HD 25171

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HD 25171
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Reticulum
Right ascension 03h 55m 49.44032s[1]
Declination –65° 11′ 12.0363″[1]
Apparent magnitude (V) 7.79[2]
Characteristics
Spectral type F8 V[2]
B−V color index 0.554[2]
Astrometry
Radial velocity (Rv)+42.8[3] km/s
Proper motion (μ) RA: +143.97[1] mas/yr
Dec.: +80.69[1] mas/yr
Parallax (π)18.19 ± 0.45[1] mas
Distance179 ± 4 ly
(55 ± 1 pc)
Absolute magnitude (MV)4.09±0.07[2]
Details
Mass1.09±0.03[2] M☉
Radius1.069±0.041[4] R☉
Luminosity1.89[2] L☉
Surface gravity (log g)4.17±0.1[4] cgs
Temperature6063±50[4] K
Metallicity [Fe/H]−0.11±0.04[2] dex
Rotation14.4±0.6 d[5]
Rotational velocity (v sin i)1.0[2] km/s
Age4.0±1.6[2] Gyr
Other designations
CD–65 199, HD 25171, HIP 9141, SAO 248911, TYC 8874-376-1.
Database references
SIMBADdata

HD 25171 is a star in the southern constellation of Reticulum, the reticle. With an apparent visual magnitude of 7.79,[2] this star is too faint to be viewed with the naked eye. However, it is readily visible through a small telescope from the southern hemisphere. Parallax measurements made during the Hipparcos mission place it at a distance of roughly 179 light-years (55 parsecs) from Earth.[1] It has a planetary companion that was announced December 2009.[6]

Based upon its spectrum, this is an ordinary F-type main sequence star with a stellar classification of 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 its outer atmosphere at an effective temperature of 6,063 K. This gives it the yellow-white hued glow of an F-type star. It appears to be roughly the same age as the Sun; around four billion years.[4][2]

The survey in 2015 have ruled out the existence of any stellar companions at projected distances above 26 astronomical units.[7]

Planetary system[]

The planetary companion was discovered in 2010 with the HARPS instrument, which measured the radial velocity displacement caused by the gravitational perturbation of 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 of Jupiter.[2] The planetary system of HD 25171 is analogous to Solar System in the sense that a gas giant orbiting outside the frost line, far enough to do not destabilize orbits within a circumstellar habitable zone.[8]

The HD 25171 planetary system[6]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b >0.956±0.234 MJ 3.02±0.16 1845±15 0.08±0.06 — —

References[]

  1. ^ a b c d e f 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, S2CID 18759600.
  2. ^ a b c d e f g h i j k l Moutou, 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, S2CID 118696125
  3. ^ Holmberg, 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, S2CID 118577511.
  4. ^ a b c d Buchhave, 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. S2CID 119332645.
  5. ^ 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, S2CID 119215361
  6. ^ a b HD 25171 System
  7. ^ 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. Retrieved 19 June 2020.
  8. ^ 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. S2CID 119232995.
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