MX Puppis (MX Pup) is a class B1.5IV[3] (blue subgiant) star in the constellation Puppis. Its apparent magnitude varies irregularly between magnitude 4.6 and 4.9 and it is classified as a Gamma Cassiopeiae variable.[2] It is approximately 930 light years away based on parallax.[1]
MX Puppis was first found to be a variable star by Alan William James Cousins in 1959.[11] It was given its variable star designation in 1972.[12]
A light curve for MX Puppis, adapted from Hubert and Floquet (1998)[13]
↑ 2.02.12.2Samus, N. N. et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S1. Bibcode: 2009yCat....102025S.
↑ 3.03.1Slettebak, A. (1982). "Spectral types and rotational velocities of the brighter Be stars and A-F type shell stars". Astrophysical Journal Supplement Series50: 55. doi:10.1086/190820. Bibcode: 1982ApJS...50...55S.
↑ 4.04.1Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues2237. Bibcode: 2002yCat.2237....0D.
↑Balona, L. A.; Ozuyar, D. (2020). "Pulsation among TESS a and B stars and the Maia variables". Monthly Notices of the Royal Astronomical Society493 (4): 5871. doi:10.1093/mnras/staa670. Bibcode: 2020MNRAS.493.5871B.
↑ 10.010.110.2Zorec, J.; Frémat, Y.; Domiciano De Souza, A.; Royer, F.; Cidale, L.; Hubert, A.-M.; Semaan, T.; Martayan, C. et al. (2016). "Critical study of the distribution of rotational velocities of Be stars". Astronomy & Astrophysics595: A132. doi:10.1051/0004-6361/201628760. Bibcode: 2016A&A...595A.132Z.