HD 25171
| Observation data EpochJ2000.0EquinoxJ2000.0(ICRS) | |
|---|---|
| Constellation | Reticulum |
| Right ascension | 03h55m49.440s[1] |
| Declination | –65° 11′ 12.03″[1] |
| Apparent magnitude(V) | 7.79[2] |
| Characteristics | |
| Spectral type | F8 V[2] |
| B−Vcolor index | 0.554[2] |
| Astrometry | |
| Radial velocity(Rv) | +42.8[3]km/s |
| Proper motion(μ) | RA:+144.020mas/yr[1] Dec.:+81.550mas/yr[1] |
| Parallax(π) | 17.928 ± 0.0163mas[4] |
| Distance | 181.9 ± 0.2ly (55.78 ± 0.05pc) |
| Absolute magnitude(MV) | 4.09±0.07[2] |
| Details | |
| Mass | 1.09±0.03[2]M☉ |
| Radius | 1.069±0.041[5]R☉ |
| Luminosity | 1.89[2]L☉ |
| Surface gravity(logg) | 4.17±0.1[5]cgs |
| Temperature | 6,063±50[5]K |
| Metallicity[Fe/H] | −0.11±0.04[2]dex |
| Rotation | 14.4±0.6 d[6] |
| Rotational velocity(vsini) | 1.0[2]km/s |
| Age | 4.0±1.6[2]Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 25171is astarwith an orbitingexoplanet[8]in the southernconstellationofReticulum,the reticle. With anapparent visual magnitudeof 7.79,[2]this star is too faint to be viewed with thenaked eye.However, it is readily visible through a smalltelescopefrom thesouthern hemisphere.Parallaxmeasurements place it at a distance of roughly 182light-years(56parsecs) fromEarth.It is drifting further away with a heliocentricradial velocityof +43 km/s.[3]
Based upon itsspectrum,this is an ordinaryF-type main sequence starwith astellar classificationof F8 V. It is slightly larger than the Sun, with 9% more mass and an 7% greater radius. As such, it is radiating 189% of the Sun's luminosity from itsouter atmosphereat aneffective temperatureof 6,063 K. This gives it the yellow-white hued glow of anF-type star.It appears to be roughly the same age as the Sun; around four billion years.[5][2]
A survey in 2015 ruled out the existence of any stellar companions at projected distances above 26astronomical units.[9]
Planetary system
[edit]The planetary companion was discovered in 2010 with theHARPSinstrument, which measured theradial velocitydisplacement caused by thegravitational perturbationof the star by the planet. This data provided an orbital period of 1,845 days and set a lower bound of the planet's mass at 95% of the mass ofJupiter.[2]The planetary system of HD 25171 is analogous to Solar System in the sense that a gas giant orbiting outside thefrost line,far enough to do not destabilize orbits within a circumstellarhabitable zone.[10]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | >0.956±0.234MJ | 3.02±0.16 | 1845±15 | 0.08±0.06 | — | — |
References
[edit]- ^abcVallenari, A.; et al. (Gaia collaboration) (2023)."GaiaData Release 3. Summary of the content and survey properties ".Astronomy and Astrophysics.674:A1.arXiv:2208.00211.Bibcode:2023A&A...674A...1G.doi:10.1051/0004-6361/202243940.S2CID244398875. Gaia DR3 record for this sourceatVizieR.
- ^abcdefghijklMoutou, Claire; Mayor, Michel; Lo Curto, Gaspare; Ségransan, Damien; Udry, Stéphane; Bouchy, François; Benz, Willy; Lovis, Christophe; Naef, Dominique; Pepe, Francesco; Queloz, Didier; Santos, Nuno C.; Sousa, Sérgio Gonçalves (2010),The HARPS search for southern extra-solar planets: XXVI: Seven new planetary systems,arXiv:1012.3830,doi:10.1051/0004-6361/201015371,S2CID118696125
- ^abHolmberg, J.; Nordstrom, B.; Andersen, J. (July 2009), "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics",Astronomy and Astrophysics,501(3): 941–947,arXiv:0811.3982,Bibcode:2009A&A...501..941H,doi:10.1051/0004-6361/200811191,S2CID118577511.
- ^van Leeuwen, F. (November 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,S2CID18759600.
- ^abcdBuchhave, Lars A.; Bitsch, Bertram; Johansen, Anders; Latham, David W.; Bizzarro, Martin; Bieryla, Allyson; Kipping, David M. (2018)."Jupiter Analogs Orbit Stars with an Average Metallicity Close to That of the Sun".The Astrophysical Journal.856(1): 37.arXiv:1802.06794.Bibcode:2018ApJ...856...37B.doi:10.3847/1538-4357/aaafca.S2CID119332645.
- ^ Suárez Mascareño, A.; Rebolo, R.; González Hernández, J. I.; Esposito, M. (2017), "Characterisation of the radial velocity signal induced by rotation in late-type dwarfs",Monthly Notices of the Royal Astronomical Society,468(4): 4772–4781,arXiv:1703.08884,Bibcode:2017MNRAS.468.4772S,doi:10.1093/mnras/stx771,S2CID119215361
- ^"HD 25171".SIMBAD.Centre de données astronomiques de Strasbourg.Retrieved2023-12-12.
- ^abHD 25171 System
- ^Mugrauer, M.; Ginski, C. (12 May 2015)."High-contrast imaging search for stellar and substellar companions of exoplanet host stars".Monthly Notices of the Royal Astronomical Society.450(3): 3127–3136.Bibcode:2015MNRAS.450.3127M.doi:10.1093/mnras/stv771.hdl:1887/49340.Retrieved19 June2020.
- ^Agnew, Matthew T.; Maddison, Sarah T.; Horner, Jonathan (2018)."Properties of the single Jovian planet population and the pursuit of Solar system analogues".Monthly Notices of the Royal Astronomical Society.477(3): 3646–3658.arXiv:1804.06547.Bibcode:2018MNRAS.477.3646A.doi:10.1093/mnras/sty868.S2CID119232995.
