Astronomy:HIP 57274
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Ursa Major |
| Right ascension | 11h 44m 40.9643s[1] |
| Declination | +30° 57′ 33.4509″[1] |
| Apparent magnitude (V) | 8.96[2] |
| Characteristics | |
| Spectral type | K5 V[2] |
| U−B color index | +1.06[3] |
| B−V color index | +1.111±0.016[4] |
| Astrometry | |
| Radial velocity (Rv) | +29.76±0.35[1] km/s |
| Proper motion (μ) | RA: −27.069±0.081[1] mas/yr Dec.: −381.708±0.079[1] mas/yr |
| Parallax (π) | 38.6381 ± 0.0499[1] mas |
| Distance | 84.4 ± 0.1 ly (25.88 ± 0.03 pc) |
| Absolute magnitude (MV) | 6.89[2] |
| Details[2] | |
| Mass | 0.73±0.05 M☉ |
| Radius | 0.68±0.03 R☉ |
| Luminosity | 0.19±0.01 L☉ |
| Surface gravity (log g) | 4.71±0.1 cgs |
| Temperature | 4,640±100 K |
| Metallicity [Fe/H] | +0.09±0.05 dex |
| Rotation | 45 d |
| Rotational velocity (v sin i) | 0.5±0.5 km/s |
| Age | 7.87±5 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| ARICNS | data |
HIP 57274 is a star in the northern circumpolar constellation of Ursa Major with a system of three planets.[2] It is invisible to the naked eye, having an apparent visual magnitude of 8.96.[2] The distance to this system is 84.4 light years based on stellar parallax, and it is drifting further away with a radial velocity of +30 km/s.[1] The star has a relatively high rate of proper motion, traversing the celestial sphere at the rate of 0.382 arcsecond/year.[6]
This is an ordinary K-type main-sequence star with a stellar classification of K5V.[2] It appears to be older than the Sun with an age of roughly eight billion years and is spinning slowly with a projected rotational velocity of under 1 km/s. The star has 73% of the mass of the Sun and 68% of the Sun's radius. The abundance of elements heavier than helium is about the same or slightly higher than in the Sun. The star is radiating just 19% of the luminosity of the Sun from its photosphere at an effective temperature of 4,640 K.
Planetary system
The three exoplanets orbiting HIP 57274 were discovered by the radial velocity method in 2011, all of them having mass significantly greater than the Earth.[2] A 2014 search for planetary transits was unsuccessful.[7] The planetary orbits are possibly highly variable, being strongly affected by mean motion resonances.[8] The most stable region for a hypothetical super-earth within the star's habitable zone would be an orbit inside 0.37–0.56 astronomical unit|AU from the host star.[8]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥11.6±1.3 M⊕ | 0.0713±0.00163 | 8.1352±0.004 | 0.187±0.10 | — | — |
| c | ≥0.41±0.01 MJ | 0.1778±0.0041 | 32.03±0.02 | 0.05±0.02 | — | — |
| d | ≥0.53±0.03 MJ | 1.007±0.027 | 431.7±8.5 | 0.27±0.05 | — | — |
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 2.7 2.8 Fischer, Debra A. et al. (2012). "M2K. II. A Triple-planet System Orbiting HIP 57274". The Astrophysical Journal 745 (1): 21. doi:10.1088/0004-637X/745/1/21. Bibcode: 2012ApJ...745...21F.
- ↑ Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Catalogue of Eggen's UBV Data. Bibcode: 1986EgUBV........0M.
- ↑ Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A.
- ↑ "BD+31 2290". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=BD%2B31+2290.
- ↑ Lépine, Sébastien; Shara, Michael M. (March 2005). "A Catalog of Northern Stars with Annual Proper Motions Larger than 0.15" (LSPM-NORTH Catalog)". The Astronomical Journal 129 (3): 1483–1522. doi:10.1086/427854. Bibcode: 2005AJ....129.1483L.
- ↑ Kammer, J. A. et al. (February 2014). "A Spitzer Search for Transits of Radial Velocity Detected Super-Earths". The Astrophysical Journal 781 (2): 6. doi:10.1088/0004-637X/781/2/103. 103. Bibcode: 2014ApJ...781..103K.
- ↑ 8.0 8.1 8.2 Elser, S. et al. (2013), "Super Earths and Dynamical Stability of Planetary Systems: First Parallel GPU Simulations Using GENGA", Monthly Notices of the Royal Astronomical Society 433 (3): 2194–2205, doi:10.1093/mnras/stt883, Bibcode: 2013MNRAS.433.2194E
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