Share to: share facebook share twitter share wa share telegram print page

 

Pi1 Pegasi

For other stars with this Bayer designation see π Pegasi
Pi1 Pegasi
Location of π2 Pegasi (circled)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Pegasus
Right ascension 22h 09m 13.61893s[1]
Declination +33° 10′ 20.4778″[1]
Apparent magnitude (V) +5.58[2]
Characteristics
Spectral type G8IIIb[3]
B−V color index +0.985±0.003[2]
Astrometry
Radial velocity (Rv)+5.1±0.9[4] km/s
Proper motion (μ) RA: −48.117[1] mas/yr
Dec.: −73.408[1] mas/yr
Parallax (π)10.2111 ± 0.1137 mas[1]
Distance319 ± 4 ly
(98 ± 1 pc)
Absolute magnitude (MV)0.84[5]
Details
Mass2.48[6] M☉
Radius11.00+0.51
−0.83[1] R☉
Luminosity62.8±0.8[1] L☉
Surface gravity (log g)2.7[7] cgs
Temperature4,898+196
−110[1] K
Metallicity [Fe/H]−0.22[5] dex
Rotational velocity (v sin i)135[7] km/s
Age530[6] Myr
Other designations
π Peg, 27 Pegasi, BD+32°4349, HD 210459, HIP 109352, HR 8449, SAO 72064[8]
Database references
SIMBADdata

Pi1 Pegasi, Latinized from π1 Pegasi, is a star in the constellation Pegasus. Based upon changes to the proper motion of the visible component, this is a probable astrometric binary.[9] It has a yellow hue and is dimply visible to the naked eye with a combined apparent visual magnitude of +5.58.[2] The system is located approximately 319 light years distant from the Sun based on parallax,[1] and is drifting further away with a radial velocity of +5 km/s.[4] It is a member of the Ursa Major Moving Group of co-moving stars.[10]

π1 Pegasi (right) and π2 Pegasi (left) in optical light

The visible component is an aging giant star with a stellar classification of G8IIIb.[3] It has a high rate of spin, with a projected rotational velocity of 135 km/s.[7] This is giving it an equatorial bulge that is 17% larger than the polar radius.[11] It is a shell star, being orbited by a circumstellar shell of cooler gas.[12][13] This star is 530[6] million years old with 2.5[6] times the mass of the Sun. With the supply of hydrogen exhausted at its core, the star has cooled and expanded to 11[1] times the Sun's radius. It is radiating 63[1] times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,898 K.[1]

References

  1. ^ a b c d e f g h i j k l 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.
  2. ^ a b c 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.
  3. ^ a b Abt, H. A. (September 1985), "Visual multiples. VIII. 1000 MK types", Astrophysical Journal Supplement Series, 59: 95–112, Bibcode:1985ApJS...59...95A, doi:10.1086/191064
  4. ^ a b Gontcharov, G. A. (November 2006), "Pulkovo Compilation of Radial Velocities for 35495 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.
  5. ^ a b Takeda, Yoichi; et al. (August 2008), "Stellar Parameters and Elemental Abundances of Late-G Giants", Publications of the Astronomical Society of Japan, 60 (4): 781–802, arXiv:0805.2434, Bibcode:2008PASJ...60..781T, doi:10.1093/pasj/60.4.781.
  6. ^ a b c d Luck, R. Earle (2015), "Abundances in the Local Region. I. G and K Giants", The Astronomical Journal, 150 (3): 88, arXiv:1507.01466, Bibcode:2015AJ....150...88L, doi:10.1088/0004-6256/150/3/88, S2CID 118505114.
  7. ^ a b c Massarotti, Alessandro; et al. (January 2008), "Rotational and Radial Velocities for a Sample of 761 HIPPARCOS Giants and the Role of Binarity", The Astronomical Journal, 135 (1): 209–231, Bibcode:2008AJ....135..209M, doi:10.1088/0004-6256/135/1/209, S2CID 121883397
  8. ^ "pi Peg". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-10-13.
  9. ^ Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
  10. ^ Schmitt, J. H. M. M.; et al. (March 1990), "X-ray studies of coeval star samples. III. X-ray emission in the UrsaMajor stream.", Astrophysical Journal, 351: 492–499, Bibcode:1990ApJ...351..492S, doi:10.1086/168486.
  11. ^ van Belle, Gerard T. (March 2012), "Interferometric observations of rapidly rotating stars", The Astronomy and Astrophysics Review, 20 (1): 51, arXiv:1204.2572, Bibcode:2012A&ARv..20...51V, doi:10.1007/s00159-012-0051-2, S2CID 119273474.
  12. ^ Hauck, B.; Jaschek, C. (February 2000), "A-shell stars in the Geneva system", Astronomy and Astrophysics, 354: 157–162, Bibcode:2000A&A...354..157H.
  13. ^ Slettebak, A. (September 1986), "H-alpha and near-infrared spectra of late-type Be and A-F-type shell stars.", Publications of the Astronomical Society of the Pacific, 98: 867–871, Bibcode:1986PASP...98..867S, doi:10.1086/131836.
Kembali kehalaman sebelumnya