HD 5319

HD 5319
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cetus
Right ascension 00h 55m 01.40s[1]
Declination +00° 47′ 22.4″[1]
Apparent magnitude (V) 8.05
Characteristics
Spectral type K3IV[2]
Astrometry
Proper motion (μ) RA: –4.93 ± 0.90[1] mas/yr
Dec.: –49.66 ± 0.53[1] mas/yr
Parallax (π)8.74 ± 0.86[1] mas
Distance370 ± 40 ly
(110 ± 10 pc)
Details
Mass1.40 ± 0.14[3] M☉
Radius3.97 ± 0.43[3] R☉
Luminosity9[3] L☉
Metallicity [Fe/H]+0.14[3] dex
Age3.30 ± 1.11[3] Gyr
Other designations
BD+00°142, HIP 4297, SAO 109532
Database references
SIMBADdata
Exoplanet Archivedata
Extrasolar Planets
Encyclopaedia		data

HD 5319 is an 8th magnitude star approximately 370 light years away[1] 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.

The absolute magnitude (apparent magnitude at 10 parsecs) is 3.05, which would translate to easy naked eye visibility, but its distance is ten times greater, so its apparent magnitude is 8.05 (100 times fainter than its absolute magnitude), it is not visible to the naked eye and binoculars are needed.

Planetary system

On January 11, 2007, the California and Carnegie Planet Search team found an extrasolar planet with a minimum mass 1.76 times that of Jupiter orbiting the star. It was published in the December 1, 2007 edition of the Astrophysical Journal.[4] A second planet was discovered in 2015. Orbital simulations of the dynamical stability of the planetary system indicate that it is likely in a 4:3 mean motion resonance.[2] Previous computer simulations have shown an inability to reproduce this resonance in gas giant systems using a variety of formation and migration mechanisms.[5] Additional analysis on the stability of the system show that the planets orbits may have to be inclined to one another to maintain stability.[6]

The HD 5319 planetary system[2]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b >1.76 ± 0.07 MJ 1.6697 ± 0.0036 641 ± 2 0.02 ± 0.03 — —
c >1.15 ± 0.08 MJ 2.071 ± 0.013 886 ± 8 0.15 ± 0.06 — —

See also

References

  1. 1 2 3 4 5 6 van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. Vizier catalog entry
  2. 1 2 3 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.
  3. 1 2 3 4 5 Ghezzi, L.; et al. (December 2010), "Metallicities of Planet-hosting Stars: A Sample of Giants and Subgiants", The Astrophysical Journal, 725 (1): 721–733, arXiv:1008.3539, Bibcode:2010ApJ...725..721G, doi:10.1088/0004-637X/725/1/721.
  4. ↑ Robinson, Sarah E.; et al. (2007). "Two Jovian-Mass Planets in Earthlike Orbits". The Astrophysical Journal. 670 (2): 1391–1400. arXiv:0708.0832. Bibcode:2007ApJ...670.1391R. doi:10.1086/522106.
  5. ↑ Rein, Hanno; et al. (2012). "Traditional formation scenarios fail to explain 4:3 mean motion resonances". Monthly Notices of the Royal Astronomical Society. 426 (1): 187–202. arXiv:1204.0974. Bibcode:2012MNRAS.426..187R. doi:10.1111/j.1365-2966.2012.21798.x.
  6. ↑ Kane, Stephen R. (2016). "Resolving Close Encounters: Stability in the HD 5319 and HD 7924 Planetary Systems". The Astrophysical Journal. 830 (2). 105. arXiv:1411.5374. Bibcode:2016ApJ...830..105K. doi:10.3847/0004-637X/830/2/105.
  • "HD 5319". The Extrasolar Planets Encyclopaedia.

Coordinates: 00h 55m 01.4005s, +00° 47′ 22.392″

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