53 Piscium
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Pisces |
| Right ascension | 00h 36m 47.31222s[1] |
| Declination | 15° 13′ 54.2151″[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: 0.85[1] mas/yr Dec.: −13.68[1] mas/yr |
| Parallax (π) | 3.14 ± 0.30[1] mas |
| Distance | 1,040 ± 100 ly (320 ± 30 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 | 17300 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,[2] it is just barely visible to the naked eye. parallax measurements made by the Hipparcos spacecraft place the star at a distance of about 1,040 light-years (320 parsecs) away.[1]
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
- 1 2 3 4 5 6 van Leeuwen, F.; et al. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. Bibcode:2007A&A...474..653V. arXiv:0708.1752
. doi:10.1051/0004-6361:20078357. - 1 2 3 4 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. doi:10.1086/190179.
- 1 2 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. 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. Bibcode:2006AstL...32..759G. arXiv:1606.08053 . doi:10.1134/S1063773706110065. Retrieved 12 December 2016.
- ↑ 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: L61. arXiv:astro-ph/0604283 . doi:10.1111/j.1745-3933.2006.00175.x.
- ↑ de Cat, P. (2007). "Observational Asteroseismology of slowly pulsating B stars" (PDF). Communications in Asteroseismology. 150: 167–74. Bibcode:2007CoAst.150..167D. doi:10.1553/cia150s167.