HD 25171

Last updated
HD 25171
Observation data
Epoch J2000.0        Equinox J2000.0 (ICRS)
Constellation Reticulum
Right ascension 03h 55m 49.440s [1]
Declination –65° 11′ 12.03″ [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: +144.020  mas/yr [1]
Dec.: +81.550  mas/yr [1]
Parallax (π)17.928 ± 0.0163  mas [4]
Distance 181.9 ± 0.2  ly
(55.78 ± 0.05  pc)
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 (log g)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 (v sin i)1.0 [2]  km/s
Age 4.0±1.6 [2]   Gyr
Other designations
CD–65 199, HD  25171, HIP  9141, SAO  248911 [7]
Database references
SIMBAD data

HD 25171 is a star with an orbiting exoplanet [8] 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 place it at a distance of roughly 182 light-years (56 parsecs ) from Earth. It is drifting further away with a heliocentric radial velocity of +43 km/s. [3]

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. [5] [2]

A survey in 2015 ruled out the existence of any stellar companions at projected distances above 26 astronomical units. [9]

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. [10]

The HD 25171 planetary system [8]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b>0.956±0.234  MJ 3.02±0.161845±150.08±0.06——

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<span class="mw-page-title-main">HD 190007</span> Star in the constellation Aquila

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HD 7449 is a binary star system about 126 light-years way. The primary star, HD 7449 A, is a main-sequence star belonging to the spectral class F9.5. It is younger than the Sun. The primary star is slightly depleted of heavy elements, having 80% of solar abundance.

HD 121056, or HIP 67851, is an aging giant star with a pair of orbiting exoplanets located in the southern constellation of Centaurus. This star is dimly visible to the naked eye with an apparent visual magnitude of 6.17. It is located at a distance of 209 light years from the Sun, based on parallax measurements, and is drifting further away with a radial velocity of 5.6 km/s.

References

  1. 1 2 3 4 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data 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 . S2CID   244398875. Gaia DR3 record for this source at VizieR.
  2. 1 2 3 4 5 6 7 8 9 10 11 12 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. 1 2 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. ↑ 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.
  5. 1 2 3 4 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.
  6. ↑ 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
  7. ↑ "HD 25171". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2023-12-12.
  8. 1 2 HD 25171 System
  9. ↑ 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 . Retrieved 19 June 2020.
  10. ↑ 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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