Eta Sagittae
  | |
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Sagitta |
| Right ascension | 20h 05m 09.49303s[1] |
| Declination | +19° 59′ 27.8575″[1] |
| Apparent magnitude (V) | +5.09[2] |
| Characteristics | |
| Spectral type | K2 III[3] |
| U−B color index | +0.98[2] |
| B−V color index | +1.06[2] |
| Astrometry | |
| Radial velocity (Rv) | −40.61[4] km/s |
| Proper motion (μ) | RA: +29.63[1] mas/yr Dec.: +79.94[1] mas/yr |
| Parallax (π) | 20.34 ± 0.39 mas[1] |
| Distance | 160 ± 3 ly (49.2 ± 0.9 pc) |
| Absolute magnitude (MV) | 1.61[5] |
| Details[6] | |
| Mass | 1.73±0.09 M☉ |
| Radius | 7.08±0.21 R☉ |
| Luminosity | 26 L☉ |
| Surface gravity (log g) | 3.03±0.10 cgs |
| Temperature | 4,784±3.03 K |
| Metallicity [Fe/H] | +0.10 dex |
| Rotational velocity (v sin i) | 1.3[5] km/s |
| Age | 1.69±0.25 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Eta Sagittae (η Sagittae) is solitary[8] star in the northern constellation of Sagitta. It is faintly visible to the naked eye, having an apparent visual magnitude of +5.09.[2] Based upon an annual parallax shift of 20.34 mas,[1] it is approximately 160 light years distant from the Sun. There is a 61.1% chance that it is a member of the Hyades-Pleiades stream of stars that share a common motion through space.[9]
This is an evolved K-type giant star with a stellar classification of K2 III.[3] At the age of about 1.7 billion years,[6] it is now a red clump star that is generating energy through the fusion of helium at its core.[10] Eta Sagittae has 1.7 times the mass of the Sun and has expanded to seven times the Sun's radius. It is radiating 25.7 times the Sun's luminosity from its photosphere at an effective temperature of 4,784 K.[6]
References
- ^ a b c d e f van Leeuwen, F. (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.
- ^ a b c d Argue, A. N. (1966), "UBV photometry of 550 F, G and K type stars", Monthly Notices of the Royal Astronomical Society, 133: 475–493, Bibcode:1966MNRAS.133..475A, doi:10.1093/mnras/133.4.475.
{{citation}}: CS1 maint: unflagged free DOI (link) - ^ a b Roman, Nancy G. (July 1952), "The Spectra of the Bright Stars of Types F5-K5", Astrophysical Journal, 116: 122, Bibcode:1952ApJ...116..122R, doi:10.1086/145598.
- ^ 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.
- ^ a b Setiawan, J.; et al. (July 2004), "Precise radial velocity measurements of G and K giants. Multiple systems and variability trend along the Red Giant Branch", Astronomy and Astrophysics, 421: 241–254, Bibcode:2004A&A...421..241S, doi:10.1051/0004-6361:20041042-1.
- ^ a b c Maldonado, J.; et al. (June 2013), "The metallicity signature of evolved stars with planets", Astronomy & Astrophysics, 554: 18, arXiv:1303.3418, Bibcode:2013A&A...554A..84M, doi:10.1051/0004-6361/201321082, A84.
- ^ "eta Sge". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-07-11.
{{cite web}}: CS1 maint: postscript (link) - ^ 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.
{{citation}}: CS1 maint: unflagged free DOI (link) - ^ Famaey, B.; et al. (January 2005), "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters", Astronomy and Astrophysics, 430: 165–186, arXiv:astro-ph/0409579, Bibcode:2005A&A...430..165F, doi:10.1051/0004-6361:20041272.
- ^ 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.
