HD 11506

Last updated • 2 min readFrom Wikipedia, The Free Encyclopedia
HD 11506
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Cetus
Right ascension 01h 52m 50.53442s [1]
Declination −19° 30′ 25.1082″ [1]
Apparent magnitude  (V)7.51 [2]
Characteristics
Spectral type G0V [3]
B−V color index 0.607±0.015 [2]
Astrometry
Radial velocity (Rv)−7.53±0.13 [1]  km/s
Proper motion (μ)RA: 22.039(22)  mas/yr [1]
Dec.: −97.904(16)  mas/yr [1]
Parallax (π)19.5342 ± 0.0221  mas [1]
Distance 167.0 ± 0.2  ly
(51.19 ± 0.06  pc)
Absolute magnitude  (MV)3.94 [2]
Details [4]
Mass 1.22±0.02 [5]   M☉
Radius 1.06±0.01  R☉
Luminosity 1.17±0.01  L☉
Surface gravity (log g)4.43±0.02  cgs
Temperature 5,833±28  K
Metallicity [Fe/H]+0.30±0.06 [5]   dex
Rotation ~15 days [5]
Rotational velocity (v sin i)5.5±0.5 [5]  km/s
Age 1.6±0.9  Gyr
Other designations
BD−20°358, HD  11506, HIP  8770, SAO  148079 [6]
Database references
SIMBAD data
Exoplanet Archive data

HD 11506 is a star in the equatorial constellation of Cetus. It has a yellow hue and can be viewed with a small telescope but is too faint to be visible to the naked eye, having an apparent visual magnitude of 7.51. [2] The distance to this object is 167  light-years based on parallax, but it is drifting closer to the Sun with a radial velocity of −7.5 km/s. [1] It has an absolute magnitude of 3.94. [2]

This object is an ordinary G-type main-sequence star with a stellar classification of G0V, [3] which indicates it is generating energy via hydrogen fusion at its core. It is around 1.6 [4]  billion years old and is spinning with a projected rotational velocity of 5 km/s. [7] The star has 112% of the mass of the Sun and 106% of the Sun's radius. The spectrum shows a higher than solar abundance of elements other than hydrogen and helium – what astronomers term the metallicity. [8] The star is radiating 117% of the Sun's luminosity from its photosphere at an effective temperature of 5,833 K. [4]

Planetary system

The superjovian planet HD 11506 b was discovered orbiting the star by the N2K Consortium in 2007 using the Doppler spectroscopy method. [3] In 2009, a second planet discovery was claimed based on Bayesian analysis of the original data. [9] However, in 2015 additional radial velocity measurements showed that the planetary parameters were significantly different than those determined by Bayesian analysis. An additional linear trend in the radial velocities indicated a stellar or planetary companion on a long term orbit. [8]

In 2022, the presence of a third planet was confirmed, and the mass and inclination of both planet b and the new planet d were measured via astrometry. [10] A 2024 study also confirmed HD 11506 d, but found a significantly wider orbit and greater mass than previously estimated. This object orbits with a 73-year period, and at about 13 times the mass of Jupiter, it is at the borderline of being a brown dwarf. [5]

The HD 11506 planetary system [5]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
c ≥0.40±0.02  MJ 0.771±0.004223.92±0.370.228±0.054——
b 4.80±0.08  MJ 2.885±0.0161,617.7±1.90.379±0.009113+23
−53 [10] ° 		—
d12.8+0.6
−0.5  MJ 		18.20+0.06
−0.09		26,517+256
−292		0.29+0.02
−0.03		90+6
−5 ° 		—

Related Research Articles

HD 208487 is a star with an orbiting exoplanet in the constellation of Grus. Based on parallax measurements, it is located at a distance of 146.5 light years from the Sun. The absolute magnitude of HD 208487 is 4.26, but at that distance the apparent visual magnitude is 7.47, which is too faint to be viewed with the naked eye. The system is drifting further away with a radial velocity of 5.6 km/s. It is a member of the thin disk population.

HD 125612 is a binary star system with three exoplanetary companions in the equatorial constellation of Virgo. It is too dim to be visible to the naked eye, having an apparent visual magnitude of 8.31. The system is located at a distance of 188 light years from the Sun based on parallax measurements, but it is drifting closer with a radial velocity of −18 km/s.

HD 170469 is a probable binary star system in the equatorial constellation of Ophiuchus. It is too faint to be viewed with the naked eye, having an apparent visual magnitude of 8.21. The system is located at a distance of 197 light years away from the Sun based on parallax. It is drifting closer with a radial velocity of −59 km/s, and is expected to come to within 49.8 light-years in about 959,000 years.

HIP 14810 is a star with three exoplanetary companions in the northern constellation of Aries. It positioned about 1.3° to the north of Delta Arietis, but is too faint to be visible to the naked eye with an apparent visual magnitude of 8.6. The system is located at a distance of 165 light-years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −5 km/s.

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 137 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 5319 is an 8th magnitude star approximately 319 light years away in the constellation Cetus. It is a subgiant star of spectral type K3, having run out of hydrogen in its core. When it was main-sequence, the spectral type was early F or late A.

HD 75898 is an 8th magnitude star approximately 255 light-years away in the constellation Lynx. The star is 28% more massive, 60% larger, and 3 times as luminous as the Sun. It is a metal-rich star, with 186% the solar abundance of iron. In 2007 the California and Carnegie Planet Search team found one planet orbiting HD 75898.

HD 33283 is a star in the southern constellation Lepus with one planet and a co-moving stellar companion. With an apparent visual magnitude of 8.05, the star is too faint to be seen with the naked eye. It is located at a distance of 294 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +4.5.

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.

HD 73256 is a variable star in the southern constellation of Pyxis. It has the variable star designation CS Pyxidis. With a baseline apparent visual magnitude of 8.08, it requires binoculars or a small telescope to view. The star is located at a distance of 120 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +30 km/s.

HD 109749 is a binary star system about 206 light years away in the constellation of Centaurus. The pair have a combined apparent visual magnitude of 8.08, which is too faint to be visible to the naked eye. The primary component has a close orbiting exoplanet companion. The system is drifting closer with a heliocentric radial velocity of −13.2 km/s.

HD 149143, also called Rosalíadecastro, is a star with a close orbiting exoplanet in the Ophiuchus constellation. Its apparent visual magnitude is 7.89 and the absolute magnitude is 3.87. The system is located at a distance of 239 light years from the Sun based on parallax measurements, and it is drifting further away with a radial velocity of 12 km/s.

HD 33636 is a G-type main-sequence star located approximately 96.5 light-years away in the Orion constellation. It is a 7th magnitude star with a metallicity of −0.05 ± 0.07. A likely substellar companion was discovered in 2002.

HD 11506 c is an extrasolar planet located approximately 167 light years away in the constellation of Cetus, orbiting the 8th magnitude G-type main sequence star HD 11506. It is the second planet in this system, and its discovery was first claimed in 2009 by using Bayesian analysis on data previously collected by the N2K Consortium. However, in 2015 additional radial velocity measurements showed that the planetary parameters were significantly different from those determined by Bayesian analysis.

HD 16760 is a binary star system approximately 227 light-years away in the constellation Perseus. The primary star HD 16760 is a G-type main sequence star similar to the Sun. The secondary, HIP 12635 is 1.521 magnitudes fainter and located at a separation of 14.6 arcseconds from the primary, corresponding to a physical separation of at least 660 AU. Announced in July 2009, HD 16760 has been confirmed to have a red dwarf orbiting it, formerly thought to be a brown dwarf or exoplanet.

HD 179079 is a star with an exoplanetary companion in the equatorial constellation of Aquila. It has an apparent visual magnitude of approximately 7.96, making it too faint to be readily visible to the naked eye. The distance to this star can be determine using parallax measurements, which yields an estimate of approximately 228 light years. It is drifting further away with a radial velocity of +20 km/s.

HD 204313 is a star with two and possibly three exoplanetary companions in the southern constellation of Capricornus. With an apparent magnitude of 7.99, it is an eighth magnitude star that is too faint to be readily visible to the naked eye. The star is located at a distance of 157 light years from the Sun based on parallax measurements, but it is drifting closer with a radial velocity of −10 km/s.

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 79498 is a double star in the northern constellation of Cancer. The primary component of this pair has an orbiting exoplanet companion. This star is too faint to be viewed with the naked eye, having an apparent visual magnitude of 8.05. The system is located at a distance of 159 light years based on parallax measurements, and is drifting further away with a heliocentric radial velocity of 20 km/s. It has a relatively high proper motion, traversing the celestial sphere at an angular rate of 0.2″·yr−1.

HD 207832 is a G-type main-sequence star. Its surface temperature is 5764±15 K. HD 207832 is slightly enriched compared to the Sun in its concentration of heavy elements, with a metallicity Fe/H index of 0.17±0.01 and is much younger at an age of 0.74±0.62 billion years. Kinematically, it belongs to the thin disk of the Milky Way.

References

  1. 1 2 3 4 5 6 7 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 4 5 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 Fischer, Debra A.; et al. (2007). "Five Intermediate-Period Planets from the N2K Sample". The Astrophysical Journal. 669 (2): 1336–1344. arXiv: 0704.1191 . Bibcode:2007ApJ...669.1336F. doi:10.1086/521869. S2CID   7774321.
  4. 1 2 3 Bonfanti, A.; et al. (2015). "Revising the ages of planet-hosting stars". Astronomy and Astrophysics. 575. A18. arXiv: 1411.4302 . Bibcode:2015A&A...575A..18B. doi:10.1051/0004-6361/201424951. S2CID   54555839.
  5. 1 2 3 4 5 6 Ruggieri, A.; Desidera, S.; et al. (September 2024). "The GAPS Programme at TNG: LVIII. Two multi-planet systems with long-period substellar companions around metal-rich stars". Astronomy & Astrophysics . 689: A235. Bibcode:2024A&A...689A.235R. doi: 10.1051/0004-6361/202449456 . hdl: 2108/390324 .
  6. ↑ "HD 11506". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2019-11-10.
  7. ↑ Delgado Mena, E.; et al. (April 2015). "Li abundances in F stars: planets, rotation, and Galactic evolution". Astronomy & Astrophysics. 576: 24. arXiv: 1412.4618 . Bibcode:2015A&A...576A..69D. doi:10.1051/0004-6361/201425433. S2CID   56051637. A69.
  8. 1 2 Giguere, Matthew J.; et al. (2015). "Newly Discovered Planets Orbiting HD 5319, HD 11506, HD 75784 and HD 10442 from the N2K Consortium". The Astrophysical Journal. 799 (1). 89. arXiv: 1411.5374 . Bibcode:2015ApJ...799...89G. doi:10.1088/0004-637X/799/1/89. S2CID   56121568.
  9. ↑ Tuomi, M.; Kotiranta, S. (2009). "Bayesian analysis of the radial velocities of HD 11506 reveals another planetary companion". Astronomy and Astrophysics. 496 (2): L13 –L16. arXiv: 0902.2997 . Bibcode:2009A&A...496L..13T. doi:10.1051/0004-6361/200811531. S2CID   16414890.
  10. 1 2 Feng, Fabo; Butler, R. Paul; et al. (August 2022). "3D Selection of 167 Substellar Companions to Nearby Stars". The Astrophysical Journal Supplement Series . 262 (21): 21. arXiv: 2208.12720 . Bibcode:2022ApJS..262...21F. doi: 10.3847/1538-4365/ac7e57 . S2CID   251864022.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.