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HD 136118 is a star in the Serpens Caput section of the Serpens constellation. The star is too dim to be readily visible to the naked eye, having an apparent visual magnitude of 6.93.[2] It is located at a distance of 165 light years from the Sun based on parallax,[1] and is drifting closer with a radial velocity of −3 km/s.[2]

HD 136118
Observation data
Epoch J2000      Equinox J2000
Constellation Serpens
Right ascension 15h 18m 55.472266s[1]
Declination −01° 35′ 32.592573″[1]
Apparent magnitude (V) 6.93[2]
Characteristics
Evolutionary stage main sequence[3]
Spectral type F7V[4]
B−V color index 0.553±0.007[2]
Astrometry
Radial velocity (Rv)−3.07±0.13[1] km/s
Proper motion (μ) RA: −123.024±0.031 mas/yr[1]
Dec.: 22.180±0.030 mas/yr[1]
Parallax (π)19.8116 ± 0.0341 mas[1]
Distance164.6 ± 0.3 ly
(50.48 ± 0.09 pc)
Absolute magnitude (MV)3.60[5]
Details
Mass1.84±0.23[6] M☉
Radius1.70±0.02[7] R☉
Luminosity3.717±0.018[7] L☉
Surface gravity (log g)4.08[5] cgs
Temperature6,148+38
−43[7] K
Metallicity [Fe/H]−0.06±0.01[2] dex
Rotational velocity (v sin i)8.5[5] km/s
Age3.5±0.4[2] Gyr
Other designations
BD−01° 3045, HD 136118, HIP 74948, SAO 140452[8]
Database references
SIMBADdata
telescope image
telescope image

This object is an F-type main-sequence star with a stellar classification of F7V.[4] The absolute visual magnitude of this star suggests that it has begun to evolve away from the main sequence.[3] The abundances of the stellar atmosphere are similar to the Sun, and it has only a modest level of chromospheric activity.[9] HD 136118 has 84% more mass compared to the Sun,[6] and is 70%[7] larger in radius. The star is an estimated 3.5[2] billion years old and is spinning with a projected rotational velocity of 8.5 km/s.[5]


Brown dwarf companion


The astronomer Debra Fischer discovered a substellar companion, originally thought to be a very massive exoplanet, which was announced on February 7, 2002.[3] Designated HD 136118 b, it is orbiting the host star with a period of 3.25 years.[9] This object has a minimum mass of 11.9 MJ.[3] On November 25, 2009, its inclination was calculated to be 163.1° and its true mass 42 MJ, classifying it as a brown dwarf.[9] A 2022 study estimated a true mass of 13.1 MJ, closer to the minimum mass.[10]

Due to its high mass the object is likely to be very hot and possibly glowing faintly. The orbit of the object has a semimajor axis of 1.45 astronomical units from the parent star, taking 1,188 days (3.25 years) to complete one eccentric orbit.

The HD 136118 planetary system[9]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b 42+11
−18 MJ		 1.45±0.25[3] 1,188±2 0.34±0.01 163.1±3.0° —

See also



References


  1. Vallenari, A.; et al. (Gaia Collaboration) (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. arXiv:2208.00211. doi:10.1051/0004-6361/202243940. Gaia DR3 record for this source at VizieR.
  2. Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID 119257644.
  3. Fischer, Debra A.; et al. (2002). "Planetary Companions to HD 136118, HD 50554, and HD 106252". Publications of the Astronomical Society of the Pacific. 114 (795): 529–535. Bibcode:2002PASP..114..529F. doi:10.1086/341677. JSTOR 10.1086/341677.
  4. Houk, N.; Swift, C. (1999). "Michigan catalogue of two-dimensional spectral types for the HD Stars". Michigan Spectral Survey. 5. Bibcode:1999MSS...C05....0H.
  5. Luck, R. Earle (January 2017). "Abundances in the Local Region II: F, G, and K Dwarfs and Subgiants". The Astronomical Journal. 153 (1): 19. arXiv:1611.02897. Bibcode:2017AJ....153...21L. doi:10.3847/1538-3881/153/1/21. S2CID 119511744. 21.
  6. Stassun, Keivan G.; et al. (2017). "Accurate Empirical Radii and Masses of Planets and Their Host Stars with Gaia Parallaxes". The Astronomical Journal. 153 (3): 136. arXiv:1609.04389. Bibcode:2017AJ....153..136S. doi:10.3847/1538-3881/aa5df3. S2CID 119219062.
  7. Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  8. "HD 81040". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-07-13.
  9. Martioli, Eder; et al. (January 2010). "The Mass of the Candidate Exoplanet Companion to HD 136118 from Hubble Space Telescope Astrometry and High-Precision Radial Velocities". The Astrophysical Journal. 708 (1): 625–634. arXiv:0911.4645. Bibcode:2010ApJ...708..625M. doi:10.1088/0004-637X/708/1/625. S2CID 119183677.
  10. Feng, Fabo; Butler, R. Paul; et al. (August 2022). "3D Selection of 167 Substellar Companions to Nearby Stars". The Astrophysical Journal Supplement Series. 262 (21). arXiv:2208.12720. Bibcode:2022arXiv220812720F. doi:10.3847/1538-4365/ac7e57.



На других языках

[de] HD 136118

HD 136118 ist ein Hauptreihenstern der Spektralklasse F9 mit einer scheinbaren visuellen Helligkeit von 6,9 mag. Er gehört Serpens Cauda an und ist rund 50 Parsec (also ca. 150 Lichtjahre) vom Sonnensystem entfernt. Der Stern wird von einem Braunen Zwerg umrundet.
- [en] HD 136118


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