Gliese 687

Gliese 687
Observation data
Epoch J2000      Equinox J2000
Constellation Draco
Right ascension 17h 36m 25.8999s[1]
Declination +68° 20′ 20.909″[1]
Apparent magnitude (V) 9.15[2]
Characteristics
Spectral type M3.5 V[3]
U−B color index 1.06
B−V color index 1.49
Astrometry
Radial velocity (Rv)–23.2[4] km/s
Proper motion (μ) RA: –320.47[1] mas/yr
Dec.: –1269.55[1] mas/yr
Parallax (π)220.86 ± 0.92[1] mas
Distance14.77 ± 0.06 ly
(4.53 ± 0.02 pc)
Absolute magnitude (MV)10.87
Details
Mass0.401 ± 0.040[5] M☉
Radius0.492 ± 0.038[5] R☉
Surface gravity (log g)4.66[5] cgs
Temperature3,095 ± 107[5] K
Metallicity [Fe/H]+0.11 ± 0.20[5] dex
Rotational velocity (v sin i)<2.8[6] km/s
Other designations
BD +68°946, GCTP 4029.00, GJ 687, HIP 86162, LHS 450, LTT 15232, SAO 17568.[2]
Database references
SIMBADdata

Gliese 687, or GJ 687 (Gliese–Jahreiß 687) is a red dwarf in the constellation Draco. This is one of the closest stars to the Sun and lies at an approximate distance of less than 15 light years. Even though it is close by, it has a magnitude of about 9, so it can only be seen through a moderately sized telescope. Gliese 687 has a high proper motion, advancing 1.304 arcseconds per year across the sky. It has a net relative velocity of about 39 km/s.[2] It is known to have a Neptune-mass planet.[7]

Distance

Gliese 687 distance estimates

Source Parallax, mas Distance, pc Distance, ly Distance, Pm Ref.
Woolley et al. (1970) 214±4 4.67±0.09 15.24+0.29
−0.28		 144.2+2.7
−2.6		 [8]
Gliese & Jahreiß (1991) 212.7±2.0 4.7±0.04 15.33+0.15
−0.14		 145.1±1.4 [9]
van Altena et al. (1995) 219.1±1.8 4.56±0.04 14.89±0.12 140.8+1.2
−1.1		 [10]
Perryman et al. (1997) (Hipparcos) 220.85±0.92 4.528±0.019 14.77±0.06 139.7±0.6 [11]
Perryman et al. (1997) (Tycho) 210.60±14.60 4.75+0.35
−0.31		 15.5+1.2
−1		 146.5+10.9
−9.5		 [12]
van Leeuwen (2007) 220.84±0.94 4.528±0.019 14.77±0.06 139.7±0.6 [13]
RECONS TOP100 (2012) 220.47±0.83[note 1] 4.536±0.017 14.79±0.06 140±0.5 [14]

Non-trigonometric distance estimates are marked in italic. The most precise estimate is marked in bold.

Properties

Gliese 687 has about 40% of the Sun's mass and nearly 50% of the Sun's radius. Compared to the Sun, it has a slightly higher proportion of elements with higher atomic numbers than helium.[5] It appears to have a rotation of 60 days and to be somewhat chromospherically active.

It displays no excess of infrared radiation that would indicate orbiting dust.[15] It is known to have a planet, Gliese 687 b, with a mass of 19 Earth masses (which makes it comparable to Neptune), an orbital period of 38.14 days, and a low orbital eccentricity.[7]

X-ray source

Gliese 687 is a solitary red dwarf that emits X-rays.[16]

See also

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 Perryman, M. A. C. et al. (July 1997). "The HIPPARCOS Catalogue". Astronomy & Astrophysics 323: L49–L52. Bibcode:1997A&A...323L..49P.
  2. ↑ 2.0 2.1 2.2 "LHS 450 -- High proper-motion Star". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2009-11-12.
  3. ↑ Endl, Michael; Cochran, William D.; Kürster, Martin; Paulson, Diane B.; Wittenmyer, Robert A.; MacQueen, Phillip J.; Tull, Robert G. (September 2006). "Exploring the Frequency of Close-in Jovian Planets around M Dwarfs". The Astrophysical Journal 649 (1): 436–443. arXiv:astro-ph/0606121. Bibcode:2006ApJ...649..436E. doi:10.1086/506465.
  4. ↑ Evans, D. S. (June 20–24, 1966). "The Revision of the General Catalogue of Radial Velocities". In Alan Henry Batten and John Frederick Heard. Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30. University of Toronto: Academic Press. Bibcode:1967IAUS...30...57E.
  5. ↑ 5.0 5.1 5.2 5.3 5.4 5.5 Berger, D. H. et al. (2006). "First Results from the CHARA Array. IV. The Interferometric Radii of Low-Mass Stars". The Astrophysical Journal 644 (1): 475–483. arXiv:astro-ph/0602105. Bibcode:2006ApJ...644..475B. doi:10.1086/503318.
  6. ↑ Jenkins, J. S.; Ramsey, L. W.; Jones, H. R. A.; Pavlenko, Y.; Gallardo, J.; Barnes, J. R.; Pinfield, D. J. (October 2009). "Rotational Velocities for M Dwarfs". The Astrophysical Journal 704 (2): 975–988. arXiv:0908.4092. Bibcode:2009ApJ...704..975J. doi:10.1088/0004-637X/704/2/975.
  7. ↑ 7.0 7.1 The Lick–Carnegie exoplanet survey: Gliese 687 b: A Neptune-mass planet orbiting a nearby red dwarf
  8. ↑ Woolley R.; Epps E. A.; Penston M. J.; Pocock S. B. (1970). "Woolley 687". Catalogue of stars within 25 parsecs of the Sun. Retrieved 2014-10-22.
  9. ↑ Gliese, W. and Jahreiß, H. (1991). "Gl 687". Preliminary Version of the Third Catalogue of Nearby Stars. Retrieved 2014-10-22.
  10. ↑ Van Altena W. F., Lee J. T., Hoffleit E. D. (1995). "GCTP 4029". The General Catalogue of Trigonometric Stellar Parallaxes (Fourth ed.). Retrieved 2014-10-22.
  11. ↑ Perryman et al. (1997). "HIP 86162". The Hipparcos and Tycho Catalogues. Retrieved 2014-10-22.
  12. ↑ Perryman et al. (1997). "HIP 86162". The Hipparcos and Tycho Catalogues. Retrieved 2014-10-22.
  13. ↑ van Leeuwen F. (2007). "HIP 86162". Validation of the new Hipparcos reduction. Retrieved 2014-10-22.
  14. ↑ "RECONS TOP100". THE ONE HUNDRED NEAREST STAR SYSTEMS brought to you by RECONS (Research Consortium On Nearby Stars). 2012. Retrieved 2014-10-22.
  15. ↑ Gautier, Thomas N., III et al. (September 2007). "Far-Infrared Properties of M Dwarfs". The Astrophysical Journal 667 (1): 527–536. arXiv:0707.0464. Bibcode:2007ApJ...667..527G. doi:10.1086/520667.
  16. ↑ Schmitt JHMM, Fleming TA, Giampapa MS (September 1995). "The X-ray view of the low-mass stars in the solar neighborhood". Ap J. 450 (9): 392–400. Bibcode:1995ApJ...450..392S. doi:10.1086/176149.

Notes

  1. ↑ Weighted parallax based on parallaxes from van Altena et al. (1995) and van Leeuwen (2007).

External links