal 657 (1): 533–45. doi:10.1086/510553. Bibcode: 2007ApJ...657..533W.
- ↑ 11.0 11.1 Xiao, Guang-Yao et al. (May 2023). "The Masses of a Sample of Radial-Velocity Exoplanets with Astrometric Measurements". Research in Astronomy and Astrophysics 23 (5): 055022. doi:10.1088/1674-4527/accb7e. Bibcode: 2023RAA....23e5022X.
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