1 Aquarii is a binary star[5] system in the zodiac constellation of Aquarius, about 263 light years away from the Sun.[1] 1 Aquarii is the Flamsteed designation. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 5.151,[2] located a degree north of the celestial equator.[5] The system is moving closer to the Earth with a heliocentric radial velocity of −41 km/s.[5]
  | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Aquarius |
| Right ascension | 20h 39m 24.8927s[1] |
| Declination | +00° 29′ 11.155″[1] |
| Apparent magnitude (V) | 5.151[2] |
| Characteristics | |
| Evolutionary stage | horizontal branch[3] |
| Spectral type | K1III[4] |
| U−B color index | 0.936[2] |
| B−V color index | 1.060[2] |
| Astrometry | |
| Radial velocity (Rv) | −40.93(3)[5] km/s |
| Proper motion (μ) | RA: 96.805(120) mas/yr[1] Dec.: −10.140(94) mas/yr[1] |
| Parallax (π) | 12.3852 ± 0.1134 mas[1] |
| Distance | 263 ± 2 ly (80.7 ± 0.7 pc) |
| Absolute magnitude (MV) | 0.77[6] |
| Orbit[5] | |
| Primary | 1 Aquarii A |
| Companion | 1 Aquarii B |
| Period (P) | 1966.7±2.9 days |
| Eccentricity (e) | 0.368±0.009 |
| Periastron epoch (T) | 54740±7 |
| Argument of periastron (ω) (secondary) | 150.7±1.6° |
| Semi-amplitude (K1) (primary) | 3.24±0.04 km/s |
| Details | |
| Mass | 1.50±0.43[7] M☉ |
| Radius | 11[8] R☉ |
| Luminosity | 53.7[8] L☉ |
| Surface gravity (log g) | 2.63±0.11[7] cgs |
| Temperature | 4715±15[9] K |
| Metallicity | −0.12[6] |
| Rotational velocity (v sin i) | 1.8[6] km/s |
| Age | 1.26[7] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Systematic observation for determining the orbit of this system began in 2002, some eighty years following the first radial velocity measurements. It is a single-lined spectroscopic binary with an orbital period of 5.385 yr and an eccentricity of 0.368.[5] The visible component is an aging giant star with a stellar classification of K1III.[4] At the age of 1.26[7] billion years old it is a red clump giant, which indicates it is on the horizontal branch and is generating energy through helium fusion at its core.[3] The star has 1.5[7] times the mass of the Sun and has expanded to 11[8] times the Sun's radius. It is radiating 53.7[8] times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,715 K.[9]
The mass of the companion appears small, suggesting a red dwarf no higher than class M5.[5] In addition to the spectroscopic companion there are two faint optical companions that have no physical relation to 1 Aqr.[11]
Etymology
edit1 Aquarii was known to the ancients as al-sa'd al-malik, or "the lucky star of the king." Interpreting the unexpressed Arabic vowels, al-sa'd al-mulk, gives an alternate translation of "the lucky star of the kingdom." In English, the name is Sadalmelik (or Sadalmelek), although rarely used today.[12][13]
References
edit- ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b c d Cousins, A. W. J. (1984). "UBV Photometry of Equatorial Stars". South African Astronomical Observatory Circulars. 8: 69–84. Bibcode:1984SAAOC...8...69C.
- ^ a b Alves, David R. (August 2000), "K-Band Calibration of the Red Clump Luminosity", The Astrophysical Journal, 539 (2): 732–741, arXiv:astro-ph/0003329, Bibcode:2000ApJ...539..732A, doi:10.1086/309278, S2CID 16673121.
- ^ a b Roman, Nancy G. (1952). "The Spectra of the Bright Stars of Types F5-K5". Astrophysical Journal. 116: 122–143. Bibcode:1952ApJ...116..122R. doi:10.1086/145598.
- ^ a b c d e f g Griffin, R. F. (2014). "Spectroscopic binary orbits from photoelectric radial velocities. Paper 239: HD 134169, HD 176526, 1 Aquarii, and HD 219420". The Observatory. 134: 316–339. Bibcode:2014Obs...134..316G.
- ^ a b c Pace, G.; Pasquini, L.; Ortolani, S. (2003). "The Wilson-Bappu effect: A tool to determine stellar distances". Astronomy and Astrophysics. 401 (3): 997–1008. arXiv:astro-ph/0301637. Bibcode:2003A&A...401..997P. doi:10.1051/0004-6361:20030163. S2CID 17029463.
- ^ a b c d e Feuillet, Diane K.; Bovy, Jo; Holtzman, Jon; Girardi, Léo; MacDonald, Nick; Majewski, Steven R.; Nidever, David L. (2016). "Determining Ages of APOGEE Giants with Known Distances". The Astrophysical Journal. 817 (1): 40. arXiv:1511.04088. Bibcode:2016ApJ...817...40F. doi:10.3847/0004-637X/817/1/40. S2CID 118675933.
- ^ a b c d 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, Bibcode:2008AJ....135..209M, doi:10.1088/0004-6256/135/1/209, S2CID 121883397
- ^ a b Luck, R. Earle (2015). "Abundances in the Local Region. I. G and K Giants". Astronomical Journal. 150 (3). 88. arXiv:1507.01466. Bibcode:2015AJ....150...88L. doi:10.1088/0004-6256/150/3/88. S2CID 118505114.Vizier catalog entry
- ^ "11 Per". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-03-28.
- ^ Mason, B. D.; et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal, 122 (6): 3466–3471, Bibcode:2001AJ....122.3466M, doi:10.1086/323920.
- ^ A Llnguist's Angle on the Star of Bethlehem — i.e. α Aquarii; Coates, Richard; Astronomy & Geophysics, Volume 49, Issue 5; (01 October 2008); Pp. 5.27–5.32; https://doi.org/10.1111/j.1468-4004.2008.49527.x
- ^ Star Names; Arecibo Observatory website; mod.: Steve Gibson; accessed March 2019