81 Cancri

81 Cancri
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cancer
Right ascension 09h 12m 17.54871s[1]
Declination +14° 59′ 45.7382″[1]
Apparent magnitude (V) 6.77
Characteristics
Spectral type G8V[2] / K1V[2] / L8[3][4] / ~L8[4]
B−V color index 0.70
Astrometry
Radial velocity (Rv)49.8252 ± 0.076[5] km/s
Proper motion (μ) RA: -524.40 ± 0.60[1] mas/yr
Dec.: 245.64 ± 0.29[1] mas/yr
Parallax (π)49.11 ± 0.54[1] mas
Distance66.4 ± 0.7 ly
(20.4 ± 0.2 pc)
Orbit[5]
Primary81 Cancri A
Companion81 Cancri B
Period (P)988.058 ± 0.34698 days
Semi-major axis (a)115.4 ± 0.63"
Eccentricity (e)0.433256 ± 0.0034
Inclination (i)124.1 ± 0.64°
Longitude of the node (Ω)317.6 ± 0.46°
Periastron epoch (T)1982.690 ± 0.0040
Argument of periastron (ω)
(secondary)		170.731 ± 0.81°
Argument of periastron (ω)
(primary)		350.731 ± 0.81°
Semi-amplitude (K1)
(primary)		11.4908 ± 0.11 km/s
Semi-amplitude (K2)
(secondary)		12.1317 ± 0.14 km/s
Details
Mass0.89 ± 0.029[5] / 0.85 ± 0.026[5] M☉
Metallicity [Fe/H]-0.14[6] dex
Other designations
Pi1 Cancri, HD 79096, HIP 45170, Gliese 337, HR 3650
Database references
SIMBADdata

81 Cancri (Pi1 Cancri, π1 Cancri) is a stellar system that lies approximately 66 light-years away. The main component of the system is a close binary, while a brown dwarf binary is located at a wide separation.

Components

81 Cancri has long been known to be a binary, both visually and spectroscopically (VBO=SB2O). Their orbit is an eccentric 2.7 year one, resolved by over 100 milli-arcseconds due to a modest separation and close distance. The two components have similar masses and temperatures, with the secondary being only ~0.04 M☉ lower in mass and a few hundred kelvin cooler.

A brown dwarf component in the system was detected in 2001.[3] The source 2MASSW J0912145+145940 (2M0912+14) in the 2MASS catalogue was identified as having a common proper motion with the AB binary, and subsequent observations confirmed the brown dwarf nature of the companion. The new component, 81 Cancri C, was found to have a spectral type of L8, near to the L-T transition. Separated from the primary components by 43 arcseconds and at a distance of 20.4 parsecs, the brown dwarf has a minimum physical separation of approximately 880 AU.

The brown dwarf was found to be about half a magnitude brighter in the JHK bands than expected, compared to others of similar spectral type and known distance. The system was not found to not be particularly young to some confidence, so it was plausible that component C could itself be a close binary not resolved by 2MASS. This was confirmed in 2006[4] as the source was found to be slightly oblong, caused by two components of similar spectral types. These two brown dwarfs, components C and D, have a separation of approximately 11 AU, and their mutual orbit likely takes on order of 150 years due to the small masses involved.

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357.
  2. ↑ 2.0 2.1 Richichi, A. et al. (2000). "New binary stars discovered by lunar occultations. V". Bibcode:2000A&A...361..594R.
  3. ↑ 3.0 3.1 Wilson, J. C. et al. (2001). "Three Wide-Separation L Dwarf Companions from the Two Micron All Sky Survey: Gliese 337C, Gliese 618.1B, and HD 89744B". arXiv:astro-ph/0108424. Bibcode:2001AJ....122.1989W. doi:10.1086/323134.
  4. ↑ 4.0 4.1 4.2 Burgasser, Adam J. et al. (2006). "Multiplicity among Widely Separated Brown Dwarf Companions to Nearby Stars: Gliese 337CD". arXiv:astro-ph/0503379. Bibcode:2005AJ....129.2849B. doi:10.1086/430218.
  5. ↑ 5.0 5.1 5.2 5.3 Pourbaix, D. (2000). "Resolved double-lined spectroscopic binaries: A neglected source of hypothesis-free parallaxes and stellar masses". Bibcode:2000A&AS..145..215P.
  6. ↑ Eggen, Olin J. et al. (1998). "Kinematics and Metallicity of Stars in the Solar Region". Bibcode:1998AJ....115.2397E. doi:10.1086/300350.