Astronomy:Omicron Aquilae
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| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Aquila |
| Right ascension | 19h 51m 01.644s[1] |
| Declination | +10° 24′ 56.59″[1] |
| Apparent magnitude (V) | 5.11[2] |
| Characteristics | |
| Spectral type | F8 V + M3 V[3] |
| U−B color index | 1.486[4] |
| B−V color index | 0.55[5] |
| R−I color index | 0.29[citation needed] |
| Astrometry | |
| Radial velocity (Rv) | 0.036±0.0003[6] km/s |
| Proper motion (μ) | RA: +241.713[1] mas/yr Dec.: −136.695[1] mas/yr |
| Parallax (π) | 51.3133 ± 0.0898[1] mas |
| Distance | 63.6 ± 0.1 ly (19.49 ± 0.03 pc) |
| Absolute magnitude (MV) | 3.71[7] |
| Details | |
| ο Aql A | |
| Mass | 1.25±0.01[8] M☉ |
| Radius | 1.48±0.03[4] R☉ |
| Luminosity | 2.79±0.13[4] L☉ |
| Surface gravity (log g) | 4.30±0.02[8] cgs |
| Temperature | 6176±9[8] K |
| Metallicity [Fe/H] | +0.137±0.007[8] dex |
| Rotational velocity (v sin i) | 3[5] km/s |
| Age | 3.30+0.07−0.20[8] Gyr |
| ο Aql B | |
| Mass | 0.33[9] M☉ |
| Radius | 0.37[10] R☉ |
| Luminosity | 0.015[10] L☉ |
| Surface gravity (log g) | 4.86[10] cgs |
| Temperature | 3,338[10] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
Omicron Aquilae is a double star in the equatorial constellation of Aquila. Its name is a Bayer designation that is Latinized from ο Aquilae, and abbreviated Omicron Aql or ο Aql. The brighter component has an apparent visual magnitude of +5.11,[2] which means it is faintly visible to the naked eye in dark suburban skies. The annual parallax shift of this star is 51.3 mas,[1] which is equivalent to a physical distance of 63.6 light-years (19.5 parsecs) from Earth.
The primary component, Omicron Aquilae A, is an F-type main sequence star with a stellar classification of F8 V.[3] It has about 125% of the mass of the Sun[8] and 148% of the Sun's radius. With an age of roughly 3.3 billion years,[8] it appears to spinning at a leisurely rate with a projected rotational velocity of 3 km/s.[5] The outer atmosphere has an effective temperature of 6,123 K,[4] giving it the yellowish-white hue of an F-type star.
In 1998, Omicron Aquilae was one of nine stars identified as experiencing a superflare. The first flare observed from Omicron Aquilae was in 1979, with a magnitude increase of 0.07 and a duration of less than five days. The second occurred in 1980, with a magnitude change of 0.09 and a duration of fifteen days. The energy released during the second flare is estimated as 9×1037 erg.[12]
There is a magnitude 12.67 common proper motion companion located at an angular separation of 22.5 arcseconds along a position angle of 221°. Based upon its matching parallax value, this corresponds to a projected separation of 431 astronomical units. (Hence, the companion is located at this separation or greater.) This is confusingly designated WDS J19510+1025C or ο Aquilae B. It is a small red dwarf star with a stellar classification of M3 V. A third star, a magnitude fainter and slightly closer to the primary, is an optical companion that appears near the primary only through a chance alignment.[3]
References
- ↑ 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.
- ↑ 2.0 2.1 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.
- ↑ 3.0 3.1 3.2 Raghavan, Deepak et al. (September 2010), "A Survey of Stellar Families: Multiplicity of Solar-type Stars", The Astrophysical Journal Supplement 190 (1): 1–42, doi:10.1088/0067-0049/190/1/1, Bibcode: 2010ApJS..190....1R.
- ↑ 4.0 4.1 4.2 4.3 Harada, Caleb K. et al. (June 2024), "Setting the Stage for the Search for Life with the Habitable Worlds Observatory: Properties of 164 Promising Planet-survey Targets", The Astrophysical Journal Supplement Series 272 (2): id. 30, doi:10.3847/1538-4365/ad3e81, Bibcode: 2024ApJS..272...30H.
- ↑ 5.0 5.1 5.2 Takeda, Yoichi et al. (February 2005), "High-Dispersion Spectra Collection of Nearby F--K Stars at Okayama Astrophysical Observatory: A Basis for Spectroscopic Abundance Standards", Publications of the Astronomical Society of Japan 57 (1): 13–25, doi:10.1093/pasj/57.1.13, Bibcode: 2005PASJ...57...13T.
- ↑ Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ Holmberg, J. et al. (July 2009), "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics", Astronomy and Astrophysics 501 (3): 941–947, doi:10.1051/0004-6361/200811191, Bibcode: 2009A&A...501..941H.
- ↑ 8.0 8.1 8.2 8.3 8.4 8.5 8.6 Carvalho-Silva, Gabriela; Meléndez, Jorge; Rathsam, Anne; Shejeelammal, J.; Martos, Giulia; Lorenzo-Oliveira, Diego; Spina, Lorenzo; Ribeiro Alves, Débora (April 2025), "A New Age–Activity Relation For Solar Analogs that Accounts for Metallicity" (in en), The Astrophysical Journal Letters 983 (2): L31, doi:10.3847/2041-8213/adc382, ISSN 2041-8205, Bibcode: 2025ApJ...983L..31C.
- ↑
- ↑ 10.0 10.1 10.2 10.3 Stassun, Keivan G. et al. (2019), "The Revised TESS Input Catalog and Candidate Target List", The Astronomical Journal 158 (4): 138, doi:10.3847/1538-3881/ab3467, Bibcode: 2019AJ....158..138S.
- ↑ "omi Aql". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=omi+Aql.
- ↑ Schaefer, Bradley E. et al. (February 2000), "Superflares on Ordinary Solar-Type Stars", The Astrophysical Journal 529 (2): 1026–1030, doi:10.1086/308325, Bibcode: 2000ApJ...529.1026S.
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