Astronomy:HD 141399

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Short description: Star in the constellation Boötes

Coordinates: Sky map 15h 46m 53.8135s, +46° 59′ 10.5407″

HD 141399
270px
Habitable zone in the HD 141399 system[1]
Observation data
Equinox J2000.0]] (ICRS)
Constellation Boötes[2]
Right ascension  15h 46m 53.8132s[3]
Declination +46° 59′ 10.543″[3]
Apparent magnitude (V) 7.20[4]
Characteristics
Evolutionary stage subgiant[3]
Spectral type K0[5]
B−V color index 0.73±0.04[6]
Astrometry
Radial velocity (Rv)−21.9±0.2[3] km/s
Proper motion (μ) RA: −108.119[3] mas/yr
Dec.: +6.040[3] mas/yr
Parallax (π)26.9888 ± 0.0146[3] mas
Distance120.85 ± 0.07 ly
(37.05 ± 0.02 pc)
Absolute magnitude (MV)+4.4[7]
Details
Mass1.09±0.08[8] M☉
Radius1.46±0.15[9] R☉
Luminosity1.59±0.39[9] L☉
Surface gravity (log g)4.24±0.05[8] cgs
Temperature5,602±34[8] K
Metallicity [Fe/H]0.36±0.03[8] dex
Rotation49±12[6]
Rotational velocity (v sin i)2.9±1.0[6] km/s
Age7.23[10] Gyr
Other designations
BD+47 2267, HIP 77301, TYC 3490-928-1, GSC 03490-00928, 2MASS J15465382+4659105[11]
Database references
SIMBADdata

HD 141399 is a K-type subgiant star 121 light-years away in the constellation of Boötes. Its surface temperature is 5602 K. HD 141399 is enriched in heavy elements compared to the Sun, with a metallicity Fe/H index of 0.36±0.03.[8] The star has very low starspot activity.[6]

Planetary system

In 2014, four planets orbiting HD 141399 were discovered by the radial velocity method.[9] Planet HD 141399c is possibly located within the habitable zone.[6] The planetary orbits are close to high-order mean-motion resonance[12] and closely conform to the Titius–Bode law. Two additional planets, one with a period of 462.9 days, are suspected by analogy with the orbits of the Solar System planets.[13] The planetary orbits around HD 141399 are expected to "jump" periodically on a timescale of a few million years between several quasi-stable configurations due to planet-planet interactions.[12] HD 141399 is one of only two known planetary systems consisting of at least four massive gas giants (the other is the system of planets around the young star HR 8799).[14]

The HD 141399 planetary system[6]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b 0.451±0.030 MJ 0.415±0.011 94.44±0.05 0.04±0.02 — —
c 1.33±0.08 MJ 0.689±0.02 201.99±0.08 0.048±0.009 — —
d 1.18±0.08 MJ 2.09±0.06 1069.8±6.7 0.074±0.025 — —
e 0.66±0.10 MJ 5.0±1.5 3370±90 <0.1 — —

References

  1. ↑ Kane, Stephen R. (2023). "Surrounded by Giants: Habitable Zone Stability within the HD 141399 System". The Astronomical Journal 166 (5). doi:10.3847/1538-3881/acfb01. Bibcode: 2023AJ....166..187K. 
  2. ↑ Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A. 
  3. ↑ 3.0 3.1 3.2 3.3 3.4 3.5 3.6 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  4. ↑ Soubiran, C. et al. (2018). "Gaia Data Release 2. The catalogue of radial velocity standard stars". Astronomy and Astrophysics 616. doi:10.1051/0004-6361/201832795. Bibcode: 2018A&A...616A...7S. 
  5. ↑ Cannon, A. J.; Pickering, E. C. (1993). "VizieR Online Data Catalog: Henry Draper Catalogue and Extension (Cannon+ 1918-1924; ADC 1989)". Vizier Online Data Catalog. Bibcode: 1993yCat.3135....0C. 
  6. ↑ 6.0 6.1 6.2 6.3 6.4 6.5 Hébrard, G.; Arnold, L.; Forveille, T.; Correia, A. C. M.; Laskar, J.; Bonfils, X.; Boisse, I.; Díaz, R. F. et al. (1 April 2016). "The SOPHIE search for northern extrasolar planets. X. Detection and characterization of giant planets by the dozen". Astronomy and Astrophysics 588: A145. doi:10.1051/0004-6361/201527585. ISSN 0004-6361. Bibcode: 2016A&A...588A.145H. 
  7. ↑ Boro Saikia, S.; Marvin, C. J.; Jeffers, S. V.; Reiners, A.; Cameron, R.; Marsden, S. C.; Petit, P.; Warnecke, J. et al. (2018). "Chromospheric activity catalogue of 4454 cool stars. Questioning the active branch of stellar activity cycles". Astronomy and Astrophysics 616. doi:10.1051/0004-6361/201629518. Bibcode: 2018A&A...616A.108B. 
  8. ↑ 8.0 8.1 8.2 8.3 8.4 Sousa, S. G.; Adibekyan, V.; Delgado-Mena, E.; Santos, N. C.; Andreasen, D. T.; Ferreira, A. C. S.; Tsantaki, M.; Barros, S. C. C. et al. (2018), "SWEET-Cat updated", Astronomy & Astrophysics 620: A58, doi:10.1051/0004-6361/201833350, Bibcode: 2018A&A...620A..58S 
  9. ↑ 9.0 9.1 9.2 Vogt, Steven S.; Butler, R. Paul; Rivera, Eugenio J.; Kibrick, Robert; Burt, Jennifer; Hanson, Russell; Meschiari, Stefano; Henry, Gregory W. et al. (2014), "A Four-Planet System Orbiting the K0V Star Hd 141399", The Astrophysical Journal 787 (2): 97, doi:10.1088/0004-637X/787/2/97, Bibcode: 2014ApJ...787...97V 
  10. ↑ Tejada Arevalo, Roberto A.; Winn, Joshua N.; Anderson, Kassandra R. (2021). "Further Evidence for Tidal Spin-up of Hot Jupiter Host Stars". The Astrophysical Journal 919 (2): 138. doi:10.3847/1538-4357/ac1429. Bibcode: 2021ApJ...919..138T. 
  11. ↑ "HD 141399". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+141399. 
  12. ↑ 12.0 12.1 Agnew, Matthew T.; Maddison, Sarah T.; Horner, Jonathan (2018), "Prospecting for exo-Earths in multiple planet systems with a gas giant", Monthly Notices of the Royal Astronomical Society 481 (4): 4680–4697, doi:10.1093/mnras/sty2509 
  13. ↑ Allen, Christine; Cordero-Tercero, Guadalupe; Lara, Patricia (2020), "The reliability of the Titius–Bode relation and its implications for the search for exoplanets", Publications of the Astronomical Society of Japan 72 (2), doi:10.1093/pasj/psz146 
  14. ↑ Staff News (2023-10-31). "Giant Exoplanets Are Potential 'Agents of Chaos' in Multiplanet Systems, Astronomers Say | Sci.News" (in en-US). https://www.sci.news/astronomy/giant-exoplanets-12407.html. 



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