Summary
HD 12661 is a G-type main sequence star in the northern constellation of Aries. The star is slightly larger and more massive than the Sun, with an estimated age of seven billion years. It has two known extrasolar planets.
 Planetary orbits of the HD 12661 system | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Aries |
| Right ascension | 02h 04m 34.2884s[1] |
| Declination | +25° 24′ 51.5142″[1] |
| Apparent magnitude (V) | 7.42[2] |
| Characteristics | |
| Spectral type | G6 V[3] |
| U−B color index | +0.33[2] |
| B−V color index | +0.71[2] |
| Astrometry | |
| Proper motion (μ) | RA: −108.181±0.089[1] mas/yr Dec.: −173.335±0.089[1] mas/yr |
| Parallax (π) | 26.3927 ± 0.0437 mas[1] |
| Distance | 123.6 ± 0.2 ly (37.89 ± 0.06 pc) |
| Absolute magnitude (MV) | 4.58[3] |
| Details | |
| Mass | 1.07[3]–1.10[4] M☉ |
| Radius | 1.096[3]–1.12[4] R☉ |
| Luminosity | 1.22[4] L☉ |
| Surface gravity (log g) | 4.43[3] cgs |
| Temperature | 5,754[3] K |
| Metallicity [Fe/H] | 0.29 ± 0.05[3] dex |
| Rotational velocity (v sin i) | 1.20[4] km/s |
| Age | 7.17[5] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Properties edit
The apparent visual magnitude of this star is 7.42,[2] making it too faint to be viewed by the naked eye even under ideal viewing conditions. However, it can be readily observed using a small telescope with an aperture of 6 cm (2 in) or more.[7] Parallax measurements of HD 12661 place it at a distance of about 123.6 light-years (37.9 parsecs) from the Earth, with a margin of error of ±0.2 light years.[1] It has a stellar classification of G6 V, indicating that it is a main sequence star that is generating energy through the thermonuclear fusion of hydrogen at its core. The effective temperature of the star's outer envelope is about 5,754 K,[3] giving it the characteristic yellow hue of a G-type star.[8] Based on stellar models, estimates of the radius of this star range from 107% to 112% times Sun's radius, while the mass is likely in the range from 107% to 110% of the Sun's mass.[3][4]
As a star ages it slows its rotation and diminishes the amount of magnetic activity in its chromosphere. Hence the measured emission from the chromosphere can be used to estimate the age of a star, particularly for F and G-type dwarf stars with an age of less than two billion years. However, this technique becomes less accurate for ages beyond about 5.6 billion years. Based upon the chromosphere emission of HD 12661, it is older than the Sun with an estimated age of roughly seven billion years.[9] It has a low projected rotational velocity of 1.20 km/s, consistent with it being an older star.[4] The age of a star can also be estimated by the abundance of lithium, as this element is destroyed through thermonuclear fusion at the core. However, this is less accurate technique. For HD 12661, the lithium abundance gives an age estimate of 4.4 billion years.[9]
The abundance of elements other than hydrogen and helium, what astronomers term the metallicity, is unusually high in this star when compared to the Sun. High metallicity has been found to be statistically correlated with the presence of a multi-planet system around a star.[3] It is possible that a planet in this system may have been scattered and ended up being accreted by the star, which may account for the large surface metallicity.[10]
Planetary system edit
The first planet was discovered in 2001 from the Lick and Keck observatories using precision measurements of the star's radial velocity variations. The periodicity in this variation allowed astronomers to extract information about the planet's orbit and minimum mass.[3] A second planet was discovered by the same team two years later.[11] Both planets are greater in mass than Jupiter.[12]
The system is dynamically unstable.[13][14] "Either this system is being observed during a relatively rare state, or additional planets are affecting the observed radial velocities and/or the system’s secular eccentricity evolution."[10]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | >2.30 ± 0.19 MJ | 0.831 ± 0.048 | 262.709 ± 0.083 | 0.3768 ± 0.0077 | — | — |
| c | >1.92 ± 0.16 MJ | 2.90 ± 0.17 | 1708 ± 14 | 0.031 ± 0.022 | — | — |
See also edit
References edit
- ^ a b c d e f 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.
- ^ a b c d Giclas, H. L.; Burnham, R.; Thomas, N. G. (1971), Lowell proper motion survey Northern Hemisphere. The G numbered stars. 8991 stars fainter than magnitude 8 with motions > 0".26/year, Flagstaff, Arizona: Lowell Observatory, Bibcode:1971lpms.book.....G
- ^ a b c d e f g h i j k Fischer, Debra A.; et al. (2001), "Planetary Companions to HD 12661, HD 92788, and HD 38529 and Variations in Keplerian Residuals of Extrasolar Planets", The Astrophysical Journal, 551 (2): 1107–1118, Bibcode:2001ApJ...551.1107F, doi:10.1086/320224
- ^ a b c d e f Fischer, Debra A.; Valenti, Jeff (April 2005), "The Planet-Metallicity Correlation", The Astrophysical Journal, 622 (2): 1102–1117, Bibcode:2005ApJ...622.1102F, doi:10.1086/428383
- ^ Koriski, Shuki; Zucker, Shay (November 2011), "On the Ages of Planetary Systems with Mean-motion Resonances", The Astrophysical Journal Letters, 741 (1): L23, arXiv:1109.6671, Bibcode:2011ApJ...741L..23K, doi:10.1088/2041-8205/741/1/L23, S2CID 118553051
- ^ "G 72-54 -- High proper-motion Star", SIMBAD, Centre de Données astronomiques de Strasbourg
- ^ Sherrod, P. Clay; Koed, Thomas L. (2003), A Complete Manual of Amateur Astronomy: Tools and Techniques for Astronomical Observations, Astronomy Series, Courier Dover Publications, p. 9, ISBN 0-486-42820-6
- ^ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on March 18, 2012, retrieved 2012-01-16
- ^ a b Saffe, C.; Gómez, M.; Chavero, C. (November 2005), "On the ages of exoplanet host stars", Astronomy and Astrophysics, 443 (2): 609–626, arXiv:astro-ph/0510092, Bibcode:2005A&A...443..609S, doi:10.1051/0004-6361:20053452, S2CID 11616693
- ^ a b Veras, Dimitri; Ford, Eric B. (2008). "Secular evolution of HD 12661: a system caught at an unlikely time". The Astrophysical Journal. 690 (1): L1–L4. arXiv:0811.0001v1. Bibcode:2009ApJ...690L...1V. doi:10.1088/0004-637X/690/1/L1. S2CID 17386482.
- ^ Fischer, Debra A.; et al. (2003). "A Planetary Companion to HD 40979 and Additional Planets Orbiting HD 12661 and HD 38529". The Astrophysical Journal. 586 (2): 1394–1408. Bibcode:2003ApJ...586.1394F. doi:10.1086/367889.
- ^ a b Wright, J. T.; et al. (2009). "Ten New and Updated Multi-planet Systems, and a Survey of Exoplanetary Systems". The Astrophysical Journal (abstract). 693 (2): 1084–1099. arXiv:0812.1582. Bibcode:2009ApJ...693.1084W. doi:10.1088/0004-637X/693/2/1084. S2CID 18169921.
- ^ Gozdziewski, K. (2003). "Stability of the HD 12661 Planetary System". Astronomy and Astrophysics. 398 (3): 1151–1161. Bibcode:2003A&A...398.1151G. doi:10.1051/0004-6361:20021713.
- ^ Rodríguez, Adrián; Gallardo, Tabaré (2005). "The Dynamics of the HD 12661 Extrasolar Planetary System". The Astrophysical Journal. 628 (2): 1006–11013. Bibcode:2005ApJ...628.1006R. doi:10.1086/430816. S2CID 31278031.
External links edit
- "Notes for star HD 12661". Extrasolar Planets Encyclopaedia. Archived from the original on 2012-05-05. Retrieved 2006-04-14.
- "Two Planets Around HD 12661". California & Carnegie Planet Search. Retrieved 2006-04-14.
- Extrasolar Planet Interactions by Rory Barnes & Richard Greenberg, Lunar and Planetary Lab, University of Arizona
- Local Sky Map