35 Aquarii

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35 Aquarii
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Aquarius
Right ascension  22h 08m 58.99033s[1]
Declination −18° 31′ 10.5372″[1]
Apparent magnitude (V) 5.80[2]
Spectral type B2 III[3]
B−V color index −0.154±0.006[2]
Radial velocity (Rv)−7.2±0.6[2] km/s
Proper motion (μ) RA: −0.102[1] mas/yr
Dec.: −8.110[1] mas/yr
Parallax (π)1.5115 ± 0.1129[1] mas
Distance2,200 ± 200 ly
(660 ± 50 pc)
Mass10.1±1.0[4] M
Luminosity1,622[5] L
Surface gravity (log g)3.31±0.10[6] cgs
Temperature17,400±300[6] K
Rotational velocity (v sin i)10[7] km/s
Age22.5±2.6[4] Myr
Other designations
35 Aqr, BD−19°6227, HD 210191, HIP 109332, HR 8439, SAO 164888, WDS J22091-1829[8]
Database references

35 Aquarii is a single[9] star located roughly 2,200 light years away from the Sun in the zodiac constellation of Aquarius. 35 Aquarii is its Flamsteed designation. It is visible to the naked eye as a dim, blue-white hued star with an apparent visual magnitude of 5.80.[2] This object is moving closer to the Earth with a heliocentric radial velocity of −7 km/s,[2] and is a suspected runaway star that may have been ejected from an open cluster as the result of a binary–binary interaction.[10]

This is a blue giant star with a stellar classification of B2 III;[3], a massive star that has evolved off the main sequence, it is around 22.5[4] million years old with a relatively low projected rotational velocity of 10 km/s.[7] The star has 10[4] times the mass of the Sun and is radiating 1,622[5] times the Sun's luminosity from its photosphere at an effective temperature of 17,400 K.[6]


  1. ^ a b c d e Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 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.
  3. ^ a b Houk, Nancy; Smith-Moore, M. (1978), Michigan catalogue of two-dimensional spectral types for the HD stars, 4, Ann Arbor: Dept. of Astronomy, University of Michigan, Bibcode:1988mcts.book.....H.
  4. ^ a b c d Tetzlaff, N.; et al. (January 2011), "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun", Monthly Notices of the Royal Astronomical Society, 410 (1): 190–200, arXiv:1007.4883, Bibcode:2011MNRAS.410..190T, doi:10.1111/j.1365-2966.2010.17434.x.
  5. ^ a b Simón-Díaz, S.; et al. (2017), "The IACOB project. III. New observational clues to understand macroturbulent broadening in massive O- and B-type stars", Astronomy and Astrophysics, 597: A22, arXiv:1608.05508, Bibcode:2017A&A...597A..22S, doi:10.1051/0004-6361/201628541.
  6. ^ a b c Lyubimkov, Leonid S.; et al. (June 2002), "Surface abundances of light elements for a large sample of early B-type stars - II. Basic parameters of 107 stars", Monthly Notices of the Royal Astronomical Society, 333 (1): 9–26, Bibcode:2002MNRAS.333....9L, doi:10.1046/j.1365-8711.2002.05341.x.
  7. ^ a b Strom, Stephen E.; et al. (2005), "B Star Rotational Velocities in h and χ Persei: A Probe of Initial Conditions during the Star Formation Epoch?", The Astronomical Journal, 129 (2): 809–828, arXiv:astro-ph/0410337, Bibcode:2005AJ....129..809S, doi:10.1086/426748.
  8. ^ "35 Aqr". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-05-16.
  9. ^ Eggleton, P. P.; Tokovinin, A. A. (2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x.
  10. ^ Leonard, Peter J. T.; Duncan, Martin J. (February 1990), "Runaway Stars from Young Star Clusters Containing Initial Binaries. II. A Mass Spectrum and a Binary Energy Spectrum", Astronomical Journal, 99: 608, Bibcode:1990AJ.....99..608L, doi:10.1086/115354.