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Gliese 674

Coordinates: Sky map 17h 28m 39.9463s, −46° 53′ 42.685″
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Gliese 674
Gliese 674 is located in the constellation Ara.
Gliese 674 is located in the constellation Ara.
Gliese 674
Location of Gliese 674 in the constellation Ara

Observation data
Epoch J2000      Equinox J2000
Constellation Ara
Right ascension 17h 28m 39.94558s[1]
Declination –46° 53′ 42.6881″[1]
Apparent magnitude (V) 9.38[2]
Characteristics
Spectral type M3V[3]
U−B color index 1.20[4]
B−V color index 1.553±0.017[2]
R−I color index 1.33[4]
Astrometry
Radial velocity (Rv)−2.904±0.0004[5] km/s
Proper motion (μ) RA: 572.568(40) mas/yr[1]
Dec.: −880.583(27) mas/yr[1]
Parallax (π)219.6463 ± 0.0262 mas[1]
Distance14.849 ± 0.002 ly
(4.5528 ± 0.0005 pc)
Absolute magnitude (MV)11.09[2]
Details
Mass0.353±0.008[6] M☉
Radius0.361+0.012
−0.011[6] R☉
Luminosity0.01575±0.00037[6] L☉
Temperature3,404+59
−57[6] K
Metallicity [Fe/H]−0.30±0.08[6] dex
Rotation32.9±0.1 d[7]
Rotational velocity (v sin i)3.2±1.2[3] km/s
Age0.1–1.0[8] Gyr
Other designations
CD−46°11540, GJ 674, HIP 85523, LFT 1351, LHS 449, LPM 645, LTT 6942[9]
Database references
SIMBADThe star
b
Exoplanet Archivedata
ARICNSdata

Gliese 674 (GJ 674) is a small red dwarf star with an exoplanetary companion in the southern constellation of Ara. It is too faint to be visible to the naked eye, having an apparent visual magnitude of 9.38[2] and an absolute magnitude of 11.09.[2] The system is located at a distance of 14.85 light-years from the Sun based on parallax measurements,[1] but is drifting closer with a radial velocity of −2.9 km/s.[5] It is a candidate member of the 200 million year old Castor stream of co-moving stars.[10]

This is a low-mass M-type main-sequence star with a stellar classification of M3V.[3] The star is weakly active and show star spots on a regular basis. Even low activity red dwarfs can flare, and in 2018 this star was observed emitting a hot ultraviolet flare with a total energy of 5.6×1023 Joules and a duration of a few hours. GJ 674 is at an intermediate stage of spin-down with a rotation period of 33.4 days, suggesting an age of up to a few billion years.[11] It is smaller and less massive than the Sun, and is radiating just 1.6%[8] of the Sun's luminosity from its photosphere at an effective temperature of 3,404 K.[6]

Planetary system

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On January 7, 2007, Bonfils et al. used the HARPS spectrograph in ESO and found an intermediate mass planet orbiting close to the red dwarf star in an eccentric orbit.[8] This system is a promising candidate for detecting radio emission caused by interaction between the planet and the stellar wind.[12] No additional planets were found as of 2024.[13]

The Gliese 674 planetary system[13]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b ≥10.95±0.14 M🜨 0.03867087(15) 4.69502±0.00003 0.242+0.012
−0.013 		— —

See also

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References

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  1. ^ a b c d e 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. ^ 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.
  3. ^ a b c Torres, G. R.; et al. (December 2006). "Search for associations containing young stars (SACY). I. Sample and searching method". Astronomy and Astrophysics. 460 (3): 695–708. arXiv:astro-ph/0609258. Bibcode:2006A&A...460..695T. doi:10.1051/0004-6361:20065602. S2CID 16080025.
  4. ^ a b Koen, C.; et al. (April 21, 2010). "UBV(RI)CJHK observations of Hipparcos-selected nearby stars". Monthly Notices of the Royal Astronomical Society. 403 (4): 1949–1968. Bibcode:2010MNRAS.403.1949K. doi:10.1111/j.1365-2966.2009.16182.x.
  5. ^ a b Soubiran, C.; et al. (2018). "Gaia Data Release 2. The catalogue of radial velocity standard stars". Astronomy and Astrophysics. 616: A7. arXiv:1804.09370. Bibcode:2018A&A...616A...7S. doi:10.1051/0004-6361/201832795. S2CID 52952408.
  6. ^ a b c d e f Pineda, J. Sebastian; et al. (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.
  7. ^ Suárez Mascareño, A.; et al. (September 2015). "Rotation periods of late-type dwarf stars from time series high-resolution spectroscopy of chromospheric indicators". Monthly Notices of the Royal Astronomical Society. 452 (3): 2745–2756. arXiv:1506.08039. Bibcode:2015MNRAS.452.2745S. doi:10.1093/mnras/stv1441. S2CID 119181646.
  8. ^ a b c Bonfils, X.; et al. (2007). "The HARPS search for southern extra-solar planets. X. A m sin i = 11 M🜨 planet around the nearby spotted M dwarf GJ 674". Astronomy and Astrophysics. 474 (1): 293–299. arXiv:0704.0270. Bibcode:2007A&A...474..293B. doi:10.1051/0004-6361:20077068. S2CID 119671420. Archived from the original on 2014-12-28. Retrieved 2013-09-08.
  9. ^ "CD-46 11540". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-11-22.
  10. ^ Caballero, J. A. (May 2010). "Reaching the boundary between stellar kinematic groups and very wide binaries . II. α Librae + KU Librae: a common proper motion system in Castor separated by 1.0 pc". Astronomy and Astrophysics. 514: 7. arXiv:1001.5432. Bibcode:2010A&A...514A..98C. doi:10.1051/0004-6361/200913986. S2CID 118875432. A98.
  11. ^ Froning, C. S.; et al. (February 2019). "A Hot Ultraviolet Flare on the M Dwarf Star GJ 674". The Astrophysical Journal Letters. 871 (2): 6. arXiv:1901.08647. Bibcode:2019ApJ...871L..26F. doi:10.3847/2041-8213/aaffcd. S2CID 119427057. L26.
  12. ^ Vidotto, A. A.; et al. (September 2019). "Can we detect aurora in exoplanets orbiting M dwarfs?". Monthly Notices of the Royal Astronomical Society. 488 (1): 633–644. arXiv:1906.07089. Bibcode:2019MNRAS.488..633V. doi:10.1093/mnras/stz1696.
  13. ^ a b Liebing, F.; Jeffers, S. V.; et al. (September 2024). "RedDots: Limits on habitable and undetected planets orbiting nearby stars GJ 832, GJ 674, and Ross 128". Astronomy & Astrophysics. arXiv:2409.01173.
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Notes

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