HD 5319: Difference between revisions
ref call fix |
m sorting |
||
| Line 110: | Line 110: | ||
[[Category:Planetary systems with two confirmed planets]] |
[[Category:Planetary systems with two confirmed planets]] |
||
[[Category:Durchmusterung objects|BD+00 142]] |
[[Category:Durchmusterung objects|BD+00 142]] |
||
[[Category:2MASS objects| |
[[Category:2MASS objects|J00550140+0047223]] |
||
Revision as of 01:29, 18 May 2021
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Cetus |
| Right ascension | 00h 77m 01.3977s[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 ± 0.0476 mas[1] |
| Distance | 397 ± 2 ly (121.8 ± 0.7 pc) |
| 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 5319 is an 8th magnitude star approximately 319 light years away 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 November 2014. 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] 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±0.29 MJ | 1.57±0.13 | 638.6±1.2 | 0.015±0.016 | — | — |
| c | ≥1.02±0.22 MJ | 1.94±0.16 | 877.0±4.9 | 0.109±0.067 | — | — |
See also
References
- ^ a b c d e Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data 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 source at VizieR.
- ^ a b 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.
- ^ a b c d e 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.
- ^ 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.
- ^ 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.
{{cite journal}}: CS1 maint: unflagged free DOI (link) - ^ 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.
{{cite journal}}: CS1 maint: unflagged free DOI (link) - ^ 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. doi:10.1093/mnras/stz345. Retrieved 28 April 2020.
- ^ 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.
{{cite journal}}: CS1 maint: unflagged free DOI (link)
External links
- "HD 5319". The Extrasolar Planets Encyclopaedia.
