HD 154088

Last updated
HD 154088
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Ophiuchus [1]
Right ascension 17h 04m 27.843s [2]
Declination −28° 34′ 57.64″ [2]
Apparent magnitude  (V)6.584±0.010 [3]
Characteristics
Evolutionary stage subgiant [2]
Spectral type K0IV-V [4]
B−V color index 0.814±0.034 [1]
Astrometry
Radial velocity (Rv)14.2972±0.0003 [5] km/s
Proper motion (μ)RA: +83.309 [2] mas/yr
Dec.: −268.614 [2] mas/yr
Parallax (π)54.726±0.0236  mas [2]
Distance 59.60 ± 0.03  ly
(18.273 ± 0.008  pc)
Absolute magnitude  (MV)5.33 [1]
Details
Mass 0.91±0.02 [6]   M☉
Radius 0.95±0.03 [7]   R☉
Luminosity 0.68+0.06
−0.05 [8]   L☉
Surface gravity (log g)4.37±0.07 [6]   cgs
Temperature 5,374±43 [6]   K
Metallicity [Fe/H]+0.28±0.03 [6]   dex
Rotation 42.6±4.4 [9] days
Rotational velocity (v sin i)1.9±0.5 [8]  km/s
Age 8±2 [6]   Gyr
Other designations
CD−28°12769, GJ 652, HIP 83541, SAO 184990
Database references
SIMBAD data
Exoplanet Archive data

HD 154088 is a seventh magnitude metal-rich K-type subgiant that lies 59.6 light-years away in the constellation of Ophiuchus. The star is orbited by a hot Super-Earth.

Contents

Properties

HRDiagram.png
Iconol teal circle.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 K0IV-V, indicating that it has characteristics intermediate to a subgiant and 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.[ citation needed ] 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. [10] It also has a magnetic cycle similar to the Sun, [9] though its length is not well constrained.

A survey in 2015 ruled out the existence of any additional stellar companions at projected distances from 8 to 119 astronomical units. [11]

Planetary system

A planet orbiting HD 154088 discovered with the HARPS spectrograph was announced in a September 2011 preprint. With a minimum mass of 6  M🜨, the companion falls into the regime of Super-Earths. [5] HD 154088 has also been observed under the Keck Eta-Earth radial velocity survey. A 2010 paper about this survey listed a "Candidate 1" that has similar properties to HD 154088 b (orbital period = 18.1 days, minimum mass = 6.5  M🜨), and so may be the same detection. [12] The planet's existence was finally confirmed and formally published in 2021. [6]

The HD 154088 planetary system [6]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b≥6.6±0.8  M🜨 0.134±0.00218.56±0.01<0.344——

References

  1. 1 2 3 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.
  2. 1 2 3 4 5 6 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.
  3. ↑ Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (March 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27 –L30. Bibcode:2000A&A...355L..27H. ISSN   0004-6361.
  4. ↑ Gray, R. O.; Corbally, C. J.; Garrison, R. F.; McFadden, M. T.; Bubar, E. J.; McGahee, C. E.; O'Donoghue, A. A.; Knox, E. R. (2006). "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 pc-The Southern Sample". The Astronomical Journal. 132 (1): 161. arXiv: astro-ph/0603770 . Bibcode:2006AJ....132..161G. doi:10.1086/504637.
  5. 1 2 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: 1109.2497 [astro-ph.EP].
  6. 1 2 3 4 5 6 7 Unger, N.; Ségransan, D.; Queloz, D.; Udry, S.; Lovis, C.; Mordasini, C.; Ahrer, E.; Benz, W.; Bouchy, F.; Delisle, J.-B.; Díaz, R. F.; Dumusque, X.; Lo Curto, G.; Marmier, M.; Mayor, M.; Pepe, F.; Santos, N. C.; Stalport, M.; Alonso, R.; Collier Cameron, A.; Deleuil, M.; Figueira, P.; Gillon, M.; Moutou, C.; Pollacco, D.; Pompei, E. (2021). "The HARPS search for southern extra-solar planets". Astronomy & Astrophysics. 654: A104. arXiv: 2108.10198 . Bibcode:2021A&A...654A.104U. doi:10.1051/0004-6361/202141351.
  7. ↑ 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 (2): 297–318. arXiv: astro-ph/0607235 . Bibcode:2007ApJS..168..297T. doi:10.1086/509763. S2CID   18775378.
  8. 1 2 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 (1): 141–166. Bibcode:2005ApJS..159..141V. doi: 10.1086/430500 .
  9. 1 2 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: 1107.5325 [astro-ph.SR].
  10. ↑ Fossati, L.; et al. (2013). "Detection of a magnetic field in three old and inactive solar-like planet-hosting stars". Astronomy. 551: A85. arXiv: 1302.0879 . Bibcode:2013A&A...551A..85F. doi:10.1051/0004-6361/201220997. S2CID   53377473.
  11. ↑ Mugrauer, M.; Ginski, C. (12 May 2015). "High-contrast imaging search for stellar and substellar companions of exoplanet host stars". Monthly Notices of the Royal Astronomical Society. 450 (3): 3127–3136. Bibcode:2015MNRAS.450.3127M. doi: 10.1093/mnras/stv771 . hdl: 1887/49340 .
  12. ↑ Howard, Andrew A.; et al. (2010). "The Occurrence and Mass Distribution of Close-in Super-Earths, Neptunes, and Jupiters". Science. 330 (6004): 653–655. arXiv: 1011.0143 . Bibcode:2010Sci...330..653H. doi:10.1126/science.1194854. PMID   21030652. S2CID   34792507.
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.