56 Pegasi
  | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Pegasus |
| Right ascension | 23h 07m 06.74364s[1] |
| Declination | 25° 28′ 05.788″[1] |
| Apparent magnitude (V) | 4.74[2] |
| Characteristics | |
| Spectral type | K0.5II:Ba1CN-2CH-0.5[3] |
| U−B color index | +1.14[2] |
| B−V color index | +1.32[2] |
| Astrometry | |
| Radial velocity (Rv) | −27.55[4] km/s |
| Proper motion (μ) | RA: −4.288[1] mas/yr Dec.: −32.639[1] mas/yr |
| Parallax (π) | 6.1131±0.4108 mas[1] |
| Distance | 530 ± 40 ly (160 ± 10 pc) |
| Absolute magnitude (MV) | −1.32[5] |
| Orbit[6] | |
| Primary | 56 Peg A |
| Companion | 56 Peg B |
| Period (P) | 111.15±0.03 d |
| Semi-major axis (a) | 0.79+0.10 −0.08 AU |
| Eccentricity (e) | 0.072+0.048 −0.045 |
| Inclination (i) | 90+42 −41° |
| Longitude of the node (Ω) | 90+60 −42° |
| Periastron epoch (T) | 2455289+15 −85 HJD |
| Argument of periastron (ω) (secondary) | 55+270 −37° |
| Semi-amplitude (K1) (primary) | 1.47±0.04[7] km/s |
| Orbit[6] | |
| Primary | 56 Peg A |
| Companion | 56 Peg C |
| Period (P) | 15,200+2,600 −1,600 d |
| Semi-major axis (a) | 22.1+3.6 −2.8 AU |
| Eccentricity (e) | 0.39+0.13 −0.12 |
| Inclination (i) | 157+4 −5° |
| Longitude of the node (Ω) | 153+14 −17° |
| Periastron epoch (T) | 2469014±2800 HJD |
| Argument of periastron (ω) (secondary) | 73+21 −24° |
| Details | |
| 56 Peg A | |
| Mass | 4.3±1.1[6] M☉ |
| Radius | 41[8] R☉ |
| Luminosity | 18.2 - 18.9[8] L☉ |
| Surface gravity (log g) | 0.50[9] cgs |
| Temperature | 4,185±85[8] K |
| Metallicity [Fe/H] | −0.21[10] dex |
| Rotational velocity (v sin i) | 4.4[11] km/s |
| Age | 100±100[12] Myr |
| 56 Peg B | |
| Mass | 0.13+0.06 −0.03[6] M☉ |
| 56 Peg C | |
| Mass | 0.85+0.25 −0.18[6] M☉ |
| Other designations | |
| 56 Peg, NSV 14429, BD+24°4716, FK5 3848, GC 32201, HD 218356, HIP 114155, HR 8796, SAO 91019, 2MASS J23070675+2528055[13] | |
| Database references | |
| SIMBAD | data |
56 Pegasi is a triple star[6] system in the northern constellation of Pegasus. It is visible to the naked eye with a combined apparent visual magnitude of 4.74.[2] The system is approximately 590 light years away from the Sun based on parallax,[14] but is drifting closer with a radial velocity of −28 km/s.[4] It is listed as a member of the Wolf 630 moving group.[15]
Characteristics
[edit]The variable radial velocity of this star was announced in 1911 by W. W. Campbell.[7] The inner system, made up by the primary and secondary components, is a single-lined spectroscopic binary in an nearly circular orbit with a period of 111.15 days. The average separation between components is 0.79 astronomical units.[6]
The primary component is a peculiar bright giant with a stellar classification of K0.5 II: Ba1 CN-2 CH-0.5.[3] This notation indicates it is a K-type giant with some uncertainty about the classification, along with an overabundance of barium and underabundances of the CN and CH radicals. It is an active star,[16] roughly 100 million years old, with 5.4 times the Sun's mass.[12] The star has expanded to 40[17] times the radius of the Sun and is radiating 680[10] times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,416 K.[18]
The secondary has a mass 0.13 times the mass of the Sun.[6]
The tertiary component is a white dwarf with 0.85 times the mass of the Sun. This companion lost mass when it was an AGB star, causing s-process elements, produced by nucleosynthesis, to be transferred to the primary star, resulting in its current unusual abundances. This star has an orbital period of 41.6 years, a moderate eccentricity, and an average separation of 22 AU.[6]
The system displays an excess of ultraviolet radiation that must be coming from the secondary. Simon et al. (1982) classified this object as a subdwarf O star.[19] Alternatively, it may be a white dwarf companion with an accretion disk.[20][7] Several puzzling features in the evolutionary history of this pair may be explained if the primary is a fast rotator being seen nearly pole-on. The star may have been spun up during a mass transfer episode with the secondary.[16]
References
[edit]- ^ a b c d e 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 c d Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237. Bibcode:2002yCat.2237....0D.
- ^ a b Keenan, Philip C.; McNeil, Raymond C. (1989). "The Perkins catalog of revised MK types for the cooler stars". Astrophysical Journal Supplement Series. 71: 245. Bibcode:1989ApJS...71..245K. doi:10.1086/191373.
- ^ a b Famaey, B.; et al. (2005). "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data". Astronomy & Astrophysics. 430: 165–186. arXiv:astro-ph/0409579. Bibcode:2005A&A...430..165F. doi:10.1051/0004-6361:20041272. S2CID 17804304.
- ^ Frankowski, A.; Jorissen, A. (2006). "The puzzling case of 56 Pegasi: A fast rotator seen nearly pole-on". The Observatory. 126: 25. arXiv:astro-ph/0512036. Bibcode:2006Obs...126...25F.
- ^ a b c d e f g h i Escorza, A.; De Rosa, R. J. (March 2023). "Barium and related stars, and their white-dwarf companions: III. The masses of the white dwarfs". Astronomy & Astrophysics. 671: A97. arXiv:2301.04232. Bibcode:2023A&A...671A..97E. doi:10.1051/0004-6361/202244782. ISSN 0004-6361.
- ^ a b c Griffin, R. F. (2006). "Spectroscopic binary orbits from photoelectric radial velocities - Paper 186: 56 Pegasi". The Observatory. 126: 1. Bibcode:2006Obs...126....1G.
- ^ a b c Messineo, M.; Brown, A. G. A. (2019). "A Catalog of Known Galactic K-M Stars of Class I Candidate Red Supergiants in Gaia DR2". The Astronomical Journal. 158 (1): 20. arXiv:1905.03744. Bibcode:2019AJ....158...20M. doi:10.3847/1538-3881/ab1cbd. S2CID 148571616.
- ^ 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 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID 119257644. Vizier catalog entry
- ^ De Medeiros, J. R.; Mayor, M. (1999). "A catalog of rotational and radial velocities for evolved stars". Astronomy and Astrophysics Supplement Series. 139 (3): 433. arXiv:astro-ph/0608248. Bibcode:1999A&AS..139..433D. doi:10.1051/aas:1999401. Vizier catalog entry
- ^ a b Tetzlaff, N.; et al. (2011). "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun". Monthly Notices of the Royal Astronomical Society. 410 (1): 190–200. arXiv:1007.4883. Bibcode:2011MNRAS.410..190T. doi:10.1111/j.1365-2966.2010.17434.x. S2CID 118629873. Vizier catalog entry
- ^ "56 Peg". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-07-01.
- ^ Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID 18759600. Vizier catalog entry
- ^ McDonald, A. R. E.; Hearnshaw, J. B. (August 1983). "The Wolf 630 moving group of stars". Monthly Notices of the Royal Astronomical Society. 204 (3): 841–852. Bibcode:1983MNRAS.204..841M. doi:10.1093/mnras/204.3.841.
- ^ a b Frankowski, A.; Jorissen, A. (February 2006). "The puzzling case of 56 Pegasi: a fast rotator seen nearly pole-on". The Observatory. 126: 25–37. arXiv:astro-ph/0512036. Bibcode:2006Obs...126...25F.
- ^ van Belle, G. T.; et al. (2009). "Supergiant temperatures and linear radii from near-infrared interferometry". Monthly Notices of the Royal Astronomical Society. 394 (4): 1925. arXiv:0811.4239. Bibcode:2009MNRAS.394.1925V. doi:10.1111/j.1365-2966.2008.14146.x. S2CID 118372600.
- ^ Martínez, M. Isabel Pérez; et al. (2011). "The basal chromospheric Mg ii h+k flux of evolved stars: Probing the energy dissipation of giant chromospheres". Monthly Notices of the Royal Astronomical Society. 414 (1): 418. arXiv:1102.4832. Bibcode:2011MNRAS.414..418P. doi:10.1111/j.1365-2966.2011.18421.x. S2CID 59268230. Vizier catalog entry
- ^ Simon, T.; et al. (1982). "On the reality of a boundary in the H-R diagram between late-type stars with and without high temperature outer atmospheres". Astrophysical Journal. 257: 225. Bibcode:1982ApJ...257..225S. doi:10.1086/159981.
- ^ Schindler, M.; et al. (December 1982). "Ultraviolet and X-ray detection of the 56 Pegasi system /K0 IIp + WD/ - Evidence for accretion of a cool stellar wind onto a white dwarf". Astrophysical Journal, Part 1. 263: 269–276. Bibcode:1982ApJ...263..269S. doi:10.1086/160501.
