HD 8357
| Observation data Epoch J2000.0 Equinox J2000.0 | ||
|---|---|---|
| Constellation | Pisces | |
| Right ascension | 01h 22m 56.757s[1] | |
| Declination | +07° 25′ 09.33″[1] | |
| Apparent magnitude (V) | 7.24[2] (7.68 + 8.43)[2] | |
| Characteristics | ||
| Primary | ||
| Spectral type | Kl IV[2] | |
| U−B color index | 0.68[2] | |
| B−V color index | 0.93[2] | |
| Variable type | RS CVn[3] | |
| Secondary | ||
| Spectral type | G7 V[2] | |
| U−B color index | 0.29[2] | |
| B−V color index | 0.71[2] | |
| Absolute magnitude (MV) | 4.03[5] | |
Semi-amplitude (K1)(primary) | 25.37±0.09 km/s | |
| Semi-amplitude (K2) (secondary) | 31.01±0.18 km/s | |
| Details | ||
| Primary | ||
Gyr | ||
| Secondary | ||
| Mass | 0.92[2] M☉ | |
LTT 10501[6] | ||
| Database references | ||
| SIMBAD | data | |
AR Piscium is a
light years from the Sun.[1] The motion of this star through the Milky Way suggests it is a member of the intermediate disc population.[2]
Variable X-ray source H0123+075 was identified from the HEAO 1 A-2 experiment and published by F. E. Marshall and associates in 1979. The following year, M. Garcia and associates identified the most probable source star as HD 8357, and determined it to be a RS Canum Venaticorum variable.[8] This has a spectral class of G5 in the Henry Draper Catalogue. Optical observations by D. S. Hall and associates in 1980–1981 confirmed the source star to be optically variable with a period of 12.3±0.1 d.[9] In 1993, AR Psc was identified as an extreme ultraviolet source by K. A. Pounds and associates using ROSAT.[10]
This is a double-lined
pseudosynchronous rotation.[2]
References
- ^ .
- ^ doi:10.1086/118010.
- S2CID 125853869.
- ^ S2CID 220496397.
- S2CID 119257644.
- ^ "HD 8357". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2023-11-12.
- Bibcode:1985IBVS.2681....1K.
- doi:10.1086/183334.
- doi:10.1086/183815.
- .
- doi:10.1086/162405.
Further reading
- Karmakar, Subhajeet; et al. (January 2023), "Swift and XMM-Newton observations of an RS CVn-type eclipsing binary SZ Psc: superflare and coronal properties", Monthly Notices of the Royal Astronomical Society, 518 (1): 900–918, .
- Nakamura, Y.; et al. (July 2016), "MAXI/GSC detection of a possible X-ray flare from an RS CVn star AR Psc", The Astronomer's Telegram, 9288, Bibcode:2016ATel.9288....1N.
- Sanz-Forcada, J.; et al. (October 2009), "No first ionization potential fractionation in the active stars AR Piscium and AY Ceti", Astronomy and Astrophysics, 505 (1): 299–306, .
- Shan, Hongguang; et al. (January 2006), "The atmospheric parameters, abundances and magnetic field of the AR piscium primary", New Astronomy, 11 (4): 287–292, .
- Montes, D.; et al. (1993), Linsky, Jeffrey L.; Serio, Salvatore (eds.), "Analysis of Chromospheric Activity Indicators in MM Her and AR Psc", Physics of Solar and Stellar Coronae: G. S. Vaiana Memorial Symposium, held 22-26 June, 1992, in Palermo, Italy, Astrophysics and Space Science Library, vol. 183, Dordrecht, The Netherlands: Kluwer Academoc Publishers, .
