HD 5608

Last updated
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]
Distance 191.1 ± 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
Mass 1.50±0.04  M☉
Radius 5.0±0.1  R☉
Luminosity 13.1±0.3  L☉
Surface gravity (log g)3.20±0.02  cgs
Temperature 4,897±25  K
Metallicity [Fe/H]+0.12±0.03 [3]   dex
Rotational velocity (v sin i)1.37 [4]  km/s
Age 3.0±0.3  Gyr
HD 5608 B
Mass 0.10±0.01 [7]   M☉
Mass 121.2+8.3
−7.0 [5]   MJup
Other designations
BD+33° 140, FK5  2061, HD  5608, HIP  4552, HR  275, SAO  54306 [8]
Database references
SIMBAD data
Extrasolar Planets
Encyclopaedia 		data

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		——

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HD 100655 is a star in the zodiac constellation of Leo, located 449 light years away from the Sun. It has an apparent visual magnitude of +6.45, which makes it a challenge to see with the naked eye under ideal viewing conditions. The star is moving closer to the Earth with a heliocentric radial velocity of −5 km/s. It has one confirmed planet.

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References

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  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.
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  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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