HD 5608
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Andromeda
Right ascension 00h 58m 14.21894s[1]
Declination +33° 57′ 03.1841″[1]
Apparent magnitude (V) +5.98[2]
Characteristics
Evolutionary stage Red giant branch[3]
Spectral type K0 IV[4]
B−V color index 1.016[2]
Astrometry
Radial velocity (Rv)−23.13±0.12[1] km/s
Proper motion (μ) RA: 36.459 mas/yr[1]
Dec.: -71.320 mas/yr[1]
Parallax (π)17.0697 ± 0.0302 mas[1]
Distance191.1 ± 0.3 ly
(58.6 ± 0.1 pc)
Absolute magnitude (MV)+2.11[4]
Orbit[5]
Period (P)146+74
−37 yr
Semi-major axis (a)0.524+0.151
−0.084"
(30.7+8.8
−4.9 AU)
Eccentricity (e)0.53+0.18
−0.26
Inclination (i)147.5+6.6
−13°
Longitude of the node (Ω)141+56
−48°
Periastron epoch (T)2,472,895+17,464
−5,098
Argument of periastron (ω)
(secondary)		257+32
−35°
Details[6]
HD 5608 A
Mass1.50±0.04 M☉
Radius5.0±0.1 R☉
Luminosity13.1±0.3 L☉
Surface gravity (log g)3.20±0.02 cgs
Temperature4,897±25 K
Metallicity [Fe/H]+0.12±0.03[3] dex
Rotational velocity (v sin i)1.37[4] km/s
Age3.0±0.3 Gyr
HD 5608 B
Mass0.10±0.01[7] M☉
Mass121.2+8.3
−7.0[5] MJup
Other designations
BD+33° 140, FK5 2061, HD 5608, HIP 4552, HR 275, SAO 54306[8]
Database references
SIMBADdata

HD 5608 is an orange-hued star in the northern constellation of Andromeda with one known planet, HD 5608 b.[4] It is a dim star near the lower limit of visibility to the naked eye, having an apparent visual magnitude of +5.98.[2] The distance to HD 5608, as estimated from an annual parallax shift of 17.07 mas,[1] is 191 light-years (59 parsecs). It is moving closer to the Earth with a heliocentric radial velocity of −23 km/s,[1] and is expected to make its closest approach in 1.285 million years when it comes to within 124 light-years.[9]

This is a K-type subgiant star on the red giant branch track with a stellar classification of K0 IV.[4] It has 1.5 times the mass of the Sun and, at the age of three billion years, has expanded to five times the Sun's radius. It is radiating 13 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,897 K. It has a higher than solar metallicity – a term astronomers use to describe the abundance of elements other than hydrogen and helium.[6]

HD 5608 has a co-moving companion, HD 5608 B, at an angular separation of 0.6″, which has been directly imaged. The physical separation of the pair is calculated as 40±1 AU or 47±3 AU, depending on the assumptions. It has an H band magnitude difference of 9.40 with the primary and an estimated mass of 0.10 M☉. A second companion at a separation of 7.4″ is a background star.[7] This companion star has since been characterized by radial velocity and astrometry in addition to imaging.[5]

Planetary companion

In 2012, the Okayama Planet Search Program reported the detection of a substellar companion in orbit around HD 5608, based upon Doppler measurements between 2003 and 2011 from the Okayama observatory in Kurashiki. These showed a linear trend indicating the existence of a distant companion. The data showed an additional periodicity of around 766 days. This object shows a minimum mass of 1.4 MJ, a semimajor axis of 1.9 AU, and an eccentricity of 0.19.[4] The high eccentricity of this planet could have been induced by the low mass companion star HD 5608 B via the Kozai mechanism.[7]

The HD 5608 A planetary system[5]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b ≥1.168+0.062
−0.057 MJ		 1.790+0.007
−0.003		 768.70+4.72
−1.67		 0.110+0.029
−0.080		 — —

References

  1. 1 2 3 4 5 6 7 8 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 Høg, E.; et al. (200). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy & Astrophysics. 355: L27–L30. Bibcode:2000A&A...355L..27H.
  3. 1 2 Stock, Stephan; et al. (August 2018). "Precise radial velocities of giant stars. X. Bayesian stellar parameters and evolutionary stages for 372 giant stars from the Lick planet search". Astronomy & Astrophysics. 616: 15. arXiv:1805.04094. Bibcode:2018A&A...616A..33S. doi:10.1051/0004-6361/201833111. S2CID 119361866. A33.
  4. 1 2 3 4 5 6 Sato, Bun'ei; et al. (2012). "Substellar Companions to Seven Evolved Intermediate-Mass Stars". Publications of the Astronomical Society of Japan. 64 (6). 135. arXiv:1207.3141. Bibcode:2012PASJ...64..135S. doi:10.1093/pasj/64.6.135. S2CID 119197073.
  5. 1 2 3 4 Teng, Huan-Yu; Sato, Bun'ei; et al. (December 2023). "Revisiting Planetary Systems in Okayama Planet Search Program: A new long-period planet, RV astrometry joint analysis, and multiplicity-metallicity trend around evolved stars". Publications of the Astronomical Society of Japan. 75 (6): 1030–1071. arXiv:2308.05343. doi:10.1093/pasj/psad056.
  6. 1 2 Bonfanti, A.; et al. (2016). "Age consistency between exoplanet hosts and field stars". Astronomy & Astrophysics. 585: A5, 14 pp. arXiv:1511.01744. Bibcode:2016A&A...585A...5B. doi:10.1051/0004-6361/201527297. S2CID 53971692.
  7. 1 2 3 Ryu, Tsuguru; et al. (July 2016). "High-contrast Imaging of Intermediate-mass Giants with Long-term Radial Velocity Trends". The Astrophysical Journal. 825 (2): 13. arXiv:1603.02017. Bibcode:2016ApJ...825..127R. doi:10.3847/0004-637X/825/2/127. PMC 7402361. PMID 32753766. 127.
  8. ↑ "HD 5608". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved October 10, 2018.
  9. ↑ 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.
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