Short description: Binary star in the constellation Aquarius
ψ3 Aquarii
Location of ψ 3 Aquarii (circled) |
Observation data
Equinox J2000.0]] (ICRS)
|
| Constellation
|
Aquarius[1]
|
| Right ascension
|
23h 18m 57.677s[2]
|
| Declination
|
−09° 36′ 38.70″[2]
|
| Apparent magnitude (V)
|
4.98[3]
|
| Characteristics
|
| Evolutionary stage
|
Main sequence[4]
|
| Spectral type
|
A0 V[5]
|
| U−B color index
|
−0.02
|
| B−V color index
|
−0.02[3]
|
| Astrometry |
|---|
|
|---|
| Radial velocity (Rv) | −10[6] km/s |
| Proper motion (μ) | RA: +44.346[2] mas/yr
Dec.: −7.951[2] mas/yr |
| Parallax (π) | 14.1132 ± 0.1253[2] mas |
| Distance | 231 ± 2 ly
(70.9 ± 0.6 pc) |
| Absolute magnitude (MV) | +0.47[1] |
|
|---|
| Details |
|---|
| A |
|---|
| Mass | 2.67±0.04[4] M☉ |
| Radius | 2[7] R☉ |
| Luminosity | 72.9+6.0−5.5[4] L☉ |
| Surface gravity (log g) | 4.2±0.14[8] cgs |
| Temperature | 9,931+69−68[4] K |
| Rotational velocity (v sin i) | 144[4] km/s |
| Age | 284+38−79[8] Myr |
| B |
|---|
| Mass | 0.8±0.02[8] M☉ |
| Temperature | 4,943±91[8] K |
| Other designations |
|---|
Psi3 Aqr, ψ3 Aqr, 95 Aquarii, BD−10 6094, FK5 1609, GC 32459, HD 219832, HIP 115115, HR 8865, SAO 146635, PPM 207410, ADS 16671, WDS J23190-0937A[9] |
| Database references |
|---|
| SIMBAD | data |
Psi3 Aquarii is a visual binary star[10] system in the constellation of Aquarius. Its name is a Bayer designation that is Latinized from ψ3 Aquarii, and abbreviated Psi3 Aqr or ψ3 Aqr. The pair have an apparent visual magnitude of 4.98,[3] which is bright enough to be seen with the naked eye. Parallax measurements give a distance estimate of roughly 262 light-years (80 parsecs),[11] but it is drifting closer with a radial velocity of −10 km/s.[6]
The main component of this system is an A-type main sequence star with a stellar classification of A0 V.[5] It has 2.7[4] times the mass and double the radius of the Sun. The star is radiating 73[4] times as much luminosity as the Sun from its photosphere at an effective temperature of 9,931 K. It is around 284[8] million years old and has a high rate of spin with a projected rotational velocity of 144 km/s.[4]
Its companion is an 9th magnitude star at an angular separation of 1.5 arcseconds from the primary.[12] This system is an X-ray source with a luminosity of 8.34×1029 erg·s−1. This radiation most likely comes from the companion star.[10]
References
- ↑ 1.0 1.1 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A.
- ↑ 2.0 2.1 2.2 2.3 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.
- ↑ 3.0 3.1 3.2 Johnson, H. L. et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory 4 (99): 99, Bibcode: 1966CoLPL...4...99J.
- ↑ 4.0 4.1 4.2 4.3 4.4 4.5 4.6 4.7 Zorec, J.; Royer, F. (2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy and Astrophysics 537: A120, doi:10.1051/0004-6361/201117691, Bibcode: 2012A&A...537A.120Z.
- ↑ 5.0 5.1 Cowley, A. et al. (April 1969), "A study of the bright A stars. I. A catalogue of spectral classifications", Astronomical Journal 74: 375–406, doi:10.1086/110819, Bibcode: 1969AJ.....74..375C.
- ↑ 6.0 6.1 Wilson, Ralph Elmer (1953), "General Catalogue of Stellar Radial Velocities", Carnegie Institute Washington D.C. Publication (Washington: Carnegie Institution of Washington), Bibcode: 1953GCRV..C......0W.
- ↑ Pasinetti Fracassini, L. E. et al. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition - Comments and statistics", Astronomy and Astrophysics 367 (2): 521–524, doi:10.1051/0004-6361:20000451, Bibcode: 2001A&A...367..521P.
- ↑ 8.0 8.1 8.2 8.3 8.4 Gullikson, Kevin et al. (2016), "The Close Companion Mass-ratio Distribution of Intermediate-mass Stars", The Astronomical Journal 152 (2): 40, doi:10.3847/0004-6256/152/2/40, Bibcode: 2016AJ....152...40G.
- ↑ "* psi03 Aqr". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=%2A+psi03+Aqr.
- ↑ 10.0 10.1 Schröder, C.; Schmitt, J. H. M. M. (November 2007), "X-ray emission from A-type stars", Astronomy and Astrophysics 475 (2): 677–684, doi:10.1051/0004-6361:20077429, Bibcode: 2007A&A...475..677S.
- ↑ van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V.
- ↑ 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.
External links
 | Original source: https://en.wikipedia.org/wiki/Psi3 Aquarii. Read more |
