HR 178 is a probable binary star in the constellation Andromeda. Located approximately 124 parsecs (400 ly) distant, it is an evolved Am star[9] with a combined apparent magnitude of 6.06, meaning that it can only be seen with the naked eye on dark, clear nights. The star is suspected of variability, possibly varying between magnitudes 6.04 and 6.06.[4] The variable magnitude period of HD 3883 is about 9.17 min.[10]
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Andromeda |
| Right ascension | 00h 41m 36.0370s[1] |
| Declination | +24° 37′ 44.43″[1] |
| Apparent magnitude (V) | 6.046[2] |
| Characteristics | |
| Spectral type | kA5hF1mF2[3] |
| B−V color index | 0.287[2] |
| Variable type | suspected[4] |
| Astrometry | |
| Radial velocity (Rv) | −15.60±0.9[5] km/s |
| Proper motion (μ) | RA: 106.272±0.499[1] mas/yr Dec.: −12.324±0.306[1] mas/yr |
| Parallax (π) | 8.0963 ± 0.2630 mas[1] |
| Distance | 400 ± 10 ly (124 ± 4 pc) |
| Orbit[6] | |
| Period (P) | 21.26 yr |
| Semi-major axis (a) | 0.126″ |
| Eccentricity (e) | 0.5 |
| Details | |
| Mass | 2.44[7] M☉ |
| Radius | 3.82[1] R☉ |
| Luminosity | 45[1] L☉ |
| Surface gravity (log g) | 3.80±0.14[8] cgs |
| Temperature | 7800±200[8] K |
| Metallicity [Fe/H] | 0.53±0.13[8] dex |
| Rotational velocity (v sin i) | 18[3] km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
The spectrum of HR 178 has been extensively studied for establishing element abundances in the evolved Am stars. It is given a spectral class of kA5hF1mF2, meaning its spectral type is A5, F1, or F2, depending on the particular spectral lines examined. The evolutionary stage of the star, and its mass determined from comparison with theoretical evolutionary tracks, is not precisely determined. However, it is very close to the end of its main sequence evolution and the margin of error in its mass is only about 0.1 M☉.[9]
HR 178 has been suspected of being a binary star since 1938 when its spectrum was interpreted as being composite.[11] The pair were resolved using speckle interferometry in 1983.[12] The companion is modelled to be between 1.5 and 3 magnitudes fainter than the primary star.[13] Although there have since been several failed attempts to resolve the pair, a tentative orbit has been calculated with a period of 21.26 years and an eccentricity of 0.5.[6]
References
edit- ^ a b c d e f g Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ a b Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (2000), "The Tycho-2 catalogue of the 2.5 million brightest stars", Astronomy & Astrophysics, 355: L27–L30, Bibcode:2000A&A...355L..27H.
- ^ a b Abt, Helmut A.; Morrell, Nidia I. (1995). "The Relation between Rotational Velocities and Spectral Peculiarities among A-Type Stars". The Astrophysical Journal Supplement Series. 99: 135. Bibcode:1995ApJS...99..135A. doi:10.1086/192182.
- ^ a b VSX (18 January 2010). "NSV 258". AAVSO Website. American Association of Variable Star Observers. Retrieved 15 June 2013.
- ^ 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.
- ^ a b Malkov, O. Yu.; Tamazian, V. S.; Docobo, J. A.; Chulkov, D. A. (2012). "Dynamical masses of a selected sample of orbital binaries". Astronomy & Astrophysics. 546: 5. Bibcode:2012A&A...546A..69M. doi:10.1051/0004-6361/201219774.
- ^ Hui-Bon-Hoa, A. (June 2000). "Metal abundances of field A and Am stars". Astronomy and Astrophysics Supplement Series. 144 (2): 203–209. Bibcode:2000A&AS..144..203H. doi:10.1051/aas:2000207. ISSN 0365-0138. S2CID 123151702.
- ^ a b c Soubiran, Caroline; et al. (2016), "The PASTEL catalogue: 2016 version", Astronomy & Astrophysics, 591: A118, arXiv:1605.07384, Bibcode:2016A&A...591A.118S, doi:10.1051/0004-6361/201628497, S2CID 119258214.
- ^ a b Burkhart, C.; Coupry, M. F.; Faraggiana, R.; Gerbaldi, M. (2005). "The field Am and ρ Puppis-like stars: Lithium and heavier elements". Astronomy and Astrophysics. 429 (3): 1043. Bibcode:2005A&A...429.1043B. doi:10.1051/0004-6361:20040467.
- ^ Chagnon, François (2009). Searching for northern roap stars: the UBC-OAN photometric survey. University of British Columbia (Thesis). doi:10.14288/1.0099308. S2CID 124888408.
- ^ Hynek, J. A. (1938). "A survey of stars with composite spectra". Contributions of Perkins Observatory. 1: 10. Bibcode:1938CoPer...1...10H.
- ^ McAlister, H. A.; Hendry, E. M.; Hartkopf, W. I.; Campbell, B. G.; Fekel, F. C. (1983). "Speckle interferometric measurements of binary stars. VIII". The Astrophysical Journal Supplement Series. 51: 309. Bibcode:1983ApJS...51..309M. doi:10.1086/190851.
- ^ Bonneau, D.; Carquillat, J. M.; Vidal, J. L. (1984). "Observations d'etoiles doubles par interferometrie des tavelures AU T2m du PIC du Midi". Astronomy and Astrophysics Supplement Series. 58: 729. Bibcode:1984A&AS...58..729B.