HD 5319
| Observation data EpochJ2000.0EquinoxJ2000.0 | |
|---|---|
| Constellation | Cetus |
| Right ascension | 00h77m01.3977s[1] |
| Declination | +00° 47′ 22.4012″[1] |
| Apparent magnitude(V) | 8.05 |
| Characteristics | |
| Spectral type | K3IV[2] |
| Astrometry | |
| Proper motion(μ) | RA:−5.398±0.105[1]mas/yr Dec.:−49.564±0.063[1]mas/yr |
| Parallax(π) | 8.2083 ± 0.0476mas[1] |
| Distance | 397 ± 2ly (121.8 ± 0.7pc) |
| Details | |
| Mass | 1.40 ± 0.14[3]M☉ |
| Radius | 3.97 ± 0.43[3]R☉ |
| Luminosity | 9[3]L☉ |
| Metallicity[Fe/H] | +0.14[3]dex |
| Age | 3.30 ± 1.11[3]Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
HD 5319is an 8thmagnitudestarapproximately 319light yearsaway in theconstellationCetus.It is asubgiant starofspectral typeK3, having run out ofhydrogenin its core. When it wasmain-sequence,the spectral type was early F or late A.
Theabsolute magnitude(apparent magnitude at 10parsecs) is 3.05, which would translate to easy naked eye visibility, but its distance is ten times greater, so itsapparent magnitudeis 8.05 (100 times fainter than its absolute magnitude), it is not visible to thenaked eyeandbinocularsare needed.
Planetary system
[edit]On January 11, 2007, theCalifornia and Carnegie Planet Searchteam found anextrasolar planetwith a minimum mass 1.76 times that ofJupiterorbiting the star. It was published in the December 1, 2007 edition of theAstrophysical Journal.[4]A second planet was discovered in November 2014. Orbital simulations of the dynamical stability of the planetary system indicate that it is likely in a 4:3mean 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 beinclinedto one another to maintain stability,[6]although simplest solution as in 2019 still indicate the planetary system of HD 5319 is unstable.[7]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥1.56±0.29MJ | 1.57±0.13 | 638.6±1.2 | 0.015±0.016 | — | — |
| c | ≥1.02±0.22MJ | 1.94±0.16 | 877.0±4.9 | 0.109±0.067 | — | — |
See also
[edit]References
[edit]- ^abcdeBrown, A. G. A.;et al. (Gaia collaboration) (August 2018)."GaiaData Release 2: Summary of the contents and survey properties ".Astronomy & Astrophysics.616.A1.arXiv:1804.09365.Bibcode:2018A&A...616A...1G.doi:10.1051/0004-6361/201833051.Gaia DR2 record for this sourceatVizieR.
- ^abGiguere, 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.S2CID56121568.
- ^abcdeGhezzi, 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,S2CID119206634.
- ^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.S2CID14454598.
- ^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.S2CID118406833.
- ^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.S2CID118542104.
- ^Agnew, Matthew T; Maddison, Sarah T; Horner, Jonathan; Kane, Stephen R (June 2019)."Predicting multiple planet stability and habitable zone companions in the TESS era".Monthly Notices of the Royal Astronomical Society.485(4): 4703–4725.arXiv:1901.11297.doi:10.1093/mnras/stz345.Retrieved28 April2020.
- ^Ment, Kristo; et al. (2018)."Radial Velocities from the N2K Project: Six New Cold Gas Giant Planets Orbiting HD 55696, HD 98736, HD 148164, HD 203473, and HD 211810".The Astronomical Journal.156(5). 213.arXiv:1809.01228.Bibcode:2018AJ....156..213M.doi:10.3847/1538-3881/aae1f5.S2CID119243619.
External links
[edit]- "HD 5319".Extrasolar Planets Encyclopaedia.Archived fromthe originalon November 6, 2007.
