Astronomy:Phi Aquarii

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Short description: Star in the constellation Aquarius
Phi Aquarii
Location of φ Aquarii (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Aquarius
Right ascension  23h 14m 19.358s[1]
Declination −06° 02′ 56.42″[1]
Apparent magnitude (V) +4.223[2]
Characteristics
Spectral type M1.5 III[3]
U−B color index +1.897[2]
B−V color index +1.563[2]
Astrometry
Radial velocity (Rv)+2.48±0.32[4] km/s
Proper motion (μ) RA: +36.575[1] mas/yr
Dec.: −195.441[1] mas/yr
Parallax (π)14.3482 ± 0.2594[1] mas
Distance227 ± 4 ly
(70 ± 1 pc)
Absolute magnitude (MV)0.30±0.120[5]
Details
A
Mass1.00±0.03[6] M☉
Radius34.77+1.83−2.04[6] R☉
Luminosity207.7±25.2[6] L☉
Surface gravity (log g)1.5[4] cgs
Temperature3,715±48[6] K
Rotational velocity (v sin i)6.7[4] km/s
Age10.97±0.83[6] Gyr
Other designations
φ Aqr, 90 Aquarii, BD−06°6170, FK5 1607, GC 32346, HD 219215, HIP 114724, HR 8834, SAO 146585, PPM 207311[7]
Database references
SIMBADdata

Phi Aquarii is a binary star[8] system in the equatorial constellation of Aquarius. Its name is a Bayer designation that is Latinized from φ Aquarii, and abbreviated Phi Aqr or φ Aqr. This system is visible to the naked eye as a point of light with a combined apparent visual magnitude of +4.223.[2] Parallax measurements indicate its distance from Earth is approximately 227 light-years (70 pc).[1] It is drifting further away with a radial velocity of +2.5 km/s.[4] The system is positioned 1.05 degrees south of the ecliptic so it is subject to lunar occultations.[9]

This is a spectroscopic binary star system with an estimated period of 2,500 days (6.8 yr).[10] The primary component is an aging red giant star with a stellar classification of M1.5 III.[3] At an estimated age of 11 billion years,[6] it has exhausted the supply of hydrogen at its core and evolved away from the main sequence. The star has the same mass as the Sun,[6] but has expanded to 35 times the Sun's girth.[6] It is radiating 208 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 3,715 K,[6] giving it the reddish hue of an M-type star.[11]

On 6 September 2019, it had a close conjunction (geocentric separation <1') with Neptune.[12] : 167 

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  2. ↑ 2.0 2.1 2.2 2.3 Gutierrez-Moreno, Adelina et al. (1966), "A System of photometric standards", Publications of the Department of Astronomy University of Chile (Publicaciones Universidad de Chile, Department de Astronomy) 1: 1–17, Bibcode: 1966PDAUC...1....1G. 
  3. ↑ 3.0 3.1 Morgan, W. W.; Keenan, P. C. (1973), "Spectral Classification", Annual Review of Astronomy and Astrophysics 11 (1): 29, doi:10.1146/annurev.aa.11.090173.000333, Bibcode: 1973ARA&A..11...29M. 
  4. ↑ 4.0 4.1 4.2 4.3 Massarotti, Alessandro et al. (January 2008), "Rotational and Radial Velocities for a Sample of 761 HIPPARCOS Giants and the Role of Binarity", The Astronomical Journal 135 (1): 209–231, doi:10.1088/0004-6256/135/1/209, Bibcode: 2008AJ....135..209M. 
  5. ↑ Park, Sunkyung et al. (2013), "Wilson-Bappu Effect: Extended to Surface Gravity", The Astronomical Journal 146 (4): 73, doi:10.1088/0004-6256/146/4/73, Bibcode: 2013AJ....146...73P. 
  6. ↑ 6.0 6.1 6.2 6.3 6.4 6.5 6.6 6.7 6.8 Baines, Ellyn K. et al. (2018), "Fundamental Parameters of 87 Stars from the Navy Precision Optical Interferometer", The Astronomical Journal 155 (1): 30, doi:10.3847/1538-3881/aa9d8b, Bibcode: 2018AJ....155...30B. 
  7. ↑ "* phi Aqr". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=%2A+phi+Aqr. 
  8. ↑ 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, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E. 
  9. ↑ White, Nathaniel M.; Feierman, Barry H. (September 1987), "A Catalog of Stellar Angular Diameters Measured by Lunar Occultation", Astronomical Journal 94: 751, doi:10.1086/114513, Bibcode: 1987AJ.....94..751W. 
  10. ↑ Famaey, B. et al. (May 2009), "Spectroscopic binaries among Hipparcos M giants,. I. Data, orbits, and intrinsic variations", Astronomy and Astrophysics 498 (2): 627–640, doi:10.1051/0004-6361/200810698, Bibcode: 2009A&A...498..627F. 
  11. ↑ "The Colour of Stars", Australia Telescope, Outreach and Education (Commonwealth Scientific and Industrial Research Organisation), December 21, 2004, http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html, retrieved 2012-07-02. 
  12. ↑ Meeus, Jan (2002). "Mutual occultations of planets". More Mathematical Astronomy Morsels. Willmann-Bell. pp. 174–185. ISBN 0943396743. https://falakmu.id/khgt/dokumen/More%20mathematical%20astronomy%20morsels%20(Jean%20Meeus)%20(Z-Library).pdf. Retrieved 2025-04-09. 



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