HD 17925 is a variable star in the equatorial constellation of Eridanus. It has the Gould designation 32 G. Eridani and the variable star designation EP Eri. The star has a yellow-orange hue and is dimly visible to the naked eye in good seeing conditions with an apparent visual magnitude that varies from 6.03 down to 6.08.[16] It is located nearby at a distance of 34 light years from the Sun based on parallax,[2] and is drifting further away with a radial velocity of +18 km/s.[7] It is a likely member of the Local Association of nearby, co-moving stars.[12] The spectrum shows a strong abundance of lithium, indicating that it is young star.[17] This likely makes its point of origin the nearby Scorpio–Centaurus Complex.[18]
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Eridanus |
| Right ascension | 02h 52m 32.12819s[2] |
| Declination | –12° 46′ 10.9681″[2] |
| Apparent magnitude (V) | 6.04[3] |
| Characteristics | |
| Evolutionary stage | Main sequence |
| Spectral type | K1V[4] |
| U−B color index | +1.41[5] |
| B−V color index | +0.86[5] |
| Variable type | RS CVn[6] |
| Astrometry | |
| Radial velocity (Rv) | +17.77±0.08[7] km/s |
| Proper motion (μ) | RA: 397.353[2] mas/yr Dec.: −189.281[2] mas/yr |
| Parallax (π) | 96.5200 ± 0.0258 mas[2] |
| Distance | 33.792 ± 0.009 ly (10.361 ± 0.003 pc) |
| Absolute magnitude (MV) | 5.97[8] |
| Details | |
| Mass | 0.88[9] M☉ |
| Radius | 0.85±0.05[10] R☉ |
| Luminosity | 0.408±0.005[2] L☉ |
| Surface gravity (log g) | 4.58[9] cgs |
| Temperature | 5,225±5[11] K |
| Metallicity [Fe/H] | +0.10[12] dex |
| Rotation | 6.6 days[12] |
| Rotational velocity (v sin i) | 4.80[13] km/s |
| Age | 100[14] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
The stellar classification of HD 17925 is K1V,[4] which indicates this is a K-type main-sequence star that is engaged in core hydrogen fusion. It is an active star[17] that is classified as a RS Canum Venaticorum variable,[16] showing a rotational modulation with a period of 6.9 days, and has been observed to flare.[6] The star has an estimated age of 100[14] million years and is spinning with a projected rotational velocity of 4.8 km/s.[13] The rotation period of 6.6 days days can be determined from its activity cycle.[12] The star has 88%[9] of the mass of the Sun and 85%[10] of the Sun's radius. It is radiating 41%[2] of the luminosity of the Sun from its photosphere at an effective temperature of 5,225 K.[11]
The presence of an unseen companion has been suggested based on variations in the widths of absorption lines in the star's photosphere.[17] It displays low-amplitude radial velocity variation, which may indicate it is a spectroscopic binary.[10] However, the binary hypothesis doesn't appear to be consistent with Hipparcos satellite data.[12] An infrared excess has been detected around this star, most likely indicating the presence of a circumstellar disk at a radius of 17.9 AU. The temperature of this dust is 52 K.[19]
References
edit- ^ Cutispoto, G. (November 1992). "Long-term monitoring of active stars. II. UBV (RI)c observations at ESO during January-March 1989". Astronomy and Astrophysics Supplement Series. 95: 397–413. Bibcode:1992A&AS...95..397C.
- ^ a b c d e f g h 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.
- ^ Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data. SIMBAD, Bibcode:1986EgUBV........0M.
- ^ a b Montes, D.; et al. (2001), "Late-type members of young stellar kinematic groups - I. Single stars", Monthly Notices of the Royal Astronomical Society, 328 (1): 45–63, arXiv:astro-ph/0106537, Bibcode:2001MNRAS.328...45M, doi:10.1046/j.1365-8711.2001.04781.x, S2CID 55727428.
- ^ a b Vieytes, M.; et al. (May 2007), Heinzel, P.; Dorotovič, I.; Rutten, R. J. (eds.), "Chromospheric Activity in K Stars", The Physics of Chromospheric Plasmas. Proceedings of the conference held 9-13 October, 2006 at the University of Coimbra in Coimbra, Portugal, ASP Conference Series, vol. 368, San Francisco: Astronomical Society of the Pacific, p. 265, Bibcode:2007ASPC..368..265V.
- ^ a b Abbott, B. P.; Pomerance, B. H.; Ambruster, C. W. (March 1995), "UBVRI Photometry of the Solar Neighborhood Pleiades-Age K Dwarfs HD 17925 and HD 1405", Bulletin of the American Astronomical Society, 27: 842, Bibcode:1995AAS...186.2210A.
- ^ a b Karataș, Yüksel; Bilir, Selçuk; Eker, Zeki; Demircan, Osman; Liebert, James; Hawley, Suzanne L.; Fraser, Oliver J.; Covey, Kevin R.; Lowrance, Patrick; Kirkpatrick, J. Davy; Burgasser, Adam J. (2004). "Kinematics of chromospherically active binaries and evidence of an orbital period decrease in binary evolution". Monthly Notices of the Royal Astronomical Society. 349 (3): 1069–1092. arXiv:astro-ph/0404219. Bibcode:2004MNRAS.349.1069K. doi:10.1111/j.1365-2966.2004.07588.x. S2CID 15290475.
- ^ Holmberg, J.; et al. (July 2009), "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics", Astronomy and Astrophysics, 501 (3): 941–947, arXiv:0811.3982, Bibcode:2009A&A...501..941H, doi:10.1051/0004-6361/200811191, S2CID 118577511.
- ^ a b c Luck, R. Earle (March 2018), "Abundances in the Local Region. III. Southern F, G, and K Dwarfs", The Astronomical Journal, 155 (3): 31, Bibcode:2018AJ....155..111L, doi:10.3847/1538-3881/aaa9b5, S2CID 125765376, 111.
- ^ a b c Ambruster, C. W.; et al. (October 2003), Brown, A.; Harper, G. M.; Ayres, T. R. (eds.), "The Radii of Solar Neighborhood ZAMS Stars", The Future of Cool-Star Astrophysics: 12th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun (2001 July 30 - August 3), vol. 12, pp. 912–915, Bibcode:2003csss...12..912A.
- ^ a b Kovtyukh, V. V.; et al. (2003), "High precision effective temperatures for 181 F-K dwarfs from line-depth ratios", Astronomy and Astrophysics, 411 (3): 559–564, arXiv:astro-ph/0308429, Bibcode:2003A&A...411..559K, doi:10.1051/0004-6361:20031378, S2CID 18478960.
- ^ a b c d e Maldonado, J.; et al. (October 2010), "A spectroscopy study of nearby late-type stars, possible members of stellar kinematic groups", Astronomy and Astrophysics, 521: A12, arXiv:1007.1132, Bibcode:2010A&A...521A..12M, doi:10.1051/0004-6361/201014948, S2CID 119209183.
- ^ a b Mishenina, T. V.; et al. (November 2012), "Activity and the Li abundances in the FGK dwarfs", Astronomy & Astrophysics, 547: 8, arXiv:1210.6843, Bibcode:2012A&A...547A.106M, doi:10.1051/0004-6361/201118412, S2CID 119287319, A106.
- ^ a b Mamajek, Eric E.; Hillenbrand, Lynne A. (November 2008), "Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics", The Astrophysical Journal, 687 (2): 1264–1293, arXiv:0807.1686, Bibcode:2008ApJ...687.1264M, doi:10.1086/591785, S2CID 27151456.
- ^ "HD 17925", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2021-01-11.
- ^ a b Samus', N. N; et al. (2017), "General catalogue of variable stars", Astronomy Reports, GCVS 5.1, 61 (1): 80, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID 125853869.
- ^ a b c Pandey, J. C.; Singh, K. P. (July 2008), "A study of X-ray flares - I. Active late-type dwarfs", Monthly Notices of the Royal Astronomical Society, 387 (4): 1627−1648, arXiv:0805.3882, Bibcode:2008MNRAS.387.1627P, doi:10.1111/j.1365-2966.2008.13342.x, S2CID 18111371.
- ^ Cayrel de Strobel, G.; Cayrel, R. (July 1989), "Strong lithium in the very nearby K-dwarf HD 17925", Astronomy and Astrophysics, 218 (1–2): L9–L12, Bibcode:1989A&A...218L...9C
- ^ Eiroa, C.; et al. (July 2013), "DUst around NEarby Stars. The survey observational results", Astronomy & Astrophysics, 555: A11, arXiv:1305.0155, Bibcode:2013A&A...555A..11E, doi:10.1051/0004-6361/201321050, S2CID 377244.
Further reading
edit- Christian, D. J.; Mathioudakis, M.; Jevremović, D. (October 2008), "6Li in the Atmosphere of GJ 117 Revisited", The Astrophysical Journal, 686 (1): 542–547, arXiv:0807.3693, Bibcode:2008ApJ...686..542C, doi:10.1086/591727, S2CID 346207
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