53 Piscium
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Pisces |
| Right ascension | 00h 36m 47.31100s[1] |
| Declination | 15° 13′ 54.1903″[1] |
| Apparent magnitude (V) | 5.87–5.88[2] |
| Characteristics | |
| Spectral type | B2.5IV[3] |
| U−B color index | −0.67[4] |
| B−V color index | −0.15[4] |
| Variable type | β Cep[2] |
| Astrometry | |
| Radial velocity (Rv) | −8.0±0.9[5] km/s |
| Proper motion (μ) | RA: +3.918[1] mas/yr Dec.: −9.890[1] mas/yr |
| Parallax (π) | 3.5167 ± 0.0782 mas[1] |
| Distance | 930 ± 20 ly (284 ± 6 pc) |
| Details[6] | |
| Mass | 5.4±0.9 M☉ |
| Radius | 3.3±1.0 R☉ |
| Luminosity | 794 L☉ |
| Surface gravity (log g) | 4.16±0.20 cgs |
| Temperature | 17,300 K |
| Rotational velocity (v sin i) | 33±17 km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
53 Piscium, abbreviated as 53 Psc, is a star in the zodiac constellation of Pisces. With an apparent magnitude of about 5.9, it is just barely visible to the naked eye. parallax measurements made by the Hipparcos spacecraft place the star at a distance of about 930 light-years (284 parsecs) away.
The spectral type of 53 Piscium is B2.5IV, meaning it is a B-type subgiant. It is 5.4 times more massive than the Sun, and has a luminosity of almost 800 L☉. Its surface temperature is over 17,000 K, typical of a B-type star.
53 Piscium is a Beta Cephei variable, varying by 0.01 magnitudes just under every two hours.[2] For that reason it has been given the AG Piscium. It has also been found to have some variability in common with slowly pulsating B stars.[7]
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 Otero, S. A (21 November 2012). "AG Piscium". AAVSO Website. American Association of Variable Star Observers. Retrieved 5 July 2014.
- ^ Rountree Lesh, Janet (1968). "The Kinematics of the Gould Belt: An Expanding Group?". The Astrophysical Journal Supplement Series. 17: 371. Bibcode:1968ApJS...17..371L. doi:10.1086/190179.
- ^ a b Crawford, D. L.; Barnes, J. V.; Golson, J. C. (1971). "Four-color, Hbeta, and UBV photometry for bright B-type stars in the northern hemisphere". The Astronomical Journal. 76: 1058. Bibcode:1971AJ.....76.1058C. doi:10.1086/111220.
- ^ Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759–771. arXiv:1606.08053. Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. S2CID 119231169.
- ^ Hubrig, S.; Briquet, M.; Scholler, M.; De Cat, P.; Mathys, G.; Aerts, C. (2006). "Discovery of magnetic fields in the Cephei star 1 CMa and in several slowly pulsating B stars". Monthly Notices of the Royal Astronomical Society: Letters. 369 (1): L61–L65. arXiv:astro-ph/0604283. Bibcode:2006MNRAS.369L..61H. doi:10.1111/j.1745-3933.2006.00175.x. S2CID 18201908.
- ^ de Cat, P. (2007). "Observational Asteroseismology of slowly pulsating B stars". Communications in Asteroseismology. 150: 167–74. Bibcode:2007CoAst.150..167D. doi:10.1553/cia150s167.
