HD 12661

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HD 12661
HD 12661 orbit.svg
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
BD+24 298, HIP 9683, SAO 75125. [6]
Database references
SIMBAD data

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.

Contents

Properties

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

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]

The HD 12661 planetary system [12]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b >2.30 ± 0.19  MJ 0.831 ± 0.048262.709 ± 0.0830.3768 ± 0.0077——
c >1.92 ± 0.16  MJ 2.90 ± 0.171708 ± 140.031 ± 0.022——

See also

Related Research Articles

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HD 46375 is double star with an exoplanetary companion in the equatorial constellation of Monoceros. It presents as an 8th-magnitude star with an apparent visual magnitude of 7.91, which is too dim to be readily visible to the naked eye. The system is located at a distance of 96.5 light-years from the Sun based on parallax measurements, but is slowly drifting closer with a radial velocity of −1 km/s. The common proper motion stellar companion, designated HD 46375 B, has a linear projected separation of 346±13 AU.

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<span class="mw-page-title-main">HD 108874</span> Star in the constellation Coma Berenices

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<span class="mw-page-title-main">HD 128311</span> Star in the constellation Boötes

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HD 217107 b is an extrasolar planet approximately 65 light-years away from Earth in the constellation of Pisces. The planet was discovered orbiting the star HD 217107 approximately every seven days, classifying the planet as a hot Jupiter. Because of the planet's somewhat eccentric orbit, scientists were able to confirm another planet within the system.

<span class="mw-page-title-main">HD 217107 c</span> Extrasolar planet in the constellation Pisces

HD 217107 c is an extrasolar planet approximately 64 light-years away from Earth in the constellation of Pisces. The planet was the second planet to be discovered orbiting the star HD 217107. HD 217107 c's existence was hypothesized in 1998 due to the eccentricity of the inner planet's orbit and confirmed in 2005 when radial velocity studies of the star indicated another, more distant and massive companion orbiting the star. The planet has an eccentric orbit lasting on order of a decade.

HD 11964 is a binary star system located 110 light-years away from the Sun in the equatorial constellation of Cetus. It is visible in binoculars or a telescope but is too faint to be seen with the naked eye, having an apparent visual magnitude of 7.51. The system is drifting closer to the Sun with a radial velocity of −9 km/s. Two extrasolar planets have been confirmed to orbit the primary.

HD 222582 is a multiple star system in the equatorial constellation of Aquarius. It is invisible to the naked eye with an apparent visual magnitude of 7.7, but can be viewed with binoculars or a small telescope. The system is located at a distance of 138 light years from the Sun based on parallax, and it is drifting further away with a radial velocity of +12 km/s. It is located close enough to the ecliptic that it is subject to lunar occultations.

HD 92788 is a star in the equatorial constellation of Sextans. It has a yellow hue but is too dim to be visible to the naked eye, having an apparent visual magnitude of 7.31. The star is located at a distance of 113 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −4.5 km/s. Two planets have been found in orbit around the star.

HD 196050 is a triple star system located in the southern constellation of Pavo. This system has an apparent magnitude of 7.50 and the absolute magnitude is 4.01. It is located at a distance of 112 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +61 km/s. It is also called by the Hipparcos number 101806.

References

  1. 1 2 3 4 5 6 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. 1 2 3 4 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
  3. 1 2 3 4 5 6 7 8 9 10 11 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
  4. 1 2 3 4 5 6 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
  5. ↑ 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
  6. ↑ "G 72-54 -- High proper-motion Star", SIMBAD, Centre de Données astronomiques de Strasbourg
  7. ↑ 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
  8. ↑ "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
  9. 1 2 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
  10. 1 2 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.
  11. ↑ 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 .
  12. 1 2 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.
  13. ↑ 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 .
  14. ↑ 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.

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