53 Aquarii

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53 Aquarii
Diagram showing star positions and boundaries of the Aquarius constellation and its surroundings
Cercle rouge 100%.svg

Location of 53 Aquarii (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Aquarius
Right ascension 22h 26m 34.2753s[1]
Declination –16° 44′ 31.697″[1]
Apparent magnitude (V) 5.56[2] (6.35/6.57)[3]
Characteristics
Spectral type G1 V + G5 V Fe–0.8 CH–1[4]
U−B color index +0.09[2]
B−V color index +0.61[2]
Astrometry
Radial velocity (Rv) +2.1[5] km/s
Proper motion (μ) RA: +200.59[1] mas/yr
Dec.: +14.51[1] mas/yr
Parallax (π) 49.50 ± 1.23[1] mas
Distance 66 ± 2 ly
(20.2 ± 0.5 pc)
Absolute magnitude (MV) 4.05[5] (4.94/4.87)[3]
Details
53 Aqr A
Mass 0.99[6] M
Radius 1.11[6] R
Luminosity 1.39[6] L
Surface gravity (log g) 4.46[3] cgs
Temperature 5,922[3] K
Metallicity [Fe/H] –0.10[3] dex
Rotational velocity (v sin i) 8[7] km/s
Age 0.18–0.37[8] Gyr
53 Aqr B
Surface gravity (log g) 4.44[3] cgs
Temperature 5,811[3] K
Metallicity [Fe/H] –0.19[3] dex
Rotational velocity (v sin i) 9[7] km/s
Other designations
f Aquarii, GJ 859, HIP 110778.[9]
53 Aqr A: BD–17 6521, HD 212698, HR 8545, LTT 9026, SAO 165078.
53 Aqr B: BD–17 6520, HD 212697, HR 8544, LTT 9025, SAO 165077.

53 Aquarii is the Flamsteed designation for a binary star [10] system in the equatorial constellation of Aquarius. The combined apparent visual magnitude of the pair is a 5.56,[2] making it just visible to the naked eye in dark suburban skies. Based upon an annual parallax shift of 49.50 milliarcseconds for the first component, this system is located at a distance of approximately 65 light-years (20 parsecs) from Earth.[1]

This is a wide binary star system with a projected separation of 100 astronomical units; indicating that the two stars are at least this distance apart.[6] The primary component is a solar-type main sequence star with a stellar classification of G1 V.[4] It has about 99% of the Sun's mass, 111% of the Sun's radius, and shines with 139% of the luminosity of the Sun.[6] This energy is being emitted from an outer envelope at an effective temperature of 5,922 K,[3] giving it the golden hue of a G-type star.[11] An examination of the primary component with the Spitzer space telescope failed to detect any infrared excess that might otherwise be an indication of a circumstellar debris disk.[6]

The companion is a slightly cooler star with an effective temperature of 5,811 K.[3] It has a stellar classification of G5 V Fe–0.8 CH–1,[4] indicating it is a chemically peculiar G-type main sequence star showing an under-abundance of iron and the molecule CH in its spectrum. As of 2008, it has an angular separation of 1.325 arcseconds along a position angle of 30.9° from the primary.[12]

This system is coeval with the Castor Moving Group of stars that share a common motion through space; hence it is a candidate member of that association. This suggests that the system is young; its estimated age is in the range of 180 to 370 million years, based upon the spectrum and X-ray luminosity, respectively.[8]

References[edit]

  1. ^ a b c d e f van Leeuwen, F. (November 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. ^ a b c d 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 d e f g h i j Pasquini, L.; Liu, Q.; Pallavicini, R. (July 1994), "Lithium abundances of nearby solar-like stars", Astronomy and Astrophysics 287 (1): 191–205, Bibcode:1994A&A...287..191P. 
  4. ^ a b c 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/0603770, Bibcode:2006AJ....132..161G, doi:10.1086/504637. 
  5. ^ a b Nordström, B. et al. (May 2004), "The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ˜14 000 F and G dwarfs", Astronomy and Astrophysics 418: 989–1019, arXiv:astro-ph/0405198, Bibcode:2004A&A...418..989N, doi:10.1051/0004-6361:20035959. 
  6. ^ a b c d e f Plavchan, Peter et al. (June 2009), "New Debris Disks Around Young, Low-Mass Stars Discovered with the Spitzer Space Telescope", The Astrophysical Journal 698 (2): 1068–1094, arXiv:0904.0819, Bibcode:2009ApJ...698.1068P, doi:10.1088/0004-637X/698/2/1068. 
  7. ^ a b 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. 
  8. ^ a b Maldonado, J. et al. (October 2010), "A spectroscopy study of nearby late-type stars, possible members of stellar kinematic groups", Astronomy and Astrophysics 521: A12, arXiv:1007.1132, Bibcode:2010A&A...521A..12M, doi:10.1051/0004-6361/201014948. 
  9. ^ "53 Aqr -- Double or multiple star", SIMBAD Astronomical Object Database (Centre de Données astronomiques de Strasbourg), retrieved 2012-07-14.  See also the children entries.
  10. ^ 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:0806.2878. Bibcode:2008MNRAS.389..869E. doi:10.1111/j.1365-2966.2008.13596.x. 
  11. ^ "The Colour of Stars", Australia Telescope, Outreach and Education (Commonwealth Scientific and Industrial Research Organisation), December 21, 2004, retrieved 2012-01-16. 
  12. ^ Tokovinin, A.; Cantarutti, R. (February 2008), "First Speckle Interferometry at SOAR Telescope with Electron-Multiplication CCD", Publications of the Astronomical Society of the Pacific 120 (864): 170–177, Bibcode:2008PASP..120..170T, doi:10.1086/528809.