HD 154088

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HD 154088
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Ophiuchus
Right ascension 17h 04m 27.84s ± 5.62[1]
Declination −28° 34′ 57.64″ ± 3.16[1]
Apparent magnitude (V) 6.7258 ± 0.005[1]
Spectral type K0V
B−V color index 0.814 ± 0.034[1]
Radial velocity (Rv) 14.2972 ± 0.0003[2] km/s
Proper motion (μ) RA: 83.76 ± 0.64[1] mas/yr
Dec.: -268.69 ± 0.36[1] mas/yr
Parallax (π) 56.06 ± 0.50[1] mas
Distance 58.2 ± 0.5 ly
(17.8 ± 0.2 pc)
Absolute magnitude (MV) 5.47 ± 0.02
Mass 0.97 ± 0.05[3] M
Radius 0.95 ± 0.03[4] R
Luminosity 0.68 +0.06
(log -0.169 ± 0.033)[5] L
Surface gravity (log g) 4.40 ± 0.11[3] cgs
Temperature 5423 ± 51[3] K
Metallicity [Fe/H] 0.31 ± 0.03[3] dex
Rotation 42.6 ± 4.4[6]
Rotational velocity (v sin i) 1.9 ± 0.5[5] km/s
Age 3 - 8[3] Gyr
Other designations
CD−28° 12769, GJ 652, HIP 83541, SAO 184990
Database references
Extrasolar Planets

HD 154088 is a seventh magnitude metal-rich K-type main sequence star that lies approximately 58 light-years away in the constellation of Ophiuchus. The star is orbited by a hot Super-Earth.


The position of HD 154088 on the Hertzsprung-Russell diagram.
Chess tile xg.svg

HD 154088 is a modestly bright star that lies at the bottom of Ophiuchus, near to the border with Scorpius and near to the plane of the Milky Way. The star was recognised as a high proper motion star during the last century, and early Earth-based parallax measurements such as that of the Gliese Catalogue of Nearby Stars indicated a distance of about 50 light-years.

The star has a spectral type of K0V, indicating that it is a main sequence star that is about 350 degrees cooler than the Sun. On the Hertzsprung-Russell diagram (left), the star lies slightly above the main sequence. This is because the star is very metal-rich; with an Fe/H of 0.3 dex the star has about twice the solar abundance of iron, which makes HD 154088 fall into the somewhat vague group of super metal-rich (SMR) stars. The giant planet occurrence rate of Fe/H = 0.3 stars is on the order of 30%, but HD 154088 is not currently known to host any giant planets.

HD 154088 has a pronounced magnetic field.[3] It also has a magnetic cycle similar to the Sun,[6] though its length is not well constrained.

Planetary system[edit]

A planet orbiting HD 154088 discovered with the HARPS spectrograph was announced in September 2011. With a minimum mass of 6 Earth masses, the companion falls into the regime of Super-Earths.

The HD 154088 planetary system[2]
(in order from star)
Mass Semimajor axis
Orbital period
Eccentricity Inclination Radius
b ≥6.15 ± 0.86 M 0.1316 ± 0.0021 18.596 ± 0.021 0.38 ± 0.15

HD 154088 is also being observed under the Keck Eta-Earth radial velocity survey.[7] HD 154088 b is a close match for planet candidate 1 (orbital period = 18.1 days, minimum mass = 6.5 M), so they may be the same detection.


  1. ^ a b c d e f g van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752Freely accessible. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. 
  2. ^ a b Mayor, M.; et al. (2011). "The HARPS search for southern extra-solar planets XXXIV. Occurrence, mass distribution and orbital properties of super-Earths and Neptune-mass planets". arXiv:1109.2497Freely accessible. Bibcode:2011arXiv1109.2497M. 
  3. ^ a b c d e f Fossati, L.; et al. (2013). "Detection of a magnetic field in three old and inactive solar-like planet-hosting stars". Astronomy. 551: A85. arXiv:1302.0879Freely accessible. Bibcode:2013A&A...551A..85F. doi:10.1051/0004-6361/201220997. 
  4. ^ Takeda, Genya; et al. (2007). "Structure and Evolution of Nearby Stars with Planets. II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog". The Astrophysical Journal Supplement Series. 168: 297–318. arXiv:astro-ph/0607235Freely accessible. Bibcode:2007ApJS..168..297T. doi:10.1086/509763. 
  5. ^ a b Valenti, J. A.; Fischer, D. A. (2005). "Spectroscopic Properties of Cool Stars (SPOCS). I. 1040 F, G, and K Dwarfs from Keck, Lick, and AAT Planet Search Programs". The Astrophysical Journal Supplement Series. 159: 141–166. Bibcode:2005ApJS..159..141V. doi:10.1086/430500. 
  6. ^ a b Lovis, C.; et al. (2011). "The HARPS search for southern extra-solar planets. XXXI. Magnetic activity cycles in solar-type stars: statistics and impact on precise radial velocities". arXiv:1107.5325Freely accessible. Bibcode:2011arXiv1107.5325L. 
  7. ^ Howard, Andrew A.; et al. (2010). "The Occurrence and Mass Distribution of Close-in Super-Earths, Neptunes, and Jupiters". Science. 330: 653–655. arXiv:1011.0143Freely accessible. Bibcode:2010Sci...330..653H. doi:10.1126/science.1194854. PMID 21030652. 

Coordinates: Sky map 17h 04m 27.84s, −28° 34′ 57.64″