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Gliese 649

Gliese 649
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Hercules[1]
Right ascension 16h 58m 08.850s[2]
Declination +25° 44′ 38.97″[2]
Apparent magnitude (V) 9.655[3]
Characteristics
Evolutionary stage Main sequence
Spectral type M1.0V[3]
Apparent magnitude (B) 11.222[1]
Apparent magnitude (R) 8.80[1]
Apparent magnitude (I) 8.000[1]
Apparent magnitude (J) 6.448[3]
Apparent magnitude (H) 5.865[3]
Apparent magnitude (K) 5.624[3]
B−V color index 1.48[3]
V−R color index 0.8
R−I color index 0.8
Astrometry
Radial velocity (Rv)3.76±0.13[2] km/s
Proper motion (μ) RA: −115.314(21) mas/yr[2]
Dec.: −508.087(26) mas/yr[2]
Parallax (π)96.2333 ± 0.0244 mas[2]
Distance33.892 ± 0.009 ly
(10.391 ± 0.003 pc)
Absolute magnitude (MV)9.63[1]
Details
Mass0.524±0.012[4] M☉
Radius0.531±0.012[4] R☉
Luminosity0.04373±0.00045[4] L☉
Surface gravity (log g)4.76±0.04[3] cgs
Temperature3,621+41
−40[4] K
Metallicity [Fe/H]−0.15±0.09[3] dex
Rotation24.89+0.34
−0.35 d[3]
Age2.96±0.51[5] Gyr
Other designations
BD+25 3173, HIP 83043, TYC 2063-00479-1, 2MASS J16580884+2544392[6]
Database references
SIMBADdata
Exoplanet Archivedata
ARICNSdata

Gliese 649 is a small star with an orbiting exoplanet in the constellation Hercules. It has an apparent visual magnitude of 9.7,[3] which is too faint to be seen with the naked eye. The system is located at a distance of 33.9 light years based on parallax, and is drifting further away with a radial velocity of 3.8 km/s.[2]

This is an M-type main-sequence star, a red dwarf, with a stellar classification of M1.0V.[3] It has 52% of the mass of the Sun and 53% of the Sun's girth. In the visible light band, the star is radiating 4.4% of the luminosity of the Sun from its photosphere at an effective temperature of 3,621 K.[4] It is spinning slowly with a rotation period of 24.9 days.[3]

Planetary system

A Saturn-mass planet was detected around the red dwarf star by J. A. Johnson and associates in 2010.[7] It has a minimum mass 32.8% of Jupiter's mass and is located 1.15 astronomical units from its star in eccentric orbit (e=0.3). Assuming a luminosity of 4.5% that of the Sun, the habitable zone is located at 0.21 AU, thus the planet should be as cold as if it were located at 5.5 AU from a Solar-like star. Also accounting for different periastron and apastron positions of 0.8 and 1.49 AU respectively, the planet could likely show seasonal temperature changes.

Debris disk

Using results from the Herschel Space Observatory survey of 21 late-type stars carried out in 2010, a debris disk was discovered between approximately 6 and 30 AU. The disk was not detected at 22μm by NASA's Wide-field Infrared Survey Explorer so therefore it is likely to be below 100 Kelvin and similar to the Kuiper belt. The disk was marginally resolved, appearing very asymmetric, and so is probably consistent with being closer to edge-on, rather than face-on, in its inclination.[8]

The Gliese 649 planetary system[3][8]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b ≥0.258+0.023
−0.022 MJ 		1.112+0.035
−0.037 		600.1±1.7 0.083+0.068
−0.055 		— —
Kuiper belt ~6–~30 AU ~45-90° —

References

  1. ^ a b c d e 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.
  2. ^ a b c d e f 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.
  3. ^ a b c d e f g h i j k l m Pinamonti, M.; Barbato, D.; et al. (June 2023). "The GAPS programme at TNG. XLVI. Deep search for low-mass planets in late-dwarf systems hosting cold Jupiters". Astronomy & Astrophysics. 677. arXiv:2306.04419. Bibcode:2023A&A...677A.122P. doi:10.1051/0004-6361/202346476. S2CID 259095781.
  4. ^ a b c d e Pineda, J. Sebastian; Youngblood, Allison; France, Kevin (September 2021). "The M-dwarf Ultraviolet Spectroscopic Sample. I. Determining Stellar Parameters for Field Stars". The Astrophysical Journal. 918 (1): 23. arXiv:2106.07656. Bibcode:2021ApJ...918...40P. doi:10.3847/1538-4357/ac0aea. S2CID 235435757. 40.
  5. ^ Gaidos, Eric; et al. (April 2023). "The TIME Table: rotation and ages of cool exoplanet host stars". Monthly Notices of the Royal Astronomical Society. 520 (4): 5283–5304. arXiv:2301.12109. Bibcode:2023MNRAS.520.5283G. doi:10.1093/mnras/stad343.
  6. ^ "9 Cet", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2015-12-10.
  7. ^ Johnson, John Asher; et al. (2010). "The California Planet Survey II. A Saturn-Mass Planet Orbiting the M Dwarf Gl649". The Publications of the Astronomical Society of the Pacific. 122 (888): 149–155. arXiv:0912.2730. Bibcode:2010PASP..122..149J. doi:10.1086/651007. S2CID 119254409.
  8. ^ a b Kennedy, Grant M.; et al. (2018). "Kuiper Belt Analogues in Nearby M-type Planet-host Systems". Monthly Notices of the Royal Astronomical Society. 476 (4): 4584–4591. arXiv:1803.02832. Bibcode:2018MNRAS.476.4584K. doi:10.1093/mnras/sty492. S2CID 62879401.

See also
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