DV Piscium is a triple star system[9] in the equatorial constellation of Pisces, abbreviated DV Psc. It is an eclipsing binary variable of the RS Canum Venaticorum class.[7] The pair have a combined apparent visual magnitude of 10.59,[4] which is too faint to be visible with the naked eye. Based on parallax measurements, DV Piscium is located at a distance of 137.5 light years from the Sun.[3] It is drifting closer with a radial velocity of −28 km/s.[6]
 Light curves for DV Piscium. The upper panel, plotted from TESS data,[1] shows the periodic variability due to eclipses. The bottom panel, adapted from Zhang et al.,[2] shows the flare which occurred at UT 11:00 on Nov. 22, 2008, in three photometric bands. | |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Pisces |
| Right ascension | 00h 13m 09.204s[3] |
| Declination | +05° 35′ 43.01″[3] |
| Apparent magnitude (V) | 10.59[4] |
| Characteristics | |
| Evolutionary stage | main sequence[5] |
| Spectral type | K5Ve[6] |
| Variable type | Eclipsing RS CVn[4] |
| Astrometry | |
| Radial velocity (Rv) | −27.8[6] km/s |
| Proper motion (μ) | RA: −111.396 mas/yr[3] Dec.: −203.771 mas/yr[3] |
| Parallax (π) | 23.7216 ± 0.0223 mas[3] |
| Distance | 137.5 ± 0.1 ly (42.16 ± 0.04 pc) |
| Absolute magnitude (MV) | 9.9±1.2[7] |
| Orbit[8] | |
| Period (P) | 0.30853609[7] d |
| Semi-major axis (a) | 2.038 R☉[7] |
| Eccentricity (e) | 0.00 |
| Inclination (i) | 74.220±0.353[9]° |
| Periastron epoch (T) | 2,451,794.1921±0.0004 HJD |
| Argument of periastron (ω) (secondary) | 0.00° |
| Semi-amplitude (K1) (primary) | 131.62±0.55 km/s |
| Semi-amplitude (K2) (secondary) | 187.55±1.80 km/s |
| Details[9] | |
| Primary | |
| Mass | 0.68±0.02 M☉ |
| Radius | 0.73±0.01 R☉ |
| Luminosity | 0.186±0.009 L☉ |
| Temperature | 4,450±40 K |
| Rotational velocity (v sin i) | 120±20[6] km/s |
| Age | 1.8±0.5 Gyr |
| Secondary | |
| Mass | 0.47±0.02 M☉ |
| Radius | 0.52±0.01 R☉ |
| Luminosity | 0.044±0.003 L☉ |
| Temperature | 3,680±50 K |
| Other designations | |
| Database references | |
| SIMBAD | data |
In 1994, this target was found to show emission line features in the calcium H and K lines. It was classified as a K-type star with high proper motion in 1986. Data from the ROSAT satellite showed significant X-ray emission. In 1999, it was shown to be a near-contact eclipsing binary star system by R. M. Robb and associates, with an orbital period of 0.30855 days. The shape of the light curve suggested the presence of one or more star spots on the cooler component.[11] A flare event was observed on November 22, 2008, indicative of a high level of magnetic activity.[2]
Combining photometric results across several years demonstrated that the light curve is highly variable, with star spot activity on both components. This varied over time in quantity, size, and location.[12] This is a detached binary system with the components in near contact at a separation of just two solar radii. As of 2007, the period of the system is decreasing over time at a rate of about −8.6×10−7 d·yr–1.[7] The primary component has 68% of the mass of the Sun and 73% of the Sun's radius; the cooler secondary has 47% of the mass and 52% of the radius of the Sun.[9] Both components are slightly evolved main sequence stars. The system has an activity cycle estimated at 14.74±0.84 years.[5]
Evidence from O–C diagrams suggests there is a third component to this system, orbiting the inner pair with a period of 9.79±0.60 years on an eccentric orbit. This body has less than 62% of the mass of the Sun.[9]
References
edit- ^ MAST: Barbara A. Mikulski Archive for Space Telescopes, Space Telescope Science Institute, retrieved 15 February 2023.
- ^ a b Zhang, Liyun; Zhang, Xiliang; Zhu, Zhongzhong (April 2010), "The CCD photometric study of the newly identified RS CVn binary star DV Piscium", New Astronomy, 15 (4): 362–366, Bibcode:2010NewA...15..362Z, doi:10.1016/j.newast.2009.10.004.
- ^ a b c d e Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
- ^ a b c Samus, N. N.; et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1, 61 (1): 80–88, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID 125853869.
- ^ a b Palafouta, S.; Gazeas, K. (March 2020), "Temporal evolution of the magnetically active eclipsing binary DV Psc", Contributions of the Astronomical Observatory Skalnaté Pleso, 50 (2): 521–522, Bibcode:2020CoSka..50..521P, doi:10.31577/caosp.2020.50.2.521, S2CID 216389865.
- ^ a b c d Torres, C. A. O.; Quast, G. R.; da Silva, L.; de La Reza, R.; Melo, C. H. F.; Sterzik, M. (December 2006), "Search for associations containing young stars (SACY). I. Sample and searching method", Astronomy and Astrophysics, 460 (3): 695–708, arXiv:astro-ph/0609258, Bibcode:2006A&A...460..695T, doi:10.1051/0004-6361:20065602, S2CID 16080025.
- ^ a b c d e Zhang, X. B.; Zhang, R. X. (December 2007), "The physical nature of the short-period RS CVn system DV Psc", Monthly Notices of the Royal Astronomical Society, 382 (3): 1133–1138, Bibcode:2007MNRAS.382.1133Z, doi:10.1111/j.1365-2966.2007.12293.x, S2CID 120164879.
- ^ Lu, Wenxian; Rucinski, Slavek M.; Ogłoza, Waldemar (July 2001), "Radial Velocity Studies of Close Binary Stars. IV.", The Astronomical Journal, 122 (1): 402–412, arXiv:astro-ph/0104065, Bibcode:2001AJ....122..402L, doi:10.1086/321131.
- ^ a b c d e Gazeas, K.; Palafouta, S. (September 2019), "DV Psc: A Magnetically Active Hierarchical Triple System", Acta Astronomica, 69 (3): 261–282, Bibcode:2019AcA....69..261G, doi:10.32023/0001-5237/69.3.3.
- ^ "DV Psc". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2023-02-12.
- ^ Robb, R. M.; Wagg, J.; Berndsen, A.; Desroches, L. (November 1999), "Photometry of the Eclipsing Binary Star GSC 0008 324 = 1RXS J001309+053550", Information Bulletin on Variable Stars, 4800: 1, Bibcode:1999IBVS.4800....1R.
- ^ Parimucha, Š.; Pribulla, T.; Rucinski, S.; Kaluzny, J.; Thompson, I.; Vaňko, M.; Hambálek, L. (December 2010), Prša, Andrej; Zejda, Miloslav (eds.), "Preliminary Analysis of DV Psc: A Spotted, Short-Period Eclipsing Binary", Binaries - Key to Comprehension of the Universe. Proceedings of a conference held June 8-12, 2009 in Brno, Czech Republic, vol. 435, San Francisco: Astronomical Society of the Pacific, p. 99, Bibcode:2010ASPC..435...99P.
Further reading
edit- Pi, Qing-feng; Zhang, Li-yun; Bi, Shao-lan; Han, Xianming L.; Lu, Hong-peng; Yue, Qiang; Long, Liu; Yan, Yan (June 2019), "Magnetic Activity and Orbital Period Study for the Short-period RS CVn-type Eclipsing Binary DV Psc", The Astrophysical Journal, 877 (2): 75, Bibcode:2019ApJ...877...75P, doi:10.3847/1538-4357/ab19c3, S2CID 191144926, 75.
- Pi, Qing-feng; Zhang, Li-Yun; Li, Zhong-mu; Zhang, Xi-liang (March 2014), "Magnetic Activity and Orbital Period Variation of the Short-period Eclipsing Binary DV Psc", The Astronomical Journal, 147 (3): 50, Bibcode:2014AJ....147...50P, doi:10.1088/0004-6256/147/3/50, S2CID 250769694, 50.
- Pi, Qingfeng; Zhang, Liyun; Li, Zhongmu; Sang, Hongyan; Zhu, Zhongzhong (September 2012), "Photometric study of the short-period RS CVn eclipsing binary DV Psc", arXiv:1209.1862 [astro-ph.SR]