94 Aquarii

From Wikipedia, the free encyclopedia
Jump to: navigation, search
94 Aquarii
Observation data
Epoch J2000      Equinox J2000
Constellation Aquarius
Right ascension 23h 19m 06.66907s[1]
Declination –13° 27′ 30.8023″[1]
Apparent magnitude (V) 5.19 / 7.52[2]
Characteristics
94 Aqr A
Spectral type G8.5 IV[3] + K V[4]
U−B color index +0.42[2]
B−V color index +0.79[2]
94 Aqr B
Spectral type K2 V[3]
U−B color index +0.60[2]
B−V color index +0.88[2]
Astrometry
Radial velocity (Rv) +10.8[5] km/s
Proper motion (μ) RA: +267.23[1] mas/yr
Dec.: −46.21[1] mas/yr
Parallax (π) 47.35 ± 2.47[1] mas
Distance 69 ± 4 ly
(21 ± 1 pc)
Orbit[5]
Primary 94 Aqr Aa
Companion 94 Aqr Ab
Period (P) 2323.6 ± 10.7 days
Eccentricity (e) 0.082 ± 0.06
Periastron epoch (T) JD 2429308.4 ± 22
Argument of periastron (ω)
(secondary)
225.7 ± 44.5°
Semi-amplitude (K1)
(primary)
+5.9 ± 0.37 km/s
Details
94 Aqr Aa
Mass 1.29[4] M
Surface gravity (log g) 3.88[6] cgs
Temperature 5,461[6] K
Metallicity [Fe/H] +0.23[6] dex
Rotational velocity (v sin i) 8[7] km/s
94 Aqr Ab
Mass 0.85 or 0.91[4] M
Temperature 4,670 or 4,970[4] K
94 Aqr B
Surface gravity (log g) 4.54[4] cgs
Temperature 5,136[4] K
Metallicity [Fe/H] +0.24[4] dex
Other designations
BD−14 6448, GJ 894.2, HD 219834, HIP 115126, HR 8866, SAO 165625.[8]
Database references
SIMBAD data

94 Aquarii (abbreviated 94 Aqr) is a triple star[5] system in the equatorial constellation of Aquarius. 94 Aquarii is the Flamsteed designation. The brightest member has an apparent visual magnitude of 5.19,[2] making it visible to the naked eye. An annual parallax shift of 47.35 milliarcseconds yields a distance estimate of around 69 light-years (21 parsecs) from Earth.[1]

The inner pair of this triple star system form a spectroscopic binary with an orbital period of 2323.6 days (6.36 years), a low orbital eccentricity of 0.08,[5] and a combined visual magnitude of 5.19.[1] The primary component of this pair has a stellar classification of G8.5 IV,[6] with the luminosity class of IV indicating this is a subgiant star. At an angular separation of 13.0 arcseconds from this pair is a magnitude 7.52[1] K-type main sequence star with a classification of K2 V.[3]

See also[edit]

References[edit]

  1. ^ a b c d e f g h van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752Freely accessible, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357. 
  2. ^ a b c d e f Nicolet, B. (1978), "Photoelectric photometric Catalogue of homogeneous measurements in the UBV System", Astronomy and Astrophysics Supplement Series, 34: 1–49, Bibcode:1978A&AS...34....1N. 
  3. ^ a b c Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv:0806.2878Freely accessible, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x. 
  4. ^ a b c d e f g Fuhrmann, Klaus (February 2008). "Nearby stars of the Galactic disc and halo - IV". Monthly Notices of the Royal Astronomical Society. 384 (1): 173–224. Bibcode:2008MNRAS.384..173F. doi:10.1111/j.1365-2966.2007.12671.x. 
  5. ^ a b c d Sarma, M. B. K. (January 1962), "The Orbit of the Spectroscopic Binary 94 Aquarii", Astrophysical Journal, 135: 301, Bibcode:1962ApJ...135..301S, doi:10.1086/147268. 
  6. ^ a b c d Gray, R. O.; et al. (July 2006), "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 parsecs: The Northern Sample I", The Astronomical Journal, 132 (1): 161–170, arXiv:astro-ph/0603770Freely accessible, Bibcode:2006AJ....132..161G, doi:10.1086/504637. 
  7. ^ Bernacca, P. L.; Perinotto, M. (1970), "A catalogue of stellar rotational velocities", Contributi Osservatorio Astronomico di Padova in Asiago, 239 (1), Bibcode:1970CoAsi.239....1B. 
  8. ^ "* 94 Aqr". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2012-07-17. 

External links[edit]