References analysis of the Wikipedia article "Gamma Pegasi" in the English version

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Neiner, C.; et al. (February 2014), "γ Pegasi: testing Vega-like magnetic fields in B stars", Astronomy & Astrophysics, 562: 8, arXiv:1312.3521, Bibcode:2014A&A...562A..59N, doi:10.1051/0004-6361/201323093, S2CID 54652836, A59, We find that no magnetic signatures are visible in the very high quality spectropolarimetric data. The average longitudinal field measured in the Narval data is Bl = −0.1 ± 0.4 G. We derive a very strict upper limit of the dipolar field strength of Bpol ~ 40 G.

arxiv.org

van Leeuwen, F. (November 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

Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (January 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

Walczak, P.; Daszyńska-Daszkiewicz, J. (December 2010), "Complex asteroseismology of the hybrid B-type pulsator γ Pegasi: A test of stellar opacities", Astronomische Nachrichten, 331 (9/10): 1057–1060, arXiv:1004.2366, Bibcode:2010AN....331.1057W, doi:10.1002/asna.201011456, S2CID 119218384

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.

Huang, W.; et al. (2012), "A catalogue of Paschen-line profiles in standard stars", Astronomy & Astrophysics, 547: A62, arXiv:1210.7893, Bibcode:2012A&A...547A..62H, doi:10.1051/0004-6361/201219804, S2CID 119286159.

Fitzpatrick, E. L.; Massa, D. (March 2005), "Determining the Physical Properties of the B Stars. II. Calibration of Synthetic Photometry", The Astronomical Journal, 129 (3): 1642–1662, arXiv:astro-ph/0412542, Bibcode:2005AJ....129.1642F, doi:10.1086/427855, S2CID 119512018

Hohle, M. M.; Neuhäuser, R.; Schutz, B. F. (April 2010), "Masses and luminosities of O- and B-type stars and red supergiants", Astronomische Nachrichten, 331 (4): 349, arXiv:1003.2335, Bibcode:2010AN....331..349H, doi:10.1002/asna.200911355, S2CID 111387483

Handler, G.; et al. (June 2009), "Asteroseismology of Hybrid Pulsators Made Possible: Simultaneous MOST Space Photometry and Ground-Based Spectroscopy of γ Peg", The Astrophysical Journal Letters, 698 (1): L56–L59, arXiv:0905.1193, Bibcode:2009ApJ...698L..56H, doi:10.1088/0004-637X/698/1/L56

doi.org

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.

Crawford, D. L.; Barnes, J. V.; Golson, J. C. (1971), "Four-color, H-beta, and UBV photometry for bright B-type stars in the northern hemisphere", The Astronomical Journal, 76: 1058, Bibcode:1971AJ.....76.1058C, doi:10.1086/111220

Gies, Douglas R.; Lambert, David L. (March 10, 1992), "Carbon, nitrogen, and oxygen abundances in early B-type stars", Astrophysical Journal, Part 1, 387: 673–700, Bibcode:1992ApJ...387..673G, doi:10.1086/171116

Abt, Helmut A.; Levato, Hugo; Grosso, Monica (July 2002), "Rotational Velocities of B Stars", The Astrophysical Journal, 573 (1): 359–365, Bibcode:2002ApJ...573..359A, doi:10.1086/340590. The zero value is for v sin i, so v and/or i must be small.

McNamara, D. H. (June 1953), "Gamma Pegasi: A Beta Canis Majoris Star of Small Velocity Amplitude", Publications of the Astronomical Society of the Pacific, 65 (384): 144, Bibcode:1953PASP...65..144M, doi:10.1086/126561

Butkovskaya V.V., Plachinda S.I. (2007). "A study of the β Cephei star γ Pegasi: binarity, magnetic field, rotation, and pulsations". Astronomy and Astrophysics. 469 (3 Jul): 1069–1076. doi:10.1051/0004-6361:20065563. We have detected the presence of a weak magnetic field on the star. The longitudinal component of the field varies from -10 G to 30 G with the stellar rotation. The most probable rotational period is P_rot = 6.6538 ± 0.0016 days. Both the orbital and the rotational periods are integral multiples of the difference between them: P_orb/|P_orb - P_rot| = 42.002, and P_rot/|P_orb - P_rot| = 41.002. Variation in the longitudinal magnetic field during the pulsation period with an amplitude about 7 G was detected.

harvard.edu

ui.adsabs.harvard.edu

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.

Wilson, Ralph Elmer (1953), "General Catalogue of Stellar Radial Velocities", Carnegie Institute Washington D.C. Publication, Washington: Carnegie Institution of Washington, Bibcode:1953GCRV..C......0W

semanticscholar.org

api.semanticscholar.org

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.

Gamma Pegasi (English Wikipedia)

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